{"id":32078,"date":"2019-01-31T16:30:31","date_gmt":"2019-01-31T13:30:31","guid":{"rendered":"https:\/\/bilimvegelecek.com.tr\/?p=32078"},"modified":"2020-04-15T11:24:50","modified_gmt":"2020-04-15T08:24:50","slug":"bilim-devriminde-sira-disi-isbirligibrahe-ve-kepler","status":"publish","type":"post","link":"https:\/\/bilimvegelecek.com.tr\/index.php\/2019\/01\/31\/bilim-devriminde-sira-disi-isbirligibrahe-ve-kepler","title":{"rendered":"Bilim devriminde s\u0131ra d\u0131\u015f\u0131 i\u015fbirli\u011fi: Brahe ve Kepler"},"content":{"rendered":"
Bir y\u00f6n\u00fcyle bilim fenomenlerin \u00fczerinde y\u00fckselebilen yarat\u0131c\u0131, cesur teorisyenlere ihtiya\u00e7 duyar; Kepler bu t\u00fcrden biriydi. Di\u011fer bir y\u00f6n\u00fcyle bilim teorik kurgular\u0131n test edilebilmesi i\u00e7in do\u011fru g\u00f6zlemsel verilere ihtiya\u00e7 duyar; Tycho Brahe\u2019nin verileri bu gereksinimi kar\u015f\u0131lad\u0131. Brahe ve Kepler aras\u0131nda kurulan bu s\u0131ra d\u0131\u015f\u0131 ili\u015fkinin \u00e7ok verimli oldu\u011funa ve bilim devrimini h\u0131zland\u0131ran bir etki yaratt\u0131\u011f\u0131na ku\u015fku yoktur. <\/em><\/p>\n
Johannes Kepler modern astronominin kurucusu olarak hakl\u0131 bir \u00fcne sahip olsa da Tycho Brahe\u2019nin g\u00f6zlemsel verileri olmadan bunu asla ba\u015faramazd\u0131. Brahe\u2019nin g\u00f6zlemleri teleskop \u00f6ncesi astronomide en do\u011fru ve en kapsaml\u0131 veriler olarak kabul edilir. Bir y\u00f6n\u00fcyle bilim fenomenlerin \u00fczerinde y\u00fckselebilen yarat\u0131c\u0131, cesur teorisyenlere ihtiya\u00e7 duyar; Kepler bu t\u00fcrden biriydi. Di\u011fer bir y\u00f6n\u00fcyle bilim teorik kurgular\u0131n test edilebilmesi i\u00e7in do\u011fru g\u00f6zlemsel verilere ihtiya\u00e7 duyar; Tycho\u2019nun verileri bu gereksinimi kar\u015f\u0131lad\u0131. Ancak Brahe ve Kepler \u00f6rne\u011finde teori ve deneyin birlikteli\u011fi hi\u00e7 de kolay ger\u00e7ekle\u015fmedi. Bununla birlikte Brahe ve Kepler aras\u0131nda kurulan bu s\u0131ra d\u0131\u015f\u0131 ili\u015fkinin \u00e7ok verimli oldu\u011funa ve bilim devrimini h\u0131zland\u0131ran bir etki yaratt\u0131\u011f\u0131na ku\u015fku yoktur.<\/p>\n
Copernicus ile Ptolemaios\u2019un \u2018iki b\u00fcy\u00fck d\u00fcnya sistemine\u2019 alternatif kendi ad\u0131yla an\u0131lan \u2018Tychocu sistem\u2019i kuran ve yapt\u0131\u011f\u0131 b\u00fcy\u00fck g\u00f6zlemlerle bilim tarihine y\u00f6n veren Danimarkal\u0131 g\u00f6kbilimci Tycho Brahe (1546-1601) bilim devriminin ana fig\u00fcrlerinden biridir. \nKendi d\u00f6neminin bir\u00e7ok g\u00f6kbilimcisi gibi Brahe de \u00e7ok etkilenmesine ra\u011fmen Copernicus sistemini benimsemekten ka\u00e7\u0131nm\u0131\u015f, astronomi \u00e7al\u0131\u015fmalar\u0131nda -fizik bilimi alan\u0131nda rakipsiz g\u00f6r\u00fcnen- Aristoteles\u00e7i yakla\u015f\u0131ma ba\u011fl\u0131 kalmaya \u00e7al\u0131\u015fm\u0131\u015ft\u0131r.<\/p>\n
\u2018Tychocu\u2019 evren anlay\u0131\u015f\u0131 \n<\/em><\/strong>Brahe\u2019nin Copernicus sistemini kabul etmemesinin hem dinsel hem de bilimsel nedenleri vard\u0131. \u00c7ok dindar biri olmasa da, bu konudaki g\u00f6r\u00fc\u015flerini esas olarak Protestan Luteryen Kilisesi\u2019ne dayand\u0131rmaktayd\u0131. Copernicus sistemini de\u011ferlendirirken \u201cfizi\u011fe ve Kitab-\u0131<\/em> Mukaddes<\/em>\u2019e ayk\u0131r\u0131 noktalar\u0131 oldu\u011fu\u201dnu tekrar tekrar vurgulam\u0131\u015ft\u0131r. Ona g\u00f6re Copernicus sistemi dine ayk\u0131r\u0131yd\u0131, \u00e7\u00fcnk\u00fc yer-merkezlili\u011fe i\u015faret eden G\u00fcne\u015f\u2019in Ye\u015fu\u2019nun emriyle \u201cg\u00f6klerin ortas\u0131nda belirli bir s\u00fcre durdu\u011fu\u201d Kitab-\u0131<\/em> Mukaddes<\/em>\u2019te a\u00e7\u0131k\u00e7a yaz\u0131l\u0131yd\u0131. Brahe bilimsel nedenlerle de g\u00fcne\u015f-merkezli modele kar\u015f\u0131 \u00e7\u0131kmaktayd\u0131. Copernicus\u2019un \u201cmatematik prensiplerini hi\u00e7bir \u015fekilde ihlal etmedi\u011fini, ama harekete uygun olmayan a\u011f\u0131r ve cans\u0131z bir cisim olan Yer\u2019e, etherik me\u015faleler [g\u00f6ksel \u0131\u015f\u0131kl\u0131 cisimler] gibi bir h\u0131z atfetti\u011fini\u201d\u00a0 (Gingerich, 2016: 508) ileri s\u00fcr\u00fcyordu. Onun Copernicus sistemine y\u00f6nelik bilimsel itirazlar\u0131 biri fiziksel di\u011feri kozmolojik olmak \u00fczere iki t\u00fcrl\u00fcd\u00fcr. Fiziksel itiraza g\u00f6re bir kulenin tepesinden b\u0131rak\u0131lan ta\u015f kulenin dibine d\u00fc\u015fmektedir. E\u011fer Copernicus\u2019un iddia etti\u011fi gibi d\u00fcnya d\u00f6n\u00fcyor olsayd\u0131, ta\u015f kulenin dibine d\u00fc\u015fmeyip bat\u0131da bir noktaya d\u00fc\u015fecekti. Demek ki Copernicus\u2019un sistemi do\u011fru de\u011fildir. Kozmolojik itiraza g\u00f6re ise e\u011fer d\u00fcnya g\u00fcne\u015fin etraf\u0131nda hareket ediyorsa, d\u00fcnya y\u0131ld\u0131zlara bazen yakla\u015facak bazen de uzakla\u015facakt\u0131r. Bundan dolay\u0131 da y\u0131ld\u0131zlar\u0131n b\u00fcy\u00fckl\u00fckleri ve \u0131rakl\u0131k a\u00e7\u0131lar\u0131 de\u011fi\u015fmeliydi. Oysa y\u0131ld\u0131zlar\u0131n ne b\u00fcy\u00fckl\u00fcklerinde ne de \u0131rakl\u0131k a\u00e7\u0131lar\u0131nda herhangi bir de\u011fi\u015fiklik g\u00f6zlemlenmi\u015ftir. \nBrahe bir g\u00f6kbilimci olarak hem Copernicus sistemini hem de Ptolemaios sistemini gezegenlerin konumunu \u00f6ng\u00f6rmede ba\u015far\u0131s\u0131z bulur. Bu y\u00fczden 25 y\u0131ldan daha uzun s\u00fcre her gece yirmi asistan\u0131yla birlikte \u00f6l\u00e7\u00fcmler yapm\u0131\u015ft\u0131r. Brahe, hem Ptolemaios\u2019un Almagest<\/em>\u2019ini hem de Copernicus\u2019un De Revolutionibus<\/em>\u2019unu okuyarak kendi astronomi ara\u00e7lar\u0131n\u0131 olu\u015fturmak i\u00e7in harekete ge\u00e7mi\u015ftir. Bir yandan De<\/em> Revolutionibus<\/em>\u2019un astronomiye sunmu\u015f oldu\u011fu matematiksel uyumu g\u00f6rm\u00fc\u015f, di\u011fer yandan Ptolemaios sistemine kar\u015f\u0131 mesafeli bir tutum tak\u0131nm\u0131\u015ft\u0131r. Hem Ptolemaios hem de Copernicus sistemini reddederek kendi ad\u0131yla an\u0131lan, \u2018Tychocu\u2019 evren anlay\u0131\u015f\u0131n\u0131 geli\u015ftirmi\u015ftir. \nTychocu evren anlay\u0131\u015f\u0131na g\u00f6re, eski sistemdeki gibi Yer evrenin merkezini i\u015fgal ederken, G\u00fcne\u015f ve Ay, Yer\u2019in etraf\u0131nda d\u00f6nmeye devam eder. Fakat Aristoteles-Ptolemaios sisteminden farkl\u0131 olarak Tychocu \u015fema gezegenleri g\u00fcne\u015fin uydular\u0131 gibi ele al\u0131r. G\u00fcne\u015f, etraf\u0131nda d\u00f6nen gezegenlerle birlikte Yer\u2019in etraf\u0131nda d\u00f6nerler. \n\u201cBu \u00e7\u00f6z\u00fcm \u00e7ok tuhaf g\u00f6r\u00fcnse de pek \u00e7ok g\u00f6zlemi t\u0131pk\u0131 Copernicus\u2019un ya da Ptolemaios\u2019un sistemi kadar iyi a\u00e7\u0131kl\u0131yordu. \u0130\u015flemsel olarak birinden birini se\u00e7mek zordu ve on alt\u0131nc\u0131 y\u00fczy\u0131l\u0131n sonunda, hararetli destek\u00e7ileriyle birlikte bu \u00fc\u00e7 model de bir arada varl\u0131\u011f\u0131n\u0131 s\u00fcrd\u00fcr\u00fcyordu.\u201d (Fara, 2012: 159) \nBrahe\u2019nin Copernicus sisteminin g\u00fczelli\u011fini ve b\u00fct\u00fcnl\u00fc\u011f\u00fcn\u00fc bozdu\u011fu i\u00e7in \u2018abs\u00fcrt\u2019 denebilecek bir evren modeli ileri s\u00fcrm\u00fc\u015f olmas\u0131 \u015fa\u015f\u0131rt\u0131c\u0131 gelebilir. Ama Brahe\u2019nin evreni Copernicus\u2019un evrenine oranla hem Aristoteles fizi\u011fiyle hem de bilinen olgularla daha iyi uyu\u015fmaktayd\u0131. Di\u011fer bir deyi\u015fle Tycho’nun, eski ve yeni evren tasar\u0131mlar\u0131 aras\u0131nda \u00f6nerdi\u011fi \u00fc\u00e7\u00fcnc\u00fc yol (uzla\u015ft\u0131r\u0131c\u0131 yakla\u015f\u0131m) hem g\u00f6r\u00fcn\u00fc\u015f\u00fc hem de geleneksel do\u011fa felsefesini kurtar\u0131yordu. \u00d6rne\u011fin, y\u0131ld\u0131z paralaks\u0131n\u0131n (\u0131rakl\u0131k a\u00e7\u0131s\u0131) g\u00f6zlemlenmesi gerekmiyordu, \u00e7\u00fcnk\u00fc Yer sabit y\u0131ld\u0131zlara g\u00f6re konumunu de\u011fi\u015ftirmiyordu. G\u00f6zlemlenmi\u015f bir y\u0131ld\u0131z paralaks\u0131 olmad\u0131\u011f\u0131 i\u00e7in de teori bu durumu a\u00e7\u0131klam\u0131\u015f gibi g\u00f6r\u00fcn\u00fcyordu. Ayr\u0131ca Yer\u2019i hareketsiz kabul etti\u011fi i\u00e7in de, Aristoteles fizi\u011fini kullanarak g\u00f6zlenen olgular\u0131 a\u00e7\u0131klayabilmekteydi.<\/p>\n
Brahe\u2019nin y\u00fcksek de\u011ferli g\u00f6kbilimsel g\u00f6zlemleri \n<\/em><\/strong>Brahe geli\u015ftirdi\u011fi modelin sa\u011flam temellere dayand\u0131\u011f\u0131n\u0131, Yer\u2019in hareketsiz oldu\u011funu g\u00f6stermek i\u00e7in gezegenlerin ve ba\u015fl\u0131ca di\u011fer g\u00f6kcisimlerinin g\u00fcnl\u00fck konumlar\u0131n\u0131 olabilecek en do\u011fru bi\u00e7imde \u00f6l\u00e7meye \u00e7al\u0131\u015fmak gibi b\u00fcy\u00fck bir i\u015fe giri\u015fir. Ancak ne ironiktir ki Brahe\u2019nin astronomiye yapt\u0131\u011f\u0131 katk\u0131 geli\u015ftirdi\u011fi modelden ya da astronominin kavramlar\u0131na getirdi\u011fi yenilikten \u00e7ok, do\u011fruluk de\u011feri y\u00fcksek g\u00f6kbilimsel g\u00f6zlemlerinden dolay\u0131 olmu\u015ftur. \nBrahe daha on sekiz ya\u015f\u0131ndayken, yani 1564\u2019te J\u00fcpiter ve Sat\u00fcrn\u2019\u00fcn birbirlerine \u00e7ok yakla\u015ft\u0131klar\u0131n\u0131 g\u00f6zlemlemi\u015f, bu olay\u0131 \u00f6ng\u00f6rmede mevcut astronomi cetvellerinin ne denli hatal\u0131 olduklar\u0131n\u0131n fark\u0131na varm\u0131\u015f ve daha y\u00fcksek hassasiyete sahip cetveller haz\u0131rlanmas\u0131 gerekti\u011fine inanm\u0131\u015ft\u0131. Bu nedenle Brahe kendinden \u00f6nceki g\u00f6kbilimcilerin kullanm\u0131\u015f oldu\u011fu g\u00f6zlem aletlerinin daha b\u00fcy\u00fck, daha dengeli ve daha iyi ayarlanm\u0131\u015f olanlar\u0131n\u0131 tasarlam\u0131\u015f ve yapm\u0131\u015ft\u0131r. Hen\u00fcz teleskopun ke\u015ffedilmedi\u011fi bir d\u00f6nemde kendinden \u00f6nceki g\u00f6kbilimcilerin toplam\u0131\u015f oldu\u011fu astronomi verilerindeki hatalar\u0131 d\u00fczelterek d\u00fczenli ve dakik g\u00f6zlem yapma uygulamas\u0131n\u0131 ba\u015flatm\u0131\u015ft\u0131r. Thomas Kuhn\u2019un s\u00f6zleriyle: \n\u201cGezegenlerin konumlar\u0131na ili\u015fkin g\u00f6zlemlerinin ise genellikle yakla\u015f\u0131k d\u00f6rt dakikal\u0131k bir yan\u0131lma pay\u0131 i\u00e7inde do\u011fru oldu\u011fu anla\u015f\u0131lmaktad\u0131r ve bu de\u011ferler, eski\u00e7a\u011fda en iyi g\u00f6zlemcilerin ula\u015ft\u0131klar\u0131n\u0131n iki kat\u0131ndan daha hassast\u0131r. Ancak Brahe\u2019nin tek tek g\u00f6zlemlerinin do\u011frulu\u011fundan daha da \u00f6nemli olan, toplad\u0131\u011f\u0131 t\u00fcm verilerin bir b\u00fct\u00fcn olarak kapsaml\u0131 ve g\u00fcvenilir olmas\u0131yd\u0131. Ya\u015fam\u0131 boyunca kendisi ve yeti\u015ftirdi\u011fi g\u00f6zlemciler, Avrupa astronomisini eski\u00e7a\u011f verilerine ba\u011f\u0131ml\u0131 olmaktan kurtararak yanl\u0131\u015f verilerden kaynaklanan bir dizi s\u00f6zde astronomik problemi ortadan kald\u0131rd\u0131lar. Brahe\u2019nin g\u00f6zlemleri gezegenler sorununun yeniden ortaya koyulmas\u0131n\u0131 sa\u011flad\u0131; bu gezegenler sorununun \u00e7\u00f6z\u00fcmlenmesinin \u00f6nko\u015fuluydu. Hi\u00e7bir gezegen kuram\u0131 Copernicus\u2019un kulland\u0131\u011f\u0131 verileri ba\u011fda\u015ft\u0131ramazd\u0131.\u201d (Kuhn, 2007: 327)<\/p>\nBrahe\u2019nin De Mundi Aetherei Recentioribus Phaenomenis (1588) adl\u0131 kitab\u0131nda kozmolojik sistemini g\u00f6steren kendi \u00e7izimi.<\/figcaption><\/figure>\n
G\u00fcvenilir, kapsaml\u0131 ve g\u00fcncel verilerin elde edilmesi gezegenler sorununun \u00e7\u00f6z\u00fcm\u00fcne giden yolu a\u00e7m\u0131\u015ft\u0131r. Brahe\u2019nin g\u00f6zlem sonu\u00e7lar\u0131 astronomi tarihinde ilk defa Ptolemaios sistemindeki episayk\u0131l ve eksantriklerin pozisyon astronomisi a\u00e7\u0131s\u0131ndan yetersizli\u011fini ortaya koyacak bir dakiklik ve zenginlik derecesine ula\u015fm\u0131\u015ft\u0131r. Yetersizlikleri kesin bir \u015fekilde belirleyen g\u00f6kbilimci ise Brahe\u2019nin asistan\u0131 Kepler olacakt\u0131r. \nBrahe\u2019nin, ortak merkezli saydam k\u00fcrelere ve kusursuz oldu\u011fu i\u00e7in de\u011fi\u015fmeyen g\u00f6ky\u00fcz\u00fc inanc\u0131na dayanan Aristoteles kozmolojisi ile uyu\u015fmayan yeni g\u00f6kbilimsel g\u00f6zlemler yapm\u0131\u015f olmas\u0131 onun bilim tarihindeki \u00f6nemini art\u0131rm\u0131\u015ft\u0131r. Brahe yakla\u015f\u0131k 800 y\u0131ld\u0131z\u0131n durumunu g\u00f6steren ayr\u0131nt\u0131l\u0131 g\u00f6zlemler yapm\u0131\u015ft\u0131r. 1572 y\u0131l\u0131nda ise \u2018nova\u2019 ad\u0131n\u0131 verdi\u011fi (bug\u00fcn s\u00fcpernova olarak bilinen) yeni bir y\u0131ld\u0131z g\u00f6zlemi\u015ftir. Cassiope tak\u0131my\u0131ld\u0131z\u0131nda g\u00f6zlenen ve di\u011fer y\u0131ld\u0131zlardan \u00e7ok daha parlak olan (Ven\u00fcs kadar parlam\u0131\u015ft\u0131r) bu y\u0131ld\u0131z on alt\u0131 ay kadar g\u00fcnd\u00fcz g\u00f6zle g\u00f6r\u00fclebilir hale gelmi\u015ftir. Brahe profesyonel g\u00f6kbilimcilerden olu\u015fan gruba \u00e7a\u011fr\u0131 yaparak s\u00f6z konusu \u0131\u015f\u0131\u011f\u0131n Avrupa\u2019n\u0131n farkl\u0131 yerlerinden g\u00f6zlemlenmesini sa\u011flam\u0131\u015ft\u0131r. Kendi \u00f6l\u00e7\u00fcmleriyle, aralar\u0131nda Thomas Digges gibi g\u00f6kbilimcilerin de bulundu\u011fu di\u011fer Avrupal\u0131 g\u00f6zlemcilerin \u00f6l\u00e7\u00fcmlerini kar\u015f\u0131la\u015ft\u0131rd\u0131\u011f\u0131 zaman, bu \u0131\u015f\u0131\u011f\u0131n \u0131rakl\u0131k a\u00e7\u0131s\u0131n\u0131n (paralaks) bulunmad\u0131\u011f\u0131n\u0131 saptam\u0131\u015f ve bu durumda Ay\u2019dan daha uzakta, yani \u2018ay\u00fcst\u00fc\u2019 d\u00fcnyada yer ald\u0131\u011f\u0131n\u0131 ke\u015ffetmi\u015ftir. Brahe 1572 s\u00fcpernovas\u0131 olarak bilinen bu g\u00f6zlemini, 1573 y\u0131l\u0131nda yazd\u0131\u011f\u0131 De nova stella <\/em>adl\u0131 yap\u0131t\u0131nda ayr\u0131nt\u0131l\u0131 olarak betimlemi\u015ftir. 1574\u2019te g\u00f6zden kaybolan bu s\u00fcpernova g\u00f6zlemine dayanarak \u201ctek ba\u015f\u0131na bu fenomenin dahi g\u00f6ky\u00fcz\u00fcn\u00fcn de\u011fi\u015fmez olmad\u0131\u011f\u0131n\u0131 g\u00f6sterdi\u011fini\u201d ileri s\u00fcrm\u00fc\u015ft\u00fcr.<\/p>\n1586\u2019da yap\u0131lm\u0131\u015f Tycho Brahe\u2019nin bir portresi.<\/figcaption><\/figure>\n
Brahe 1572\u2019deki s\u00fcpernova g\u00f6zleminden ald\u0131\u011f\u0131 esinle 1577\u2019de g\u00f6r\u00fcnen bir kuyrukluy\u0131ld\u0131z\u0131n \u0131rakl\u0131k a\u00e7\u0131s\u0131n\u0131 da denetlemeye karar vermi\u015ftir. Brahe yine kendi g\u00f6zlemleriyle Avrupal\u0131 g\u00f6kbilimcilerin g\u00f6zlemlerini birle\u015ftirerek kuyrukluy\u0131ld\u0131z\u0131n \u0131rakl\u0131k a\u00e7\u0131s\u0131n\u0131n bulunmad\u0131\u011f\u0131n\u0131, yani Ay\u2019\u0131n \u00f6tesinde ger\u00e7ek bir g\u00f6kcismi oldu\u011funu bulmu\u015ftur. Di\u011fer bir deyi\u015fle Aristoteles\u00e7i filozoflar\u0131n savunduklar\u0131 gibi bu fenomenin ayalt\u0131 d\u00fcnyaya ait \u201ckuru buhar\u201d gibi meteorolojik bir olgu olmad\u0131\u011f\u0131n\u0131 saptam\u0131\u015ft\u0131r. Brahe ayr\u0131ca bu kuyrukluy\u0131ld\u0131z\u0131n izledi\u011fi yolun Aristoteles\u2019in evren \u015femas\u0131nda g\u00f6sterilmedi\u011fine de dikkat \u00e7ekmi\u015ftir. S\u00f6z konusu kuyrukluy\u0131ld\u0131z\u0131n belirli bir yol izledi\u011fini, bunun da gezegen k\u00fcrelerinin i\u00e7inden ge\u00e7mesi anlam\u0131na geldi\u011fini g\u00f6stermi\u015ftir. Di\u011feri gibi bu fenomen de Aristoteles\u00e7i evren anlay\u0131\u015f\u0131 ile uyu\u015fmuyordu. \u00c7\u00fcnk\u00fc kuyrukluy\u0131ld\u0131z\u0131n do\u011frusal hareketine g\u00f6re, yakla\u015ft\u0131\u011f\u0131 t\u00fcm k\u00fcreleri par\u00e7alamas\u0131 ve sonra da evrenden uzakla\u015fmas\u0131 gerekirdi:<\/p>\nBrahe\u2019nin Astronomiae instaurate mechanica adl\u0131 kitab\u0131n\u0131n ba\u015f sayfas\u0131ndaki ill\u00fcstrasyon astrolojiye olan g\u00fc\u00e7l\u00fc inanc\u0131n\u0131 yans\u0131t\u0131r. Bu ill\u00fcstrasyon Brahe\u2019yi bir elinde pusula ile g\u00f6zlerini g\u00f6ky\u00fcz\u00fcne \u00e7evirmi\u015f bir durumda bir k\u00fcrenin \u00fczerinde otururken g\u00f6stermektedir. Ba\u015fl\u0131k \u015f\u00f6yledir: yukar\u0131 bakarken, a\u015fa\u011f\u0131y\u0131 g\u00f6r\u00fcyorum.<\/figcaption><\/figure>\n
\u201cAncak her \u015feyden \u00f6nemlisi bu g\u00f6zlemler, kuyrukluy\u0131ld\u0131zlar\u0131n var oldu\u011fu ileri s\u00fcr\u00fclen g\u00f6k k\u00fcrelerin tam i\u00e7inden ge\u00e7erek hareket etti\u011fini ve bu y\u00fczden g\u00f6k k\u00fcrelerinin fiziksel olarak mevcut olamayaca\u011f\u0131n\u0131 ispatlamaktayd\u0131. Bu k\u00fcreler, Yunan hayal g\u00fcc\u00fcn\u00fcn bir \u00fcr\u00fcn\u00fcyd\u00fc. Bu da Aristoteles gelene\u011fine yap\u0131lm\u0131\u015f esasl\u0131 bir darbeydi.\u201d (Colin, 2003: 375) \nBrahe sadece g\u00f6zlemleriyle de\u011fil, geli\u015ftirdi\u011fi modelle de k\u00fcreler sistemine kar\u015f\u0131 \u00e7\u0131km\u0131\u015ft\u0131r. Tychocu modelde g\u00f6kcisimlerine ait baz\u0131 y\u00f6r\u00fcngeler birbirlerini keserler. \u00d6rne\u011fin, Mars\u2019\u0131n y\u00f6r\u00fcngesi ile G\u00fcne\u015f\u2019in y\u00f6r\u00fcngesi birbirlerini keser. E\u011fer ay\u00fcst\u00fc d\u00fcnyada ger\u00e7ek anlamda k\u00fcreler olsayd\u0131, s\u00f6z konusu k\u00fcrelerden biri di\u011ferinin hareketini engellerdi. Brahe hem evren modeliyle hem de g\u00f6zlemleriyle (ve bu g\u00f6zlemlere getirdi\u011fi yorumlarla) Aristoteles\u2019in m\u00fckemmel g\u00f6ky\u00fcz\u00fc anlay\u0131\u015f\u0131na ve kristal k\u00fcreler varsay\u0131m\u0131na a\u011f\u0131r bir darbe indirmi\u015ftir. Dolay\u0131s\u0131yla Tycho\u2019nun \u00e7al\u0131\u015fmalar\u0131, ister istemez dinamik bir evren g\u00f6r\u00fc\u015f\u00fcn\u00fc (yani ay\u00fcst\u00fc d\u00fcnyan\u0131n da t\u0131pk\u0131 ayalt\u0131 d\u00fcnya gibi s\u00fcrekli de\u011fi\u015fim i\u00e7inde oldu\u011funu varsayan Copernicus\u00e7u d\u00fc\u015f\u00fcnceyi) g\u00fc\u00e7lendiren bir etki yapm\u0131\u015ft\u0131r. Asl\u0131nda Brahe\u2019nin bu g\u00f6zlemleri Antik\u00e7a\u011fdan beri yap\u0131labilecek g\u00f6zlemlerdir:<\/p>\nCopernicus modelinden etkilenmi\u015f olmas\u0131na ra\u011fmen, Yer\u2019in hareket etmedi\u011fine inanan Brahe\u2019nin evren modelinin bir temsili. Brahe Yer\u2019i t\u0131pk\u0131 Ptolemaios modelinde oldu\u011fu gibi evrenin merkezine yerle\u015ftirmi\u015f, ancak bilinen be\u015f gezegeni de G\u00fcne\u015f\u2019in \u00e7evresinde d\u00f6n\u00fcyor olarak g\u00f6stermi\u015fti.<\/figcaption><\/figure>\n
\u201cBrahe\u2019den \u00f6nce, iki bin y\u0131ld\u0131r s\u00f6z konusu fenomenler de bu fenomenleri g\u00f6zlemlemek i\u00e7in gerekli ara\u00e7lar da vard\u0131. Ancak, b\u00f6yle g\u00f6zlemler yap\u0131lm\u0131yor ya da yap\u0131lsa bile, yayg\u0131n olarak yorumlanm\u0131yordu. On alt\u0131nc\u0131 y\u00fczy\u0131l\u0131n ikinci yar\u0131s\u0131nda, \u00e7a\u011flar boyu varolmu\u015f bu fenomenlerin anlam\u0131 ve \u00f6nemi birden de\u011fi\u015fti. Bu de\u011fi\u015fiklik, \u00f6nde gelen ilk temsilcilerinden birisinin Copernicus oldu\u011fu yeni bilimsel d\u00fc\u015f\u00fcnce iklimi i\u00e7inde de\u011ferlendirilmedi\u011finde anla\u015f\u0131lmaz gibi g\u00f6r\u00fcn\u00fcr\u2026 De Revolutionibus<\/em> bir d\u00f6n\u00fcm noktas\u0131d\u0131r ve art\u0131k geriye d\u00f6n\u00fc\u015f yoktur.\u201d (Kuhn, 2007: 339-340) \nCopernicus sistemi g\u00f6kbilimciler aras\u0131nda b\u00fcy\u00fck ilgi uyand\u0131rm\u0131\u015f olsa da h\u0131zl\u0131 ve evrensel bir kabul g\u00f6rmemi\u015ftir. Asl\u0131nda hem Ptolemaios\u2019u hem de Copernicus\u2019u yeni bir yer-merkezli modelde birle\u015ftirmek isteyen tek g\u00f6kbilimci Brahe olmam\u0131\u015ft\u0131r. Brahe\u2019nin Tychocu evren anlay\u0131\u015f\u0131 yer-merkezli modelin konforunu terk etmek istemeyen Avrupal\u0131 baz\u0131 g\u00f6kbilimcilere de ilham kayna\u011f\u0131 olmu\u015ftu: \n\u201c\u0130ngiltere\u2019de, co\u011frafyac\u0131 ve g\u00f6kbilimci Nathaneal Carpenter (1588-1628) geli\u015ftirilmi\u015f bir Tycho sistemini savunmu\u015ftur. Bu sistemde D\u00fcnya g\u00fcndelik olarak kendi ekseni etraf\u0131nda d\u00f6nmektedir. Fransa\u2019da g\u00f6kbilimci Jean Dominique Cassini (1625-1712), Copernicus sistemini g\u00f6kcisimlerinin y\u00f6r\u00fcngeleri i\u00e7in oval \u015fekilli e\u011friler (Cassini ovali) kullanan geli\u015ftirilmi\u015f bir Tycho sistemi kullanarak reddetmi\u015ftir.\u201d (Schadewald, 2016: 538)<\/p>\n
Hven Adas\u0131\u2019nda bir ara\u015ft\u0131rma enstit\u00fcs\u00fc \n<\/em><\/strong>Brahe\u2019nin Avrupa bilim ve k\u00fclt\u00fcr tarihine katk\u0131s\u0131n\u0131n yeterince anla\u015f\u0131ld\u0131\u011f\u0131 s\u00f6ylenemez. Brahe 1575 y\u0131l\u0131nda Danimarka kral\u0131n\u0131n b\u00fcy\u00fck maddi yard\u0131mlar\u0131yla Hven Adas\u0131\u2019nda bir rasathane kurarak Uraniborg\u2019u (R\u00f6nesans tarz\u0131 \u201cUrania kalesini\u201dni) Avrupa\u2019n\u0131n ilk bilimsel ara\u015ft\u0131rma enstit\u00fcs\u00fcne d\u00f6n\u00fc\u015ft\u00fcrd\u00fc. Kalenin i\u00e7inde \u00e7e\u015fitli sabit g\u00f6zlem aletleri, s\u00fcrekli zenginle\u015fen bir k\u00fct\u00fcphane, simya deneyleri i\u00e7in haz\u0131rlanm\u0131\u015f \u00f6zel bir b\u00f6l\u00fcm ve asistanlar\u0131n ya da \u00f6\u011frencilerin kalabilece\u011fi odalar bulunuyordu. Ayr\u0131ca: \n\u201cTycho\u2019nun s\u00fcrekli daha hassas ve kesin \u00f6l\u00e7\u00fcmler yapan aletler \u00fcretti\u011fi at\u00f6lyeleri ve yapt\u0131\u011f\u0131 bulu\u015flar\u0131 yay\u0131mlamak i\u00e7in bir bask\u0131 makinesi vard\u0131. Kalenin g\u00f6zetleme kulesinde bir hapishane bile bulunuyordu. Adan\u0131n ba\u015fka bir yerinde kendi k\u00e2\u011f\u0131t de\u011firmenini ve bal\u0131k havuzlar\u0131n\u0131 kurmu\u015ftu. Daha sonra Tycho daha b\u00fcy\u00fck aletlerin r\u00fczg\u00e2rdan korunakl\u0131 olarak kurulabilece\u011fi ayr\u0131 bir g\u00f6zlemevi kurman\u0131n daha iyi olaca\u011f\u0131na karar verdi. Stjerneborg yani \u2018y\u0131ld\u0131zlar\u0131n kalesi\u2019 olarak adland\u0131r\u0131lan bu yeralt\u0131 g\u00f6zlemevi Tycho\u2019nun en b\u00fcy\u00fck ve en geli\u015fmi\u015f aletlerini bar\u0131nd\u0131r\u0131yordu.\u201d (Voelkel, 2002: 48)<\/p>\nBrahe\u2019nin De Mundi Aetherei Recentioribus Phaenomenis (1588) (G\u00f6ky\u00fcz\u00fc D\u00fcnyas\u0131n\u0131n Yeni Fenomeni \u00dczerine) adl\u0131 kitab\u0131ndan al\u0131nan, 1577 Kuyrukluy\u0131ld\u0131z\u0131n\u0131n konumunu g\u00f6steren \u00e7izim.<\/figcaption><\/figure>\n
Kimi bilim tarih\u00e7ileri Brahe\u2019nin astronomi, kozmoloji ve do\u011fa felsefesine yapt\u0131\u011f\u0131 katk\u0131y\u0131 son y\u0131llarda mercek alt\u0131na almaya ba\u015flam\u0131\u015flard\u0131r. \n\u201cBrahe\u2019nin Avrupa bilim ve k\u00fclt\u00fcr tarihine katk\u0131s\u0131, 2000\u2019li y\u0131llar\u0131n ba\u015flar\u0131nda, 1970\u2019lerdekine g\u00f6re \u00e7ok daha zengin g\u00f6r\u00fcn\u00fcr. Victor E. Thoren\u2019in 1990 y\u0131l\u0131nda yay\u0131nlad\u0131\u011f\u0131 biyografisi [The Lord of Uraniborg: A Biography of Tycho Brahe<\/em>] Brahe\u2019nin astronomisini anlamak i\u00e7in yeni bir ba\u015flang\u0131\u00e7 noktas\u0131 olu\u015ftururken, Peter Zeeberg bizlere Brahe\u2019nin ge\u00e7 d\u00f6nem R\u00f6nesans\u2019\u0131n h\u00fcmanist k\u00fclt\u00fcr\u00fcnde ne kadar derinlere k\u00f6k sald\u0131\u011f\u0131n\u0131 g\u00f6sterdi ve J. R. Christianson, Brahe\u2019nin b\u00fcy\u00fck \u00e7apl\u0131 ara\u015ft\u0131rma ve k\u00fclt\u00fcrel projelerine kat\u0131lan bilim insanlar\u0131n\u0131, teknisyenleri, sanat\u00e7\u0131lar\u0131 ve do\u011fa filozoflar\u0131n\u0131 nas\u0131l himaye etti\u011fini inceledi. Di\u011fer bir\u00e7ok ara\u015ft\u0131rmac\u0131 Brahe\u2019nin astronomisi, kozmolojisi ve do\u011fa felsefesi hakk\u0131nda yeni anlay\u0131\u015flar ortaya koydular. Tycho Brahe c\u00f6mert ve nazik, ancak ilk modern ara\u015ft\u0131rma enstit\u00fcs\u00fcn\u00fcn kurucusu ve birinci s\u0131n\u0131f teorik g\u00f6kbilimcisi oldu\u011fu kadar g\u00f6zlemsel bilimin temel y\u00f6ntemlerinin mucidi olan titiz bir aristokratt\u0131.\u201d (Christianson, 2008: 380-381) \n1601\u2019de \u00f6len Brahe\u2019nin toplad\u0131\u011f\u0131 veriler asistan\u0131 Kepler taraf\u0131ndan verimli bir \u015fekilde de\u011ferlendirilmi\u015ftir. Copernicus\u00e7u sistemin devrimci potansiyeli de tam olarak Kepler ve Galileo\u2019nun bilimsel \u00e7al\u0131\u015fmalar\u0131 sayesinde a\u00e7\u0131\u011fa \u00e7\u0131kabilmi\u015ftir. Brahe\u2019nin Yer\u2019i yeniden evrenin merkezine yerle\u015ftirmesine ra\u011fmen -\u00ad\u00adk\u00fcreler sistemine kar\u015f\u0131 \u00e7\u0131kmas\u0131, di\u011fer gezegenleri G\u00fcne\u015f\u2019in etraf\u0131nda d\u00f6nd\u00fcrmesi ve \u00f6zellikle toplad\u0131\u011f\u0131 do\u011fruluk de\u011feri y\u00fcksek verilerle\u00ad- Copernicus\u2019un sessizce ba\u015flatt\u0131\u011f\u0131 devrimin h\u0131z\u0131n\u0131 art\u0131rd\u0131\u011f\u0131 s\u00f6ylenebilir.<\/p>\n
\u2018KOZMOGRAF\u0130K G\u0130ZEM\u2019\u0130N TEOR\u0130SYEN\u0130: JOHANNES KEPLER<\/strong><\/h4>\n
Johannes Kepler (1571-1630), astronomide geli\u015ftirdi\u011fi eliptik y\u00f6r\u00fcnge modeliyle gezegenlerin \u00fcniform dairesel hareketiyle ilgili eski ilkeyi y\u0131kt\u0131\u011f\u0131 gibi, astronomiyi ve fizi\u011fi Nicolaus Copernicus\u2019tan bile daha fazla devrimcile\u015ftirmeyi ba\u015farm\u0131\u015ft\u0131r. Onun ak\u0131l y\u00fcr\u00fctmesi hem fiziksel hem de matematiksel oldu\u011fu i\u00e7in gezegenlerin hareketinin matematiksel bir modelini yaratabilmi\u015ftir. G\u00fcn\u00fcm\u00fczde her ne kadar gezegenlerle ilgili \u00fc\u00e7 yasas\u0131yla biliniyor olsa da, Kepler\u2019in bilim tarihindeki \u00f6nemi bununla s\u0131n\u0131rl\u0131 de\u011fildir. \nAsl\u0131nda Kepler\u2019in gezegenlerle ilgili yasalar\u0131 evrenin kozmik uyumunu ke\u015ffetmek ve bir g\u00f6k fizi\u011fi olu\u015fturmak i\u00e7in giri\u015filen metafizik bir aray\u0131\u015f\u0131n \u00f6\u011feleri olarak ortaya \u00e7\u0131km\u0131\u015ft\u0131r. Kepler Copernicus\u2019un kendisinden sonra (Rheticus hari\u00e7) ilk co\u015fkulu Copernicus\u00e7u olmu\u015f ve kendi \u00e7al\u0131\u015fmas\u0131n\u0131 tarihsel ba\u011flam\u0131nda ele alarak yeri geldi\u011finde bilimsel hatalar\u0131n\u0131 kabul etmesini bilmi\u015ftir. Ger\u00e7ekten de Kepler, Copernicus sisteminin savunucusundan biri olmakla kalmam\u0131\u015f ve onu daha y\u00fcksek bir bilimsel d\u00fczeye ula\u015ft\u0131rm\u0131\u015ft\u0131r. Bilim tarih\u00e7isi Richard S. Westfall\u2019un saptad\u0131\u011f\u0131 gibi: \n\u201cCopernicus, gezegenler kuram\u0131 i\u00e7in, Aristoteles\u00e7i bilimin benimsenmi\u015f \u00e7er\u00e7evesinin \u00e7izdi\u011fi geni\u015f s\u0131n\u0131rlar i\u00e7inde s\u0131n\u0131rl\u0131 bir reform \u00f6nermi\u015fti. Kepler ve Galileo\u2019dan sonra ise, bu s\u0131n\u0131rl\u0131 reform k\u00f6ktenci bir devrim haline geldi. Modern bilimin yap\u0131lan\u0131\u015f\u0131n\u0131n temelini haz\u0131rlayan 17. y\u00fczy\u0131l \u00e7abalar\u0131, Kepler ve Galileo\u2019nun ortaya \u00e7\u0131kard\u0131\u011f\u0131 sorunlar\u0131n takibinden ibaret oldu.\u201d (Westfall, 1995: 1)<\/p>\nKepler\u2019in k\u00fc\u00e7\u00fck bir \u00e7ocukken g\u00f6rd\u00fc\u011f\u00fc 1577 kuyrukluy\u0131ld\u0131z\u0131 ba\u015fta Brahe olmak \u00fczere d\u00f6nemin Avrupal\u0131 g\u00f6kbilimcilerin ilgisini \u00e7ekmi\u015fti.<\/figcaption><\/figure>\n
Dindar bir d\u00fc\u015f\u00fcn\u00fcr \n<\/em><\/strong>Tanr\u0131\u2019n\u0131n evrende uyumlu bir yap\u0131 in\u015fa etti\u011fine inanan ve bu yap\u0131y\u0131 ara\u015ft\u0131ran Kepler olduk\u00e7a dindar bir d\u00fc\u015f\u00fcn\u00fcrd\u00fc. \u00d6yle ki \u201cg\u00f6kbilimi ve Copernicus sistemi, dinsel \u00e7al\u0131\u015fmalar\u0131n\u0131n yan\u0131nda her zaman ikincil ilgi alanlar\u0131 olarak\u201d (Voelkel, 2002: 16) kalm\u0131\u015ft\u0131r. Bir teolog olmak isteyen Kepler \u201cuzun s\u00fcredir huzursuzdum, ama \u015fimdi, Tanr\u0131\u2019n\u0131n astronomide nas\u0131l parlad\u0131\u011f\u0131n\u0131 g\u00f6rd\u00fcm\u201d demi\u015ftir. (Whitfield, 2008: 153) Yer\u2019in hareket etmekte oldu\u011fu d\u00fc\u015f\u00fcncesine y\u00f6nelik fiziksel itirazlar teolojik nedenlerle Kepler\u2019e \u00f6nemsiz g\u00f6r\u00fcn\u00fcyordu: \u201cOna g\u00f6re Copernicus sisteminin daha kapsaml\u0131, dinsel bir \u00f6nemi vard\u0131. Ona g\u00f6re evren, yarat\u0131c\u0131s\u0131n\u0131n yani Tanr\u0131\u2019n\u0131n imgesinden ba\u015fka bir \u015fey de\u011fildi.\u201d (Voelkel, 2002: 16) Kepler\u2019in gen\u00e7lik y\u0131llar\u0131ndan beri ilgisini \u00e7eken (astronomiyi de kapsayan) matematik ile teoloji hayat\u0131n\u0131n sonuna kadar \u00fczerinde \u00e7al\u0131\u015faca\u011f\u0131 iki alan olmu\u015ftur: \n\u201cBu iki alan bir bak\u0131ma birbirine benziyordu: Her ikisi de ebedi ger\u00e7ek aray\u0131\u015f\u0131nda d\u00fcnyevi deneyimlerimizin d\u0131\u015f\u0131na ta\u015f\u0131yordu. Kepler\u2019e g\u00f6re geometrik kan\u0131tlar, \u00f6l\u00fcml\u00fc ya\u015fam\u0131m\u0131zda eri\u015febilece\u011fimiz en kesin bilgiydi. G\u00f6kbilime gelince, G\u00fcne\u015f sisteminin d\u00fczeninde Tanr\u0131n\u0131n imgesini g\u00f6r\u00fcyordu.\u201d (Voelkel, 2002: 13)<\/p>\n
Brahe ile ortak \u00e7al\u0131\u015fma \n<\/em><\/strong>Kepler T\u00fcbingen \u00dcniversitesi\u2019ndeki Copernicus\u00e7u hocas\u0131 Johannes Maestlin\u2019den hem Ptolemaios hem de Copernicus sistemini \u00f6\u011frenmi\u015f ve kendisi de \u201cbasitli\u011fi ve g\u00fczelli\u011fi\u201d nedeniyle Copernicus sistemini tercih etmi\u015ftir. Evrenin geometrik ilkelere g\u00f6re yap\u0131land\u0131\u011f\u0131na inanan Kepler Copernicus sistemini m\u00fckemmelle\u015ftirebilmek ve dayand\u0131\u011f\u0131 geometrik plan\u0131 a\u00e7\u0131\u011fa \u00e7\u0131karabilmek i\u00e7in \u00e7al\u0131\u015fmalar\u0131na ba\u015flam\u0131\u015ft\u0131r. Bunun sonucunda 1596 y\u0131l\u0131nda yay\u0131nlad\u0131\u011f\u0131 Mysterium <\/em>Cosmographicum<\/em> (Kozmografik Gizem) do\u011fan\u0131n matematiksel bir \u015fekilde d\u00fczenlenmi\u015f oldu\u011funa ili\u015fkin \u201cmetafizik inan\u00e7lar\u0131n\u201d Kepler\u2019in \u00fczerindeki etkisini ortaya koyar. Yap\u0131t\u0131n bir kopyas\u0131n\u0131 g\u00f6nderdi\u011fi Tycho Brahe\u2019den ald\u0131\u011f\u0131 ortak \u00e7al\u0131\u015fma teklifi bilim tarihinde bir d\u00f6n\u00fcm noktas\u0131d\u0131r. Brahe yap\u0131t\u0131n\u0131 \u201c\u00e7ok ba\u015far\u0131l\u0131 bir spek\u00fclasyon\u201d olarak niteledi\u011fi Kepler\u2019e \u015funlar\u0131 s\u00f6ylemi\u015ftir: \u201cBuraya sadece misafir olarak de\u011fil, ayn\u0131 zamanda ba\u015f \u00fcst\u00fcnde tutulacak bir arkada\u015f ve g\u00f6zlemevimiz i\u00e7in \u00e7ok\u00e7a arzu edilen bir kat\u0131l\u0131mc\u0131 ve yolda\u015f olarak geleceksiniz.\u201d (Freely, 2014: 252) \nBrahe\u2019nin \u00f6l\u00fcm\u00fcnden sonra Kepler, Brahe\u2019nin verilerini kullanarak gezegen hareketlerini g\u00f6steren tablolar haz\u0131rlam\u0131\u015ft\u0131r. Brahe\u2019nin dikkatli g\u00f6zlemleri ve ayr\u0131nt\u0131l\u0131 \u00f6l\u00e7\u00fcmlerine dayanan bu tablolar, Rudolphine Tablolar\u0131<\/em> ad\u0131yla 1627 y\u0131l\u0131nda yay\u0131nlanm\u0131\u015ft\u0131r. Kepler gezegenlerin y\u00f6r\u00fcngelerine ili\u015fkin matematiksel teorilerini test edebilmeyi Brahe\u2019nin olduk\u00e7a g\u00fcvenilir kay\u0131tlar tutmu\u015f olmas\u0131na bor\u00e7ludur. Bu tablolar sayesinde, gezegenlerin G\u00fcne\u015f\u2019in etraf\u0131nda eliptik y\u00f6r\u00fcngeler \u00e7izerek d\u00f6nd\u00fcklerini g\u00f6sterebilmi\u015ftir.<\/p>\n
Gezegen y\u00f6r\u00fcngeleri dairesel de\u011fil, eliptik \n<\/em><\/strong>Kepler bilimsel \u00e7al\u0131\u015fmalar\u0131na gezegenlerin dairesel bir y\u00f6r\u00fcnge izledi\u011fi inanc\u0131yla ba\u015flam\u0131\u015f, ama bir s\u00fcre sonra bu inanc\u0131n\u0131 terk etmi\u015ftir. Kepler\u2019in ilk \u00f6nemli \u00e7al\u0131\u015fmas\u0131 olan Mysterium Cosmographicum<\/em>, dairesel hareket kavram\u0131 temel al\u0131narak yaz\u0131lm\u0131\u015ft\u0131r. Bu yap\u0131t\u0131nda Kepler, Copernicus\u2019a oranla daha say\u0131sal bir dil kullanm\u0131\u015f ve daha ayr\u0131nt\u0131l\u0131 \u00e7izelgeler haz\u0131rlam\u0131\u015ft\u0131r. Yeni astronominin matematiksel potansiyeli tam olarak Kepler\u2019in \u00e7al\u0131\u015fmalar\u0131nda a\u00e7\u0131\u011fa \u00e7\u0131km\u0131\u015ft\u0131r.<\/p>\nUraniborg G\u00f6zlemevi\u2019nin plan\u0131. Brahe\u2019nin Hven adas\u0131ndaki bu g\u00f6zlemevi Avrupa\u2019n\u0131n ilk bilimsel ara\u015ft\u0131rma enstit\u00fcs\u00fcd\u00fcr.<\/figcaption><\/figure>\n
Kepler\u2019in deyi\u015fiyle \u201ckendi teorisinin zenginliklerinin fark\u0131nda olmayan\u201d Copernicus, sisteminin ayr\u0131nt\u0131lar\u0131n\u0131 geli\u015ftirirken Ptolemaios sisteminin tekniklerini kullanm\u0131\u015ft\u0131r. Kepler ayr\u0131ca g\u00fcne\u015f-merkezli sistemdeki uyumsuzluklar\u0131 ortadan kald\u0131rmak istemi\u015ftir. Ona g\u00f6re bu uyumsuzlu\u011fun ba\u015fl\u0131ca nedeni, Yer\u2019in g\u00fcne\u015f-merkezli sisteme uygun olarak s\u0131radan bir gezegen olarak ele al\u0131nmamas\u0131 olmu\u015ftur. \u00d6rne\u011fin De<\/em> Revolutionibus<\/em>\u2019ta Yer\u2019in y\u00f6r\u00fcnge bas\u0131kl\u0131\u011f\u0131 G\u00fcne\u015f\u2019ten, di\u011fer y\u00f6r\u00fcnge bas\u0131kl\u0131klar\u0131 ise Yer\u2019in y\u00f6r\u00fcnge merkezinden \u00f6l\u00e7\u00fclm\u00fc\u015ft\u00fcr. (Kuhn, 2007: 342) Bu \u00e7al\u0131\u015fmalar\u0131 sonucunda, gezegenlerin konumlar\u0131n\u0131 \u201cdo\u011fru ve basit\u201d bir \u015fekilde hesaplayan kendi y\u00f6ntemini geli\u015ftirmi\u015ftir. Kepler en temel ke\u015fiflerini Mars\u2019\u0131n hareketi \u00fczerine \u00e7al\u0131\u015f\u0131rken yapm\u0131\u015ft\u0131r: \n\u201cKepler, Tycho\u2019nun verilerine dayanarak Mars\u2019\u0131n dairesel y\u00f6r\u00fcngesinin merkez ve \u00e7ap gibi \u00f6zelliklerini saptamak istedi. Ancak b\u00fct\u00fcn bu \u00e7abalara kar\u015f\u0131n Tycho\u2019nun verilerinin dairesel bir y\u00f6r\u00fcngeye uygun d\u00fc\u015ft\u00fc\u011f\u00fcn\u00fc g\u00f6steremedi ve b\u00f6ylelikle Mars\u2019\u0131n d\u00fczg\u00fcn hareket etmedi\u011fini anlad\u0131. Mars, y\u00f6r\u00fcngesi i\u00e7indeki merkezi ya da herhangi bir noktaya g\u00f6re d\u00fczg\u00fcn a\u00e7\u0131sal bir harekete sahip de\u011fildi.\u201d (Akdo\u011fan, 1996: 92) \nMars konumu ile ilgili g\u00f6zlemler Yer\u2019den yap\u0131ld\u0131\u011f\u0131 i\u00e7in Kepler dikkatini Yer\u2019in y\u00f6r\u00fcngesine \u00e7evirmi\u015f ve Yer\u2019in de t\u0131pk\u0131 Mars gibi \u201cd\u00fczg\u00fcn yani sabit bir h\u0131zla hareket etmedi\u011fini\u201d tespit etmi\u015ftir. Tycho\u2019nun verilerini temel alan Kepler, gezegen hareketlerinin dairesel ve sabit h\u0131zda olmad\u0131\u011f\u0131 g\u00f6r\u00fc\u015f\u00fcne ula\u015fm\u0131\u015ft\u0131r. Di\u011fer bir deyi\u015fle, Brahe\u2019nin g\u00fcvenilir verilerini kullanan Kepler, bir\u00e7ok denemeden sonra \u00e7emberler kombinasyonuna dayal\u0131 hi\u00e7bir modelin gezegen hareketleri sorununu \u00e7\u00f6zemeyece\u011fine karar vermi\u015ftir. \nKepler, gezegen hareketleri sorununu \u00e7\u00f6zebilecek anahtar formun \u00e7emberden ba\u015fka bir form olabilece\u011fini d\u00fc\u015f\u00fcnmeye ba\u015flam\u0131\u015f ve bu ama\u00e7la \u201cfarkl\u0131 oval y\u00f6r\u00fcnge\u201d modellerini Brahe\u2019nin g\u00f6zlemleriyle kar\u015f\u0131la\u015ft\u0131rm\u0131\u015f, buna ra\u011fmen teori ile g\u00f6zlem aras\u0131ndaki uyumsuzlu\u011fun devam etti\u011fini g\u00f6rm\u00fc\u015ft\u00fcr. Daha sonra gezegenlerin y\u00f6r\u00fcngeleri \u00fczerinde de\u011fi\u015fken h\u0131zlarda devindiklerini fark ederek \u015fu sonuca ula\u015fm\u0131\u015ft\u0131r: E\u011fer gezegenler eliptik y\u00f6r\u00fcngelerde ve de\u011fi\u015fken h\u0131zlarda hareket ederlerse, teori ile g\u00f6zlemler uyu\u015fur. Gezegen hareketlerine kar\u015f\u0131l\u0131k gelen elipsler \u00f6l\u00e7ekli bir \u00e7izim \u00fczerinde g\u00f6zle fark edilemeyecek kadar daireye yak\u0131nd\u0131. Asl\u0131nda Kepler, alanlar yasas\u0131n\u0131 elipse uygulam\u0131\u015f ve b\u00f6ylece ilk yasas\u0131n\u0131 elde etmi\u015ftir. Richard Feynman\u2019\u0131n tan\u0131m\u0131yla: \n\u201cElips sadece oval bir \u015fekil de\u011fildir, \u00e7ok \u00f6zel ve kesin bir e\u011fridir: Her biri bir odakta olmak \u00fczere iki \u00e7ivi, bir halka ip ve bir kalemle \u00e7izilebilir; daha matematiksel bir deyi\u015fle, elips, tespit edilmi\u015f iki noktadan (odaklar) uzakl\u0131klar\u0131n\u0131n toplam\u0131 bir sabite e\u015fit olan noktalar\u0131n geometrik yeridir. Ya da, isterseniz, bas\u0131k bir \u00e7emberdir de diyebilirsiniz.\u201d (Fizik Dersleri, 1. Cilt: Mekanik, I\u015f\u0131n\u0131m, Is\u0131<\/em>)<\/p>\n
Kepler Yasalar\u0131 \n<\/em><\/strong>Kepler bu ke\u015fiflerini ilk kez 1609 y\u0131l\u0131nda yay\u0131nlanan k\u0131sa ad\u0131 Astronomia Nova <\/em>olan yap\u0131t\u0131nda a\u00e7\u0131klam\u0131\u015ft\u0131r. Bu yap\u0131t\u0131n uzun ba\u015fl\u0131\u011f\u0131 devrimci i\u00e7eri\u011fini daha iyi yans\u0131t\u0131r: Centilmen Tycho Brahe\u2019nin g\u00f6zlemlerine dayanarak Mars\u2019\u0131n hareketleri \u00fczerine yorumlar arac\u0131l\u0131\u011f\u0131yla nedensel Yeni Astronomi ya da G\u00f6ksel Fizik<\/em>. \u2018Kepler Yasalar\u0131\u2019 olarak bilinen bu ke\u015fifler, kozmolojide b\u00fcy\u00fck bir ilerlemeyi temsil ederler. Kepler\u2019in bu yasalar\u0131 form\u00fcle edebilmesini sa\u011flayan \u00fc\u00e7 temel neden vard\u0131r: Biri Brahe\u2019nin verilerine g\u00fcvenmesi, ikincisi Copernicus sisteminin \u00f6z\u00fcne uygun olarak Yer\u2019i s\u0131radan bir gezegen olarak kabul etmesi, \u00fc\u00e7\u00fcnc\u00fcs\u00fc ise ate\u015fli bir Yeni Platoncu olmas\u0131. Bu yasalar daha sonra Newton\u2019un ters kare ba\u011f\u0131nt\u0131l\u0131 genel \u00e7ekim yasas\u0131n\u0131 geli\u015ftirmesine temel olu\u015fturacakt\u0131r. Kepler ilk iki yasas\u0131n\u0131 Astronomia Nova<\/em>\u2019da (1609) \u00fc\u00e7\u00fcnc\u00fcn\u00fc ise Harmonices Mundi<\/em> (1619) adl\u0131 yap\u0131t\u0131nda a\u00e7\u0131klam\u0131\u015ft\u0131r. Kepler\u2019in ula\u015ft\u0131\u011f\u0131 gezegen hareketleri ile ilgili yasalar \u015funlard\u0131r:<\/p>\n
1) Gezegenler eliptik y\u00f6r\u00fcngelerde hareket ederler ve elipsin odaklar\u0131ndan birinde G\u00fcne\u015f vard\u0131r.<\/p>\n
2) Bir gezegenin y\u00f6r\u00fcnge h\u0131z\u0131, gezegeni G\u00fcne\u015f\u2019e ba\u011flayan do\u011fru e\u015fit zaman aral\u0131klar\u0131nda e\u015fit elips alan\u0131 tarayacak bi\u00e7imde de\u011fi\u015fir.<\/p>\n
3) Bir gezegenin periyodunun karesinin, G\u00fcne\u015f\u2019e olan ortalama uzakl\u0131\u011f\u0131n\u0131n k\u00fcp\u00fcne b\u00f6l\u00fcm\u00fc, ba\u015fka bir gezegenin periyodunun karesinin ortalama uzakl\u0131\u011f\u0131n\u0131n k\u00fcp\u00fcne b\u00f6l\u00fcm\u00fcne e\u015fittir.<\/p>\n
Kepler\u2019in ilk iki yasas\u0131 gezegen hareketlerine uyguland\u0131\u011f\u0131nda (dairesel y\u00f6r\u00fcngeler yerine eliptik y\u00f6r\u00fcngeler; merkez ya da merkez yak\u0131n\u0131ndaki bir nokta \u00e7evresinde \u00fcniform hareket yasas\u0131 yerine, e\u015fit alanlar yasas\u0131 kullan\u0131ld\u0131\u011f\u0131nda), eksantrikler, episayk\u0131llar, ekuantlar ve di\u011fer ad<\/em> hoc<\/em> ara\u00e7lara gerek kalm\u0131yordu. Ptolemaios sisteminde oldu\u011fu kadar olmasa da Copernicus astronomisinde de bu t\u00fcrden ad<\/em> hoc<\/em> hipotezlere ihtiya\u00e7 duyulmaktayd\u0131. Kepler\u2019in bu yasalar\u0131yla birlikte Ptolemaios\u2019tan beri h\u00fck\u00fcm s\u00fcren bu t\u00fcrden ad hoc<\/em> a\u00e7\u0131klamalara son vermi\u015ftir.<\/p>\n
\u2018Kuvvet\u2019 sorunu g\u00fcndeme geliyor \n<\/em><\/strong>Kepler\u2019e g\u00f6re gezegenleri y\u00f6r\u00fcngelerinde hareket ettiren kuvvet, G\u00fcne\u015f\u2019ten etrafa yay\u0131lan fiziksel \u00f6zellikteki kuvvet \u0131\u015f\u0131nlar\u0131d\u0131r. Kepler bu \u0131\u015f\u0131nlara \u201canima motrix\u201d ad\u0131n\u0131 vermi\u015ftir. Gezegen G\u00fcne\u015f\u2019ten uzakla\u015ft\u0131k\u00e7a bu kuvvetin etkisi azalmakta ve G\u00fcne\u015f\u2019e yakla\u015ft\u0131k\u00e7a bu kuvvetin etkisi artmaktad\u0131r. Bu nedenle bir gezegen G\u00fcne\u015f\u2019e yak\u0131nsa daha h\u0131zl\u0131, uzakta ise daha yava\u015f hareket edecektir. Kepler bu fiziksel mekanizmaya dayanarak \u00f6nce \u201calanlar yasas\u0131n\u0131\u201d bulmu\u015f, daha sonra da birinci yasas\u0131n\u0131 form\u00fcle etmi\u015ftir. \nBrahe\u2019nin g\u00f6k k\u00fcrelerinin varl\u0131\u011f\u0131n\u0131 reddetmesi g\u00f6kbilimciler aras\u0131nda Aristoteles kozmolojisi hakk\u0131nda baz\u0131 \u015f\u00fcphelere yol a\u00e7m\u0131\u015f olsa da, \u00f6nemli bir g\u00f6kbilimsel soruna yol a\u00e7mam\u0131\u015ft\u0131. Daha do\u011frusu dairesel hareket do\u011fal hareket olarak kabul edildi\u011fi i\u00e7in \u201cgezegenleri g\u00f6ky\u00fcz\u00fcnde tutan, ta\u015f\u0131yan ve hareket ettiren\u201d dayanak sorunu hen\u00fcz tam olarak g\u00fcndeme gelmemi\u015fti. Bu nedenle Kepler\u2019in en b\u00fcy\u00fck ba\u015far\u0131s\u0131, Antik\u00e7a\u011fdan beri kabul edilen ve Copernicus sisteminin de temel bir \u00f6zelli\u011fini olu\u015fturan dairesel hareket yerine eliptik y\u00f6r\u00fcnge d\u00fc\u015f\u00fcncesini koymu\u015f olmas\u0131d\u0131r. Ancak eliptik y\u00f6r\u00fcnge kavram\u0131yla birlikte gezegenleri y\u00f6r\u00fcngelerinde tutan \u201ckuvvet\u201d sorununu g\u00fcndeme gelebilmi\u015ftir. Nitekim Kepler\u2019in kendisi de bu sorunu fiziksel bir kuvvetle a\u00e7\u0131klamay\u0131 denemi\u015ftir. Bu nedenle onun bir ba\u015far\u0131s\u0131 da ilk kez g\u00f6k mekani\u011fi sorununu ele almas\u0131d\u0131r:<\/p>\nBrahe\u2019nin yeralt\u0131 g\u00f6zlemevi Stjerneborg\u2019un \u00fcstten bir \u00e7izimi.<\/figcaption><\/figure>\n
\u201cKepler\u2019in eliptik y\u00f6r\u00fcngelerden s\u00f6z etmesiyle birlikte fiziksel sorun zorunlu olarak \u00f6n plana \u00e7\u0131kt\u0131: Acaba hangi kuvvet gezegenlerin y\u00f6r\u00fcngesel hareketlerine neden olmaktad\u0131r? \u0130\u015fte on yedinci y\u00fczy\u0131lda Descartes, Huygens, Robert Hooke ve Isaac Newton bu soruna bir \u00e7\u00f6z\u00fcm bulmaya \u00e7al\u0131\u015ft\u0131lar.\u201d (Akdo\u011fan, 1996: 93) \nNe var ki Kepler d\u00f6neminde Ptolemaios sistemi gibi Copernicus sistemi de g\u00f6kbilimciler ve denizciler taraf\u0131ndan yaln\u0131zca g\u00f6kcisimlerinin konumlar\u0131n\u0131 \u00f6ng\u00f6rmede kullan\u0131labilecek faydal\u0131 bir \u015fema olarak kabul edilmekteydi. Ayn\u0131 nedenle, Kepler\u2019in astronomisi de \u00f6nceleri, \u201cdaha kesin bir tahmin kayna\u011f\u0131\u201d olarak ele al\u0131nm\u0131\u015f ve Copernicus \u015femas\u0131n\u0131n geli\u015ftirilmi\u015f bir bi\u00e7imi oldu\u011fu d\u00fc\u015f\u00fcn\u00fclm\u00fc\u015ft\u00fcr. Ancak \u201cfiziksel bir tan\u0131mlama olarak\u201d kabul edildi\u011finde Kepler\u2019in astronomisi, Copernicus sistemine y\u00f6neltilen b\u00fct\u00fcn bilimsel ele\u015ftirilerin hedefi olmu\u015ftur. Copernicus sistemine y\u00f6neltilen ele\u015ftirileri yan\u0131tlayabilmek, ancak i\u00e7inde madde ve hareket kavramlar\u0131n\u0131n yeniden tan\u0131mland\u0131\u011f\u0131 matematiksel bir fizik sayesinde m\u00fcmk\u00fcn olabilmi\u015ftir. 17. y\u00fczy\u0131lda mekanik felsefe olarak bilinen maddenin alternatif bir teorisi geli\u015ftirilmi\u015f ve Aristoteles\u2019in d\u00f6rt neden kavram\u0131ndan -\u00fc\u00e7\u00fc reddedilerek- yaln\u0131zca etkin neden kavram\u0131na yer verilmi\u015ftir. Eylemsizlik ilkesi \u00fczerine temellenen matematiksel fizik Galileo\u2019nun \u00e7al\u0131\u015fmalar\u0131yla ba\u015flam\u0131\u015ft\u0131r.<\/p>\n
Kepler\u2019in geometrici tanr\u0131s\u0131 \n<\/em><\/strong>Kepler\u2019in astronomi alan\u0131ndaki \u00f6nemli ke\u015fiflerinin arka plan\u0131nda matematiksel bir metafizik vard\u0131r. Ortaya koydu\u011fu yasalar\u0131 nicel bir dille ifade etmi\u015f, gezegen hareketlerinin nedeniyle ilgili olarak yeni kavramlar ortaya atm\u0131\u015ft\u0131r. Bruno ve Gilbert\u2019in kozmoloji anlay\u0131\u015f\u0131n\u0131 bilimsel a\u00e7\u0131dan ele\u015ftirmi\u015f ve astronomi bilimini tan\u0131mlamaya \u00e7al\u0131\u015fm\u0131\u015ft\u0131r. Di\u011fer bir deyi\u015fle Kepler bilimsel bulu\u015flar\u0131yla oldu\u011fu kadar felsefi g\u00f6r\u00fc\u015fleriyle de modern bilimi etkilemi\u015ftir. \nT\u00fcbingen \u00dcniversitesi\u2019ndeki \u00f6\u011frencilik y\u0131llar\u0131ndan itibaren Copernicus sistemini desteklemi\u015f olan Kepler\u2019in, R\u00f6nesans mistisizminin, Pythagoras\u00e7\u0131 ve Yeni-Pythagoras\u00e7\u0131 say\u0131 teorisinin ve Hermetik eserlerdeki matematiksel yakla\u015f\u0131m\u0131n etkisi alt\u0131nda, kendi bilim ve felsefe anlay\u0131\u015f\u0131n\u0131 olu\u015fturdu\u011fu anla\u015f\u0131lmaktad\u0131r. (Trusted, 1994: 44; Burtt, 1980: 58; H\u00f6ffding, 1955: 168) Copernicus\u00e7u yeni evren modeline metafizik bir temel sa\u011flayan Yeni-Platoncu arka plan Kepler\u2019e olduk\u00e7a \u00e7ekici gelmi\u015ftir. Bu arka plan evrenin basit bir matematiksel harmoni olarak kavranmas\u0131n\u0131 sa\u011flad\u0131\u011f\u0131 i\u00e7in \u00f6zellikle estetik a\u00e7\u0131dan doyurucuydu. Kepler\u2019in deyi\u015fiyle: \n\u201cKesinlikle biliyorum ki [Copernicus\u00e7u teoriye] bir \u00f6dev bor\u00e7luyum, zira b\u00fct\u00fcn kalbimle bunun do\u011fru oldu\u011funu onaylad\u0131\u011f\u0131mdan ve inan\u0131lmaz ve b\u00fcy\u00fcleyici hazz\u0131yla onun g\u00fczelli\u011fini d\u00fc\u015f\u00fcnd\u00fc\u011f\u00fcmden, b\u00fct\u00fcn g\u00fcc\u00fcmle onu kamuoyu \u00f6n\u00fcnde de okurlar\u0131m i\u00e7in savunmal\u0131yd\u0131m.\u201d (Burtt, 1980: 58)<\/p>\nBrahe 1572 s\u00fcpernova\u2019s\u0131 olarak bilinen g\u00f6zlemi, 1573 y\u0131l\u0131nda yazd\u0131\u011f\u0131 De nova stella adl\u0131 yap\u0131t\u0131nda ayr\u0131nt\u0131l\u0131 olarak betimlemi\u015ftir.<\/figcaption><\/figure>\n
Tanr\u0131\u2019n\u0131n evreni geometrik ilkelere g\u00f6re yaratt\u0131\u011f\u0131na inanan Kepler g\u00fcne\u015f-merkezli sistemin dayana\u011f\u0131n\u0131n ilahi bir plan oldu\u011funu d\u00fc\u015f\u00fcnm\u00fc\u015ft\u00fcr. Bu nedenle, Copernicus sistemini m\u00fckemmelle\u015ftirmek ve g\u00fcne\u015f-merkezli sistemin dayand\u0131\u011f\u0131 \u201cgeometrik plan\u0131 a\u00e7\u0131\u011fa \u00e7\u0131karabilmek i\u00e7in\u201d \u00e7al\u0131\u015fmalar yapm\u0131\u015ft\u0131r. Onun evrenin merkezine G\u00fcne\u015f\u2019i koyan metafizi\u011finde \u201chermetizmin yay\u0131lan etkisi\u201d g\u00f6r\u00fclebilir. Ama Kepler\u2019in hermetizmi mistik de\u011fil \u201ctitiz matematik analizlere dayal\u0131 bir mistisizm\u201d olmu\u015ftur. (Whitfield, 2008: 155) Kepler\u2019in deyi\u015fiyle: \n\u201cG\u00fcne\u015f kesinlikle kendisindeki bizim \u0131\u015f\u0131k dedi\u011fimiz do\u011fal yetene\u011fini her \u015feye ileten bir cisimdir. S\u0131rf bu nedenle, onun uygun yeri g\u00fcc\u00fcn\u00fc s\u00fcrekli ve d\u00fczenli olarak t\u00fcm evrene yayabilece\u011fi, ortadaki, evrenin merkezindeki noktad\u0131r. I\u015f\u0131\u011f\u0131 payla\u015fan t\u00fcm di\u011fer varl\u0131klar g\u00fcne\u015fi taklit eder.\u201d (Trusted, 1994: 47-48) \nKepler, ilk \u00e7al\u0131\u015fmas\u0131 olan Mysterium cosmographicum <\/em>isimli eserini teolojik ve Pythagoras\u00e7\u0131 varsay\u0131mlara dayand\u0131rm\u0131\u015ft\u0131r. Kepler g\u00fcne\u015f-merkezli sistemi yak\u0131ndan inceleyince Copernicus\u2019un gezegenlerin neden bu belirli uzakl\u0131klarda oldu\u011funa dair bir a\u00e7\u0131klama yapmad\u0131\u011f\u0131n\u0131 g\u00f6rd\u00fc. Bu yap\u0131t\u0131nda Kepler, gezegenler aras\u0131ndaki uzakl\u0131klar\u0131 ve gezegenlerin say\u0131lar\u0131n\u0131n neden alt\u0131 oldu\u011funu Pythagoras\u00e7\u0131lar\u0131n kabul etmi\u015f olduklar\u0131 be\u015f d\u00fczg\u00fcn cisim, yani her y\u00fcz\u00fc e\u015fit kenarlara ve a\u00e7\u0131lara sahip cisim ile a\u00e7\u0131klamaya \u00e7al\u0131\u015fm\u0131\u015ft\u0131r. \n\u201cBunlar tetrahedron (d\u00f6rt e\u015f kenar \u00fc\u00e7gen), k\u00fcp (alt\u0131 kare), dodecahedron (on iki be\u015fgen), octahedron (sekiz e\u015f kenar \u00fc\u00e7gen) ve icosahedron (yirmi e\u015f kenar \u00fc\u00e7gen)\u2019dur. Kepler be\u015f d\u00fczg\u00fcn cisimle alt\u0131 k\u00fcreyi a\u00e7\u0131klayabilece\u011fini anlad\u0131 ve be\u015f d\u00fczg\u00fcn cismin i\u00e7 i\u00e7e yerle\u015fti\u011fini tasavvur etti. Be\u015f cismin aras\u0131na d\u00f6rt gezegenin k\u00fcresi yerle\u015febilirdi. Be\u015finci k\u00fcre en alttaki cismin i\u00e7ine ve alt\u0131nc\u0131 k\u00fcre de en \u00fcstteki cisimden sonra konabilirdi. Kepler gezegenlerin birbirlerine olan uzakl\u0131klar\u0131n\u0131 da hesaba katarak be\u015f d\u00fczg\u00fcn cismi i\u00e7ten ba\u015flayarak \u015f\u00f6yle s\u0131ralad\u0131: octahedron, icosahedron, k\u00fcp, tetrahedron ve dodecahedron.\u201d (Akdo\u011fan, 1996: 91) \nKepler, Mysterium cosmographicum\u2019<\/em>un \u00f6ns\u00f6z\u00fcnde teoremini ilk akl\u0131na geldi\u011fi andaki gibi anlatt\u0131: \n\u201cD\u00fcnya \u00e7emberi her \u015feyin \u00f6l\u00e7\u00fcs\u00fcd\u00fcr. \u00c7evresine bir onikiy\u00fczl\u00fc \u00e7izin. Onu \u00e7evreleyen \u00e7ember Mars olacakt\u0131r. Mars\u2019\u0131n \u00e7evresine bir d\u00f6rty\u00fczl\u00fc \u00e7izin. Onu \u00e7evreleyen \u00e7ember J\u00fcpiter\u2019dir. J\u00fcpiter\u2019in \u00e7evresine bir k\u00fcp \u00e7izin. Onu \u00e7evreleyen \u00e7ember Sat\u00fcrn\u2019d\u00fcr. \u015eimdi, D\u00fcnyan\u0131n i\u00e7ine bir yirmiy\u00fczl\u00fc \u00e7izin. Bunun i\u00e7ine \u00e7izilecek \u00e7ember Ven\u00fcs\u2019t\u00fcr. Ven\u00fcs\u2019\u00fcn i\u00e7ine bir sekizy\u00fczl\u00fc \u00e7izin. Bunun i\u00e7ine \u00e7izilecek \u00e7ember Merk\u00fcr\u2019d\u00fcr.\u201d (Voelkel, 2002: 27).<\/p>\n
\u0130lahiyat\u00e7\u0131lar Kepler\u2019i uyar\u0131yor: \u2018\u0130\u015fine bak!\u2019 \n<\/em><\/strong>Gezegenlerin \u00e7oky\u00fczl\u00fclerin i\u00e7ine nas\u0131l dizildi\u011fini ve neden sadece alt\u0131 gezegen oldu\u011funu buldu\u011funu d\u00fc\u015f\u00fcnen Kepler, Maestlin\u2019e yazd\u0131\u011f\u0131 mektupta, yapt\u0131\u011f\u0131 ke\u015fifleri \u201cTanr\u0131n\u0131n harikulade mucizeleri\u201d olarak nitelendiriyordu. Kepler\u2019de g\u00f6kbilimsel sorunlar teolojik sorunlarla i\u00e7 i\u00e7e ge\u00e7mi\u015fti. Bu nedenle Kepler\u2019in Mysterium cosmographicum<\/em>\u2019u sorunsuz bir \u015fekilde yay\u0131nlanabilmi\u015f de\u011fildir. G\u00f6kbilimsel sorunlar\u0131 teolojik sorunlarla birlikte ele alm\u0131\u015f olmas\u0131 bu iki alan\u0131n uzla\u015f\u0131lm\u0131\u015f s\u0131n\u0131rlar\u0131n\u0131 ihlal etti\u011fi anlam\u0131na geliyordu. \n\u201c\u2018Mysterium cosmographicum<\/em>\u2019dan ilahiyat fak\u00fcltesinin \u00e7\u0131kar\u0131lmas\u0131n\u0131 istedi\u011fi tek k\u0131s\u0131m, Kepler\u2019in g\u00fcne\u015f-merkezlili\u011fin, Kitab-\u0131 Mukaddes<\/em>\u2019teki yer-merkezlili\u011fi destekler g\u00f6r\u00fcnen pasajlarla, \u00f6rne\u011fin \u2018Tanr\u0131 yery\u00fcz\u00fcn\u00fc temeller \u00fczerine kurdu, asla sars\u0131lmas\u0131n diye\u2019 diyen mezmur 104:5 ile nas\u0131l ba\u011fda\u015ft\u0131r\u0131laca\u011f\u0131n\u0131 anlatt\u0131\u011f\u0131 b\u00f6l\u00fcmd\u00fc. Kutsal metinlerin ger\u00e7ek anlam\u0131n\u0131n ne oldu\u011fu Kepler\u2019in i\u015fi de\u011fildi. Tanr\u0131bilim profes\u00f6r\u00fc Matthias Hafenreffer\u2019in Kepler\u2019e g\u00f6nderdi\u011fi uyar\u0131 mektubuna g\u00f6re Kepler kendini \u2018soyut matematik\u00e7i rol\u00fcn\u00fc oynamakla\u2019 s\u0131n\u0131rlamal\u0131yd\u0131. Kepler \u00e7al\u0131\u015fmas\u0131n\u0131n g\u00fcne\u015f-merkezlili\u011fin do\u011frulu\u011funun fiziksel bir kan\u0131t\u0131 oldu\u011funu d\u00fc\u015f\u00fcnd\u00fc\u011f\u00fc i\u00e7in bu durum tam bir d\u00fc\u015f k\u0131r\u0131kl\u0131\u011f\u0131yd\u0131. Sadece varsay\u0131mlardan bahsederek Tanr\u0131\u2019y\u0131 nas\u0131l y\u00fcceltebilirdi ki? Ancak, Luterci yetkililere itaat ederek onlar\u0131n dedi\u011fini yapt\u0131.\u201d (Voelkel, 2002: 32-33)<\/p>\nKepler\u2019in gezegen hareketlerine kar\u015f\u0131l\u0131k gelen elipsleri \u00f6l\u00e7ekli bir \u00e7izim \u00fczerinde g\u00f6zle fark edilemeyecek kadar daireye yak\u0131nd\u0131. Tam daire eksantrik, oval, yakla\u015f\u0131k elips (k\u0131r\u0131k \u00e7izgi) ve ger\u00e7ek elips. \u015eekildeki F\u2019ler yakla\u015f\u0131k elipsin odaklar\u0131n\u0131, E ise ger\u00e7ek elipsin \u2018bo\u015f oda\u011f\u0131\u2019n\u0131 g\u00f6steriyor.<\/figcaption><\/figure>\n
Fizik ile astronomiyi birle\u015ftirme hedefi \n<\/em><\/strong>Kepler Pythagoras\u00e7\u0131lar\u0131n be\u015f temel geometrik bi\u00e7imi ile g\u00f6kcisimlerinin uzaydaki da\u011f\u0131l\u0131mlar\u0131 aras\u0131nda paralellik kurmu\u015ftur. Bu paralellik \u201cKepler\u2019in \u00fczerinde durdu\u011fu, sonraki ara\u015ft\u0131rmalar\u0131nda daha ileriye g\u00f6t\u00fcrd\u00fc\u011f\u00fc ve kontrol etti\u011fi kozmografik gizemdir. Bu g\u00f6r\u00fc\u015f, onun hi\u00e7 vazge\u00e7medi\u011fi, evrende belirli matematiksel ili\u015fkilerin olana\u011f\u0131na olan inanc\u0131n\u0131 yans\u0131t\u0131yordu.\u201d (H\u00f6ffding, 1955: 168) Kepler\u2019in bu temel yakla\u015f\u0131m\u0131 b\u00fct\u00fcn yap\u0131tlar\u0131nda g\u00f6r\u00fcl\u00fcr. Mysterium Cosmographicum<\/em> (1596) d\u0131\u015f\u0131nda Astronomia Nova <\/em>(1609), Harmonices Mundi <\/em>(1619) ve Epitome Astronomiae Copernicanae <\/em>(1618-1621 tarihleri aras\u0131nda yedi cilt olarak yay\u0131nlanm\u0131\u015ft\u0131r) adl\u0131 yap\u0131tlar\u0131nda da g\u00f6ksel d\u00fczeni ke\u015ffetmek isteyen Kepler, Pythagoras\u00e7\u0131 gelene\u011fin etkisinde kalm\u0131\u015f, say\u0131lar\u0131n de\u011fil ama geometrinin evrene h\u00fckmetmekte oldu\u011funu d\u00fc\u015f\u00fcnm\u00fc\u015f ve harmonik oranlar\u0131 bulmaya \u00e7al\u0131\u015fm\u0131\u015ft\u0131r. \n\u201cPythagoras\u00e7\u0131lar ve Platon say\u0131lar\u0131n vazge\u00e7ilmez oldu\u011funu d\u00fc\u015f\u00fcn\u00fcyordu. Ama Kepler\u2019e g\u00f6re say\u0131lar yani nicelikler esas de\u011fildi. Bu y\u00fczden, Mysterium<\/em> Cosmographicum<\/em>\u2019da, neden sadece alt\u0131 gezegen oldu\u011funu sordu\u011funda alt\u0131 say\u0131s\u0131n\u0131n \u00f6nemi \u00fczerine d\u00fc\u015f\u00fcnmemi\u015fti. Bunun yerine geometriyi esas alm\u0131\u015ft\u0131. \u2018Cisimlerin ba\u015flang\u0131c\u0131ndan \u00f6nce, geometri ilahi Zihin de e\u015f sonsuzluktayd\u0131\u2019 diyordu.\u201d (Voelkel, 2002: 91) \nEvrenin geometrik bir yap\u0131da oldu\u011fu g\u00f6r\u00fc\u015f\u00fcn\u00fc her zaman korumu\u015f olan Kepler\u2019in \u015fa\u015f\u0131rt\u0131c\u0131 ve bir o kadar da modern olan tutumu deneysel verilerle \u00e7eli\u015fen metafizik g\u00f6r\u00fc\u015flerini de\u011fi\u015ftirmekte teredd\u00fct etmemesidir. \u00d6rne\u011fin Kepler \u00f6nceleri \u201cevrenin temelinde hangi nicel ili\u015fkilerin yatt\u0131\u011f\u0131 sorusuna verilecek cevab\u0131n tamamen a<\/em> priori<\/em> oldu\u011fu\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc savunmu\u015f, bu yakla\u015f\u0131m\u0131ndan Brahe\u2019nin \u201cdeneye dayal\u0131 materyallerini inceledikten ve kendi g\u00f6zlemlerinden sonra\u201d vazge\u00e7mi\u015ftir. Kepler bu sayede Antik\u00e7a\u011fdan beri kutsal bir \u00f6zellik atfedilen \u201cdaire\u201dnin yerine \u201celips\u201di koyabilmi\u015ftir. (H\u00f6ffding, 1955: 170) Gezegen y\u00f6r\u00fcngelerinin m\u00fckemmel kabul edilen daire \u015feklinde de\u011fil de elips bi\u00e7iminde olmas\u0131 Kepler\u2019i evrene geometrik yakla\u015f\u0131m\u0131ndan vazge\u00e7irememi\u015ftir. \u00c7\u00fcnk\u00fc eliptik y\u00f6r\u00fcnge modeli de Kepler\u2019in g\u00f6z\u00fcne fazlas\u0131yla g\u00fczel g\u00f6r\u00fcnm\u00fc\u015ft\u00fcr. \n\u201cKepler\u2019in yapt\u0131\u011f\u0131, Tanr\u0131n\u0131n neden elips yerine k\u00fcre kullanmay\u0131 se\u00e7ti\u011fi (ne de olsa k\u00fcreler, Antik Yunanlar\u0131n g\u00f6rd\u00fc\u011f\u00fc gibi, estetik a\u00e7\u0131dan en anlaml\u0131s\u0131yd\u0131), hepsinin d\u00fczenli devinimler yapmalar\u0131n\u0131 sa\u011flayabilece\u011fi yerde neden gezegenleri bir h\u0131zland\u0131r\u0131p bir yava\u015flatmay\u0131 se\u00e7ti\u011fi oldu. Kepler h\u00e2l\u00e2 \u2018Tanr\u0131n\u0131n d\u00fc\u015f\u00fcnceleri \u00fczerine d\u00fc\u015f\u00fcnmeye\u2019 \u00e7al\u0131\u015f\u0131yordu.\u201d (Henry, 2016: 148) \nKepler\u2019in tek amac\u0131 teolojik bir metafizik kurmak de\u011fildi. Koyr\u00e9\u2019nin i\u015faret etmi\u015f oldu\u011fu gibi Kepler\u2019in fizik ile astronomiyi birle\u015ftirmek gibi \u201cmodern\u201d denebilecek bir amac\u0131 da vard\u0131. O yaln\u0131zca \u201cg\u00f6r\u00fcn\u00fcm\u00fc kurtarmay\u0131\u201d sa\u011flayacak bir astronomi sistemi de\u011fil, evrendeki g\u00f6kcisimlerinin ger\u00e7ek hareketlerinin fiziksel nedenlerini a\u00e7\u0131klayacak bir fizik teorisi de kurmak istiyordu. \nKepler bilim tarihinde, fiziksel olaylar\u0131 nicel bir dil ile ifade etmenin ilk \u00f6nemli \u00f6rne\u011fini vermi\u015ftir. Kepler taraf\u0131ndan ortaya konan ve Kepler Yasalar\u0131 olarak bilinen fizik kurallar\u0131 nicel bir dil arac\u0131l\u0131\u011f\u0131yla ifade edilmi\u015ftir. H\u00f6ffding\u2019in belirtti\u011fi gibi: \n\u201cKepler Do\u011fa\u2019daki nicel ili\u015fkilerin \u00f6nemini belirtti\u011fi g\u00f6r\u00fc\u015fleriyle kesin fizik biliminin (kesin bilimler -exact sciences-, denetlenebilir \u00f6l\u00e7\u00fc ve hesaplara dayanan bilimlerdir) kurucular\u0131ndan biri oldu. Bu g\u00f6r\u00fc\u015fe teoloji, psikoloji ve do\u011fa felsefesi arac\u0131l\u0131\u011f\u0131yla ula\u015ft\u0131. Teolojik yolu zaten biliyoruz. Evren, Tanr\u0131\u2019n\u0131n do\u011fas\u0131n\u0131n g\u00fczel bir resmi olabilmesi i\u00e7in, belirli nicel ili\u015fkilerle d\u00fczenlenmi\u015ftir. Kepler de Copernicus gibi Do\u011fa\u2019n\u0131n basit ve a\u00e7\u0131k kurallara g\u00f6re i\u015fledi\u011fini d\u00fc\u015f\u00fcn\u00fcyordu. Do\u011fa\u2019n\u0131n kavran\u0131\u015f\u0131ndaki basitlik ve s\u0131ral\u0131 d\u00fczenlilik [ordered regularity] ona \u00fcn getirdi. Her \u015feyi m\u00fcmk\u00fcn oldu\u011funca en az ve en basit ilkelere indirgemeliydik. Psikolojik temel insan zihninin en a\u00e7\u0131k nicel ili\u015fkileri kavrayabilmesinde yat\u0131yordu. Nitelik a\u00e7\u0131s\u0131ndan Do\u011fa\u2019n\u0131n etkinlikleri farkl\u0131 alanlarda, farkl\u0131 bi\u00e7imlerde kendini g\u00f6steriyordu. Tam bir kesinlik ancak kendimizi nicel ili\u015fkilerle s\u0131n\u0131rland\u0131rd\u0131\u011f\u0131m\u0131zda elde edilebilirdi. Bu y\u00fczden de bize ger\u00e7ek do\u011fruyu g\u00f6steren nicelikti\u2026[Kepler\u2019in] do\u011fa felsefesine g\u00f6re \u2018maddenin oldu\u011fu yerde geometri de vard\u0131r\u2019.\u201d (H\u00f6ffding, 1955: 169-170)<\/p>\nKepler\u2019in ilk iki yasas\u0131n\u0131n \u00f6l\u00e7eksiz bir \u00e7izim \u00fczerinde g\u00f6sterimi: 1) B\u00fct\u00fcn gezegenler, odaklar\u0131ndan birinde G\u00fcne\u015f\u2019in bulundu\u011fu elips bi\u00e7imli y\u00f6r\u00fcngeler \u00fczerinde hareket ederler. 2) Bir gezegeni G\u00fcne\u015f\u2019e ba\u011flayan do\u011fru par\u00e7as\u0131 e\u015fit zaman aral\u0131klar\u0131nda e\u015fit alanlar tararlar. Di\u011fer bir deyi\u015fle bir gezegenin y\u00f6r\u00fcngesindeki h\u0131z\u0131 sabit de\u011fildir; G\u00fcne\u015f\u2019e olan uzakl\u0131\u011f\u0131na g\u00f6re artar ya da azal\u0131r.<\/figcaption><\/figure>\n
\u2018Ruh\u2019 kavram\u0131ndan \u2018kuvvet\u2019 kavram\u0131na\u2026 \n<\/em><\/strong>Kepler, Mysterium Cosmographicum<\/em>\u2019un 1596\u2019daki ilk bask\u0131s\u0131nda gezegen hareketleri ba\u011flam\u0131nda \u201cgezegenlerin ruhlar taraf\u0131ndan y\u00f6netildi\u011fi, hatta asl\u0131nda b\u00fct\u00fcn sistemin G\u00fcne\u015f\u2019te ya\u015fayan D\u00fcnya-ruhu taraf\u0131ndan y\u00f6netildi\u011fi\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc ortaya atm\u0131\u015f olsa da sonras\u0131nda bu animizm anlay\u0131\u015f\u0131n\u0131 terk etmi\u015ftir. 1609 y\u0131l\u0131nda Mars gezegeni ile ilgili yazd\u0131\u011f\u0131 ve d\u00f6n\u00fcm noktas\u0131 niteli\u011findeki kitab\u0131nda \u201c\u00f6nemli olan\u0131n fiziksel nedenleri belirtmek oldu\u011funu\u201d vurgulam\u0131\u015ft\u0131r. Kepler Mysterium Cosmographicum<\/em>\u2019un 2. bask\u0131s\u0131nda da \u201chareket eden ruhlar\u201d deyimine bir not olarak \u015funu ilave etmi\u015ftir: \u201cMars\u2019la ilgili kitab\u0131mda b\u00f6yle \u015feyler olmad\u0131\u011f\u0131n\u0131 g\u00f6sterdim.\u201d Ger\u00e7ekten de Kepler \u201cruh\u201d kavram\u0131n\u0131n \u201ckuvvet\u201d kavram\u0131 ile yer de\u011fi\u015ftirmesi gerekti\u011fine karar vermi\u015ftir: \u201cBa\u015flang\u0131\u00e7ta gezegenleri hareket ettiren kuvvetin ger\u00e7ekten bir ruh oldu\u011funa inan\u0131yordum. Fakat, bu hareket ettiren kuvvetin daha b\u00fcy\u00fck bir uzakl\u0131kta azald\u0131\u011f\u0131n\u0131 g\u00f6r\u00fcnce, bunun maddi bir \u015fey olmas\u0131 gerekti\u011fini d\u00fc\u015f\u00fcnd\u00fcm.\u201d (H\u00f6ffding, 1955: 171-172) Kepler\u2019in Astronomia Nova<\/em>\u2019da yer alan \u015fu s\u00f6zleri daha da ilgin\u00e7tir: \n\u201c\u00c7ekim g\u00fcc\u00fc, ayn\u0131 t\u00fcrden cisimler aras\u0131ndaki, birle\u015fmeye veya temas etmeye y\u00f6nelik kar\u015f\u0131l\u0131kl\u0131 cisimsel e\u011filimdir (manyetik g\u00fc\u00e7 de bu t\u00fcrdendir), bu y\u00fczden D\u00fcnya bir ta\u015f\u0131, ta\u015f\u0131n onu \u00e7ekti\u011finden \u00e7ok daha fazla \u00e7eker …. D\u00fcnya\u2019y\u0131 nereye yerle\u015ftirirsek yerle\u015ftirelim \u2026 a\u011f\u0131r cisimler her zaman ona do\u011fru \u00e7aba g\u00f6sterir. \u2026 E\u011fer iki ta\u015f, birbirlerine yak\u0131n olacak ve ayn\u0131 t\u00fcrden \u00fc\u00e7\u00fcnc\u00fc bir cismin g\u00fcc\u00fcn\u00fcn eri\u015femeyece\u011fi \u015fekilde uzayda bir yere konursa, her biri di\u011ferinin k\u00fctlesine orant\u0131l\u0131 olarak ona yakla\u015farak<\/em>, t\u0131pk\u0131 manyetik cisimlerde oldu\u011fu gibi, aralar\u0131ndaki bir noktada bir araya geleceklerdir.\u201d (Koestler, 2013: 310-311) \nKepler\u2019in kavramsal planda ger\u00e7ekle\u015ftirdi\u011fi de\u011fi\u015fim, bilim tarihinin geni\u015f \u00e7er\u00e7evesi i\u00e7inde de\u011ferlendirilmelidir. Kendi ad\u0131yla an\u0131lan \u00fc\u00e7 yasas\u0131n\u0131 ke\u015ffinin \u00f6tesinde, \u00e7ekim kavram\u0131na do\u011fru ilk ad\u0131m\u0131 atan Kepler, \n\u2018a\u011f\u0131rl\u0131\u011f\u0131\u2019 iki cisim aras\u0131ndaki kar\u015f\u0131l\u0131kl\u0131 \u00e7ekim diye a\u00e7\u0131klayan ilk ki\u015fi olmu\u015ftu; hatta uzayda bulunan ve ba\u015fka hi\u00e7bir etkiye maruz kalmayan iki cismin birbirlerine yakla\u015faca\u011f\u0131n\u0131 ve bir orta noktada bulu\u015facaklar\u0131n\u0131, \u00f6yle ki her birinin kat etti\u011fi uzakl\u0131\u011f\u0131n k\u00fctleleriyle ters orant\u0131l\u0131 olaca\u011f\u0131n\u0131 bile \u00f6ne s\u00fcrm\u00fc\u015f ve gelgitleri do\u011fru bir bi\u00e7imde G\u00fcne\u015f ve Ay\u2019\u0131n \u00e7ekimine ba\u011flam\u0131\u015ft\u0131.\u201d (Koestler, 2013: 460) \nB\u00f6ylece Kepler, Copernicus ve Brahe\u2019den farkl\u0131 olarak y\u0131pranm\u0131\u015f eski g\u00f6k k\u00fcreleri modeline alternatif bir g\u00f6k mekani\u011fi geli\u015ftiren ilk g\u00f6kbilimci olmu\u015ftur. Kepler, William Gilbert\u2019in \u201cmanyetizma \u00e7al\u0131\u015fmalar\u0131ndan belirgin bi\u00e7imde yararlanarak\u201d (Henry, 2016: 140) G\u00fcne\u015f\u2019ten yay\u0131lan ve ondan uzakla\u015ft\u0131k\u00e7a etkisi azalan bir kozmik kuvvet ke\u015ffetti. B\u00f6ylece bir anlamda k\u00fctle \u00e7ekimi teorisinin e\u015fi\u011fine ula\u015fm\u0131\u015f oldu: \n\u201cKepler, Antik\u00e7a\u011fdan R\u00f6nesans\u2019\u0131n ilk d\u00f6nemlerine kadar hakim olan \u2018do\u011fal hareket\u2019 kavram\u0131 yerine \u2018\u00e7ekim\u2019 kavram\u0131n\u0131 koymu\u015ftur. Kepler\u2019in kulland\u0131\u011f\u0131 anlamda \u2018\u00e7ekim\u2019 kavram\u0131n\u0131 ilk tan\u0131mlayan d\u00fc\u015f\u00fcn\u00fcrlerden biri W. Gilbert\u2019dir. \u00c7\u00fcnk\u00fc Gilbert, elektrik konusundaki \u00e7al\u0131\u015fmalar\u0131nda \u2018manyetik \u00e7ekim kuvveti\u2019 kavram\u0131n\u0131 kullanm\u0131\u015ft\u0131r. Gilbert\u2019in bu \u00e7al\u0131\u015fmas\u0131, Kepler\u2019de gezegenlerin hareketlerini nicel bir dil arac\u0131l\u0131\u011f\u0131yla a\u00e7\u0131klarken kulland\u0131\u011f\u0131 \u2018\u00e7ekim kuvvetleri\u2019 kavram\u0131n\u0131n ilk \u00f6rne\u011fi ve haz\u0131rlay\u0131c\u0131s\u0131d\u0131r. Kepler b\u00f6ylece hareketin a\u00e7\u0131klanmas\u0131nda, \u2018canl\u0131l\u0131k\u2019 (\u2018anima\u2019) yerine nicel bir dil ile ifade edilebilen \u2018kuvvet\u2019 (\u2018vis\u2019) kavram\u0131n\u0131 koymu\u015ftur. Kepler\u2019in bu ba\u015far\u0131s\u0131, kavramsal yap\u0131da ger\u00e7ekle\u015fen k\u00f6kl\u00fc de\u011fi\u015fimin ilk \u00f6nemli \u00f6rneklerinden birisidir.\u201d (Ural, 1994: 39)<\/p>\n
Nicel \u00f6zellikler d\u00fcnyas\u0131 \n<\/em><\/strong>Kepler\u2019in k\u00fctle \u00e7ekimi teorisi onun yasalar\u0131nda \u00f6rt\u00fck olarak vard\u0131r. Kepler\u2019in ikinci yasas\u0131 (Bir gezegenin y\u00f6r\u00fcnge h\u0131z\u0131, gezegeni G\u00fcne\u015f\u2019e ba\u011flayan do\u011fru e\u015fit zaman aral\u0131klar\u0131nda e\u015fit elips alan\u0131 tarayacak bi\u00e7imde de\u011fi\u015fir) gezegenlerin hareketinin G\u00fcne\u015f taraf\u0131ndan kontrol edildi\u011fi anlam\u0131na gelir. Newton, Kepler\u2019in 3. yasas\u0131n\u0131 temele alarak \u201cgezegenleri G\u00fcne\u015f\u2019e \u00e7eken kuvvetin, gezegenlerin G\u00fcne\u015f\u2019e olan uzakl\u0131klar\u0131n\u0131n karesiyle ters orant\u0131l\u0131 olarak azalaca\u011f\u0131n\u0131\u201d bulmu\u015f ve onun \u00fc\u00e7 yasas\u0131n\u0131 da kendi sistemi i\u00e7ine yerle\u015ftirmi\u015ftir.<\/p>\n) Harmonices Mundi\u2019de Kepler, evrenin s\u0131rlar\u0131n\u0131 a\u00e7\u0131\u011fa \u00e7\u0131karmak i\u00e7in d\u00fczenli \u015fekiller denedi. Gezegenler armonik aral\u0131klara denk gelen uzakl\u0131klarda dizilmi\u015f olmal\u0131yd\u0131. Bu uyumlu aral\u0131klar \u201ck\u00fcrelerin bir m\u00fczi\u011fi\u201d oldu\u011fu d\u00fc\u015f\u00fcncesini uyand\u0131r\u0131yordu.<\/figcaption><\/figure>\n
Burtt\u2019e g\u00f6re, Kepler yeni metafizi\u011fi form\u00fcle ederken, \u201cnedensellik\u201d, \u201chipotez\u201d, \u201cnicelik\u201d gibi kavramlar\u0131 (yeniden) tan\u0131mlam\u0131\u015f ve birincil nitelikler ile ikincil nitelikler aras\u0131nda bir ayr\u0131m yapm\u0131\u015ft\u0131r. Kepler nedensellik ve hipotez kavramlar\u0131n\u0131 harmoni ve matematiksel basitlik ba\u011flam\u0131nda yeniden tan\u0131mlam\u0131\u015ft\u0131r. Kepler\u2019e g\u00f6re bir sonucu ortaya \u00e7\u0131karan neden her zaman matematiksel harmonidir. Kepler hipotezle ilgili olarak da \u201cayn\u0131 olgular hakk\u0131nda de\u011fi\u015fik bir\u00e7ok hipotezden, olgular\u0131n ni\u00e7in \u00f6yle oldu\u011funu g\u00f6steren bir tanesi do\u011frudur\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc savunmu\u015ftur. Kepler i\u00e7in, \u201chipotezin ve nedenselli\u011fin matematiksel ve estetik kavran\u0131\u015f\u0131 d\u00fcnyan\u0131n yeni bir kavran\u0131\u015f\u0131 demektir.\u201d (Burtt, 1980: 64-66) \nKepler, ilk kez Antik\u00e7a\u011fda ortaya konan birincil nitelikler ile ikincil nitelikler aras\u0131ndaki ayr\u0131m\u0131 felsefesinin temeline yerle\u015ftirmi\u015ftir. Democritos\u2019un ve Lukretius\u2019un spek\u00fclatif metafizi\u011fine dayanan bu ayr\u0131ma g\u00f6re Antik\u00e7a\u011f atomcular\u0131 nesnelerin g\u00f6zlemlenen \u00f6zelliklerini, g\u00f6r\u00fcnmez, de\u011fi\u015fmez ve b\u00f6l\u00fcnmez \u00f6zelliklere sahip atomlarla a\u00e7\u0131klam\u0131\u015flard\u0131r. 16. y\u00fczy\u0131lda Vives, Sanchez, Montaigne ve Campanella gibi d\u00fc\u015f\u00fcn\u00fcrler taraf\u0131ndan yeniden canland\u0131r\u0131lm\u0131\u015f olan birincil ve ikincil nitelikler ayr\u0131m\u0131n\u0131n g\u00fcncellik kazanmas\u0131 asl\u0131nda bilgi sorununun felsefede \u00f6ne \u00e7\u0131kmas\u0131 ile yak\u0131ndan ilgilidir. Bilgi edinmede duyular i\u015fe kar\u0131\u015ft\u0131\u011f\u0131 i\u00e7in, ikincil nitelikler, yani duyusal bilgi kar\u0131\u015f\u0131k, \u00e7eli\u015fkili ve bunlardan dolay\u0131 da g\u00fcvenilmezdir. Nesnenin duyusal \u00f6zellikleri, nesnenin birincil (objektif) nitelikleri de\u011fildir; \u00f6zneye ba\u011fl\u0131 olarak ortaya \u00e7\u0131kan ikincil (s\u00fcbjektif) nitelikleridir. Kepler i\u00e7in \u201cger\u00e7ek \u00f6zellikler duyular d\u00fcnyas\u0131n\u0131n temelini olu\u015fturan matematiksel harmoninin i\u00e7indeki\u201d \u00f6zelliklerdir. Ger\u00e7ek ya da birincil nitelikler, duyusal \u00f6zelliklerle \u201cnedensellik ili\u015fkisi\u201d i\u00e7indedirler. Kepler\u2019e g\u00f6re ger\u00e7ek d\u00fcnya yaln\u0131zca nicel \u00f6zelliklerin d\u00fcnyas\u0131d\u0131r; onun farklar\u0131 yaln\u0131zca say\u0131 farklar\u0131d\u0131r: \n\u201cKepler\u2019in pozisyonu \u00f6nemli bir bilgi doktrinine yol a\u00e7t\u0131. Yaln\u0131zca duyular\u0131m\u0131za sunulan b\u00fct\u00fcn nesnelerdeki matematiksel ili\u015fkileri ke\u015ffetmeyiz; kesin b\u00fct\u00fcn bilgiler nicel \u00f6zelliklerin bilgileri olmal\u0131d\u0131r, m\u00fckemmel bilgi daima matematikseldir<\/em>… Kepler kendisine arad\u0131\u011f\u0131 onay\u0131 en iyi sa\u011flayacak olan optik, m\u00fczik ve mekanikten baz\u0131 pratik \u00f6rneklere ba\u015fvurur. \u2018T\u0131pk\u0131 g\u00f6z\u00fcn renkleri g\u00f6rmek, kula\u011f\u0131n sesleri duymak i\u00e7in yarat\u0131lmas\u0131 gibi, insan zihni de ne isterse onu de\u011fil de, niceli\u011fi anlamak i\u00e7in yarat\u0131lm\u0131\u015ft\u0131r.\u2019 Bu nedenle nicelik \u015feylerin temel \u00f6zeli\u011fidir, \u2018di\u011fer kategorilerden \u00f6nce gelir\u2019. Bilgimizin d\u00fcnyas\u0131 s\u00f6z konusu oldu\u011fu \u00f6l\u00e7\u00fcde \u015feylerin biricik \u00f6zelli\u011fi nicel \u00f6zelliklerdir.\u201d (Burtt, 1980: 67-68) \nKoyr\u00e9\u2019nin i\u015faret etti\u011fi gibi metafizik bir doktrin olan evrenin sonsuzlu\u011fu anlay\u0131\u015f\u0131na -bu anlay\u0131\u015f empirik bilgilere teorik bir temel olu\u015fturabilirse de- empirik bilgilerden yola \u00e7\u0131k\u0131larak ula\u015f\u0131lamaz. Bu nedenle Kepler, evrenin sonsuzlu\u011fu anlay\u0131\u015f\u0131n\u0131 hem metafizik hem de bilimsel gerek\u00e7elere dayanarak reddetmi\u015ftir. Asl\u0131nda Kepler\u2019in evrenin sonsuzlu\u011funu reddederken kulland\u0131\u011f\u0131 metafizik gerek\u00e7elerinin temelinde dini inan\u00e7lar\u0131 oldu\u011funu fark etmek \u00f6nemlidir. Orta\u00e7a\u011f gelene\u011finin etkilerini ta\u015f\u0131yan ve koyu bir H\u0131ristiyan olan Kepler\u2019e g\u00f6re evren, Teslis inanc\u0131n\u0131 simgeler. (Koyr\u00e9, 1998: 51; Trusted, 1994: 45) \u2018Tanr\u0131\u2019 H\u0131ristiyanl\u0131\u011f\u0131n Teslis inanc\u0131na g\u00f6re, Baba, O\u011ful ve Kutsal Ruh\u2019dan olu\u015fur. Kepler\u2019e g\u00f6re G\u00fcne\u015f Baba\u2019n\u0131n, G\u00f6ksel Tonoz O\u011ful\u2019un ve aradaki uzay da Kutsal Ruh\u2019un simgesidir. Kepler\u2019in deyi\u015fiyle:<\/p>\nKepler\u2019e g\u00f6re m\u00fckemmel kat\u0131lardaki geometrik uyum. Harmonices Mundi\u2019den (1619).<\/figcaption><\/figure>\n
\u201cG\u00f6r\u00fcn\u00fcr evren Kutsal \u00dc\u00e7leme\u2019nin simgesi ve \u2018damga\u2019s\u0131d\u0131r: G\u00fcne\u015f Baba\u2019y\u0131, sabit y\u0131ld\u0131zlar k\u00fcresi O\u011ful\u2019u, Baba\u2019dan yay\u0131l\u0131p y\u0131ld\u0131zlararas\u0131 uzayda etkiyen g\u00f6r\u00fcnmez g\u00fc\u00e7ler de Kutsal Ruh\u2019u temsil eder: Kendisi hareketsiz olup da hareketin kayna\u011f\u0131 olan ve hareketli y\u0131ld\u0131zlar\u0131n ortas\u0131nda yer alan G\u00fcne\u015f, Tanr\u0131 Baba\u2019n\u0131n ve Yarat\u0131c\u0131n\u0131n imgesini ta\u015f\u0131r. … T\u0131pk\u0131 Baba\u2019n\u0131n Kutsal Ruh arac\u0131l\u0131\u011f\u0131yla yaratmas\u0131 gibi, o da itici g\u00fcc\u00fcn\u00fc, hareketli cisimleri i\u00e7eren bir ortam boyunca da\u011f\u0131t\u0131r.\u201d (Koestler, 2013: 242)<\/p>\n
Evrenin sonsuzlu\u011funa itiraz \n<\/em><\/strong>G\u00fcn\u00fcm\u00fcz\u00fcn bak\u0131\u015f a\u00e7\u0131s\u0131ndan Kepler, hi\u00e7bir bi\u00e7imde bilimsel olarak nitelendiremeyece\u011fimiz sorular\u0131n yan\u0131t\u0131n\u0131 aram\u0131\u015ft\u0131r. Modern bak\u0131\u015f a\u00e7\u0131s\u0131ndan bu sorular bilimsel de\u011filmi\u015f gibi g\u00f6r\u00fcnse de Kepler i\u00e7in son derece \u00f6nemliydi. Bu sorular \u015f\u00f6yleydi: \u201cNeden yaln\u0131z alt\u0131 gezegen var? (O d\u00f6nemde kimse Uran\u00fcs ve Nept\u00fcn\u2019\u00fc bilmiyordu.) Neden G\u00fcne\u015f\u2019e \u00f6zellikle bu uzakl\u0131kta duruyorlar?\u201d \nKepler\u2019in neden bu t\u00fcrden sorularla ilgilendi\u011finin yan\u0131t\u0131 onun metafizi\u011finde, daha do\u011frusu dini inan\u00e7lar\u0131nda aranmal\u0131d\u0131r. Ona g\u00f6re evren matematiksel bir d\u00fczen ve uyumun cisimle\u015fmi\u015f bir anlat\u0131m\u0131d\u0131r. Bununla birlikte Kepler, Bruno gibi evrenin sonsuzlu\u011funu savunanlara kar\u015f\u0131 \u00e7\u0131karken, metafizik kabullerini de\u011fil g\u00f6zlemsel astronominin fenomenlerini kullanm\u0131\u015ft\u0131r. Kepler, evrenin sonsuz oldu\u011fu g\u00f6r\u00fc\u015f\u00fcn\u00fc savunan Copernicus\u00e7u ak\u0131m\u0131 (Bruno ve Gilbert) metafizik de\u011fil bilimsel bir ak\u0131l y\u00fcr\u00fctmeyle ele al\u0131r. Dolay\u0131s\u0131yla onlar\u0131n g\u00f6r\u00fc\u015flerini b\u00fct\u00fcn\u00fcyle ya da kategorik olarak reddetmez. \u00d6rne\u011fin Kepler, Bruno\u2019nun evrenin sonsuz oldu\u011fu g\u00f6r\u00fc\u015f\u00fcn\u00fc reddetmekle birlikte, t\u0131pk\u0131 Bruno gibi \u201ce\u011fer gezegenlerin uydular\u0131 varsa \u00fczerinde insanlar\u0131n ya\u015famas\u0131 da m\u00fcmk\u00fcnd\u00fcr\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc de savunur. Kepler\u2019e i\u00e7in Bruno ve Gilbert\u2019in temsil etti\u011fi Copernicus\u00e7u ak\u0131m bilimsel otoritenin k\u00f6t\u00fcye kullan\u0131lmas\u0131n\u0131n \u00f6rnekleridir. Kepler\u2019in deyi\u015fiyle, bu d\u00fc\u015f\u00fcn\u00fcrler \u201cgenel olarak sabit y\u0131ld\u0131zlar\u0131n inan\u0131lmaz bir y\u00fckseklikte olduklar\u0131n\u0131 tan\u0131tlayan astronominin -\u00f6zellikle Copernicus astronomisinin- otoritesini k\u00f6t\u00fcye kulland\u0131\u011f\u0131 gibi Copernicus\u2019un otoritesini de k\u00f6t\u00fcye kulland\u0131\u011f\u0131 i\u00e7in, o zaman \u00e7areyi astronominin kendisinde aramal\u0131y\u0131z.\u201d (Koyr\u00e9, 1998: 53) \nKepler, sonsuzluk d\u00fc\u015f\u00fcncesine kar\u015f\u0131 ak\u0131l y\u00fcr\u00fctmesini kar\u015f\u0131tlar\u0131 ile payla\u015ft\u0131\u011f\u0131 iki \u00f6nc\u00fcle dayand\u0131rm\u0131\u015ft\u0131r: Bu \u00f6nc\u00fcllerden biri evrenin hi\u00e7bir s\u0131n\u0131r\u0131n\u0131n ve belirli hi\u00e7bir yap\u0131s\u0131n\u0131n olmamas\u0131 (yani \u00fcniform olmas\u0131), di\u011feri astronominin g\u00f6zlem verilerine dayanmas\u0131 gerekti\u011fi, yani g\u00f6kbilimsel teorilerin g\u00f6zlem verilerini \u201ca\u015famayaca\u011f\u0131\u201d ile ilgilidir. Kepler\u2019e g\u00f6re e\u011fer evren s\u0131n\u0131rs\u0131z ve \u00fcniform bir yap\u0131da olsayd\u0131 o zaman sabit y\u0131ld\u0131zlar\u0131n evrendeki da\u011f\u0131l\u0131mlar\u0131 da \u00fcniform, yani sabit y\u0131ld\u0131zlar\u0131 birbirinden ay\u0131ran mesafenin de e\u015fit olmas\u0131 gerekirdi (bu ak\u0131l y\u00fcr\u00fctme bi\u00e7imi modern astronominin galaksilerin da\u011f\u0131l\u0131m\u0131yla ilgili g\u00f6r\u00fc\u015f\u00fcn\u00fcn benzeridir). Kepler\u2019e g\u00f6re astronomi g\u00f6r\u00fcnmeyen cisimlerin varl\u0131\u011f\u0131n\u0131 kabul edemeyece\u011fi i\u00e7in sonsuz say\u0131da g\u00f6kcisminin varl\u0131\u011f\u0131n\u0131 da kabul edemez. Di\u011fer bir deyi\u015fle g\u00f6rme ile yak\u0131ndan ilgili olan (g\u00f6zlemsel) astronomi optik kurallarla \u00e7eli\u015fen g\u00f6kcisimlerinin varl\u0131\u011f\u0131n\u0131 kabul edemez. Ancak Kepler\u2019in bu g\u00f6r\u00fc\u015flerini, teleskopun icad\u0131ndan \u00f6nce (1606\u2019da) ifade etti\u011fini unutmamak gerekir.<\/p>\nKepler\u2019in i\u00e7 i\u00e7e ge\u00e7mi\u015f Platonik \u00e7oky\u00fczl\u00fcleri ve gezegen k\u00fcreleri. Mysterium Cosmographicum\u2019dan (1596).<\/figcaption><\/figure>\n
Kepler\u2019e g\u00f6re bir varsay\u0131m olarak sabit y\u0131ld\u0131zlar b\u00f6lgesinin sonsuz oldu\u011funu ve pek \u00e7ok y\u0131ld\u0131z\u0131n g\u00f6remeyece\u011fimiz kadar uzakta oldu\u011funu d\u00fc\u015f\u00fcnebiliriz. Ancak bu varsay\u0131m belli bir deneyim ve g\u00f6r\u00fc\u015f \u00fczerine dayanmayan keyfi bir varsay\u0131m olacakt\u0131r. Bu g\u00f6r\u00fclmez y\u0131ld\u0131zlar astronominin konusu olamayaca\u011f\u0131 gibi var olduklar\u0131 da herhangi bir \u015fekilde kan\u0131tlanamazlar. Kepler bu g\u00f6r\u00fc\u015fleriyle tutarl\u0131 olarak uzayda sonsuz say\u0131da g\u00f6kcismi olamayaca\u011f\u0131n\u0131 ve \u00fczerindeki g\u00f6kcisimlerinden ba\u011f\u0131ms\u0131z olarak sonsuz bir uzaydan s\u00f6z edilemeyece\u011fini dile getirmi\u015ftir. \nKepler, evrenin sonsuzlu\u011funa ili\u015fkin itirazlar\u0131n\u0131, Galileo\u2019nun teleskopla yapt\u0131\u011f\u0131 g\u00f6kbilimsel g\u00f6zlemlerden \u00f6nce ortaya koymu\u015ftur. Galileo\u2019nun yapt\u0131\u011f\u0131 g\u00f6zlemler Kepler\u2019in yeni y\u0131ld\u0131zlarla ilgili g\u00f6r\u00fc\u015flerini k\u0131smen de\u011fi\u015ftirmi\u015fti ama sonsuz bir evren g\u00f6r\u00fc\u015f\u00fcn\u00fc kabul etmesini sa\u011flamam\u0131\u015ft\u0131. Aksine Kepler, Galileo\u2019nun g\u00f6zlemlerini kendi sonlu kozmolojisini do\u011frulayan yeni veriler olarak yorumlam\u0131\u015ft\u0131r. Kepler\u2019e g\u00f6re g\u00f6zlenen g\u00f6kcisimlerinin nas\u0131l yorumland\u0131\u011f\u0131 en az g\u00f6zlem kadar \u00f6nemlidir. Bu cisimler G\u00fcne\u015f\u2019in \u00e7evresinde d\u00f6nen gezegenler olarak yorumlanabilece\u011fi gibi bu gezegenlerin uydular\u0131 olarak da yorumlanabilirler. Ba\u015fka bir yorum da bu cisimlerin baz\u0131 sabit y\u0131ld\u0131zlar\u0131n \u00e7evresinde d\u00f6nen gezegenler oldu\u011fudur. Bu son yorum zorunlu olarak evrenin sonsuzlu\u011fu g\u00f6r\u00fc\u015f\u00fcne yol a\u00e7acakt\u0131r. B\u00f6ylece Galileo\u2019nun \u00e7\u0131plak g\u00f6zle g\u00f6r\u00fclemeyen sabit y\u0131ld\u0131zlarla ilgili g\u00f6zlemlerinin iki m\u00fcmk\u00fcn yorumu ortaya \u00e7\u0131kar. Bir yoruma g\u00f6re, bu t\u00fcr sabit y\u0131ld\u0131zlar\u0131n \u00e7ok uzakta olduklar\u0131 i\u00e7in g\u00f6r\u00fclmeleri m\u00fcmk\u00fcn de\u011filken, di\u011fer yoruma g\u00f6re, bu t\u00fcr sabit y\u0131ld\u0131zlar \u00e7ok k\u00fc\u00e7\u00fck olduklar\u0131 i\u00e7in g\u00f6r\u00fclemezler. Kepler, bu iki yorumdan ikincisini tercih etmi\u015ftir.<\/p>\nKepler\u2019in en \u00fcretken y\u0131llar\u0131, Roma \u0130mparatoru II. Rudolf\u2019un (1576-1612) himayesinde oldu\u011fu Prag\u2019da ge\u00e7ti. Rudolf \u00f6zellikle astroloji ve simya ile ilgileniyordu.<\/figcaption><\/figure>\n
G\u00f6r\u00fcld\u00fc\u011f\u00fc gibi Kepler ve Galileo ayn\u0131 d\u00f6nemde ya\u015fam\u0131\u015f olsalar da aralar\u0131nda olumlu anlamda bilimsel bir etkile\u015fimden pek s\u00f6z edilemez. Kepler Mysterium Cosmographicum<\/em>\u2019unu kimin eline ula\u015faca\u011f\u0131n\u0131 bilmeden \u0130talya\u2019ya g\u00f6ndermi\u015f, o s\u0131rada Padova \u00dcniversitesi\u2019nde matematik profes\u00f6r\u00fc olan Galileo\u2019nun eline bu yap\u0131t\u0131n iki n\u00fcshas\u0131 ula\u015fm\u0131\u015ft\u0131. Galileo, Kepler\u2019e yazd\u0131\u011f\u0131 mektupta s\u0131rr\u0131n\u0131 a\u00e7arak uzun zamand\u0131r kendisinin de Copernicus\u00e7u oldu\u011funu ve Yer\u2019in hareketinin fiziksel kan\u0131tlar\u0131n\u0131 toplad\u0131\u011f\u0131n\u0131, fakat bunlar\u0131 kendine saklad\u0131\u011f\u0131n\u0131 anlatm\u0131\u015ft\u0131. Buna kar\u015f\u0131l\u0131k Kepler, Galileo\u2019ya yazd\u0131\u011f\u0131 mektupta, Copernicus\u2019u a\u00e7\u0131k\u00e7a desteklemeye \u00e7a\u011f\u0131rm\u0131\u015ft\u0131r: \u201cKendine g\u00fcven Galileo ve yoluna devam et. E\u011fer tahminlerim beni yan\u0131ltm\u0131yorsa, Avrupa\u2019daki sadece birka\u00e7 matematik\u00e7i bizden uzak durmaya \u00e7al\u0131\u015facakt\u0131r. \u00c7\u00fcnk\u00fc ger\u00e7e\u011fin g\u00fcc\u00fc \u00e7ok b\u00fcy\u00fckt\u00fcr.\u201d (Voelkel, 2002: 36, 72-73) Ama Galileo sessiz kalmay\u0131 tercih etmi\u015f ve uzun y\u0131llar boyunca Kepler ondan haber alamam\u0131\u015ft\u0131r. Bu iki b\u00fcy\u00fck g\u00f6kbilimci, ayn\u0131 devirde ya\u015fam\u0131\u015f ve ileti\u015fim kurmu\u015f olsalar da, ger\u00e7ek anlamda ba\u011flant\u0131lar\u0131 yoktu. \u00d6yle anla\u015f\u0131l\u0131yor ki Galileo Kepler\u2019in astronomide yapt\u0131\u011f\u0131 reformun fark\u0131nda de\u011fildi, Kepler ise Galileo\u2019nun bulu\u015flar\u0131n\u0131 kendince yorumlam\u0131\u015ft\u0131. \nBununla birlikte Kepler, teleskopunun gezegenleri bir \u00f6l\u00e7\u00fcde b\u00fcy\u00fck g\u00f6sterirken sabit y\u0131ld\u0131zlar\u0131n g\u00f6r\u00fcnen boyutlar\u0131nda bir de\u011fi\u015fikli\u011fe yol a\u00e7mamas\u0131n\u0131n a\u00e7\u0131klamas\u0131n\u0131 yapm\u0131\u015ft\u0131r. Kepler\u2019e g\u00f6re, teleskopla bak\u0131ld\u0131\u011f\u0131nda sabit y\u0131ld\u0131zlar\u0131 ku\u015fatan \u201c\u0131\u015f\u0131kl\u0131 pus\u201d yok olur. \u00c7\u00fcnk\u00fc \u0131\u015f\u0131kl\u0131 pus \u201cg\u00f6r\u00fclen y\u0131ld\u0131zlara ait de\u011fil ama g\u00f6ren g\u00f6ze aittir\u201d. Di\u011fer bir deyi\u015fle, \u201cgezegenlerin g\u00f6r\u00fcl\u00fcr boyutlar\u0131n\u0131n ger\u00e7ek boyutlar\u0131yla belirli bir ili\u015fkileri varken, buna kar\u015f\u0131 sabit y\u0131ld\u0131zlar i\u00e7in\u201d durum b\u00f6yle de\u011fildir. Bu nedenle gezegenlerin boyutlar\u0131n\u0131 hesaplamak kolay, sabit y\u0131ld\u0131zlar\u0131n boyutlar\u0131n\u0131 hesaplamak zordur. (Koyr\u00e9, 1998: 62) \nKepler\u2019e g\u00f6re gezegenler G\u00fcne\u015f\u2019in \u0131\u015f\u0131\u011f\u0131n\u0131 yans\u0131t\u0131rken sabit y\u0131ld\u0131zlar kendi \u0131\u015f\u0131klar\u0131 ile parlamaktad\u0131rlar. Ancak, sabit y\u0131ld\u0131zlar Bruno\u2019nun iddia etmi\u015f oldu\u011fu gibi birer g\u00fcne\u015f de de\u011fildir. Sabit y\u0131ld\u0131zlar\u0131n boyutlar\u0131 G\u00fcne\u015f\u2019e g\u00f6re \u00e7ok k\u00fc\u00e7\u00fckt\u00fcr. Kepler\u2019e g\u00f6re, e\u011fer sabit y\u0131ld\u0131zlar da G\u00fcne\u015f kadar b\u00fcy\u00fck ve parlak olsayd\u0131, g\u00f6ky\u00fcz\u00fc G\u00fcne\u015f kadar ayd\u0131nl\u0131k olurdu. \nAstronomide teleskopun kullan\u0131lmas\u0131 Kepler\u2019in ak\u0131l y\u00fcr\u00fctme bi\u00e7imini de\u011fi\u015ftirmemi\u015ftir. (Koyr\u00e9 1998: 67-68) Kepler\u2019e g\u00f6re, teleskop, \u00e7\u0131plak g\u00f6zle g\u00f6remedi\u011fimiz \u00e7ok say\u0131da g\u00f6kcismini bize g\u00f6sterse bile g\u00f6rme duyumuzun temel \u00f6zelli\u011fi de\u011fi\u015fmez. Sonsuz uzakl\u0131ktaki cisimler teleskoplu ya da teleskopsuz g\u00f6r\u00fclemezler. \u201cOptik d\u00fcnya sonludur\u201d (Koyr\u00e9, 1998: 69-70). Kepler\u2019e g\u00f6re, g\u00f6kbilimsel de\u011fil ama metafizik bir g\u00f6r\u00fc\u015f olarak uzay\u0131n ve y\u0131ld\u0131zlar\u0131n sonsuz oldu\u011fu d\u00fc\u015f\u00fcncesi ileri s\u00fcr\u00fclebilir. Ancak bu iyi bir metafizik g\u00f6r\u00fc\u015f olmayacakt\u0131r.<\/p>\n) Tycho\u2019nun \u00fcnl\u00fc aletlerinden B\u00fcy\u00fck Ekvatoral Halka. Tycho\u2019nun \u00f6l\u00fcm\u00fcnden sonra \u0130mparator II. Rudolf taraf\u0131ndan Kepler\u2019in kullan\u0131m\u0131na verilen aletlerden biri.<\/figcaption><\/figure>\n
Kepler, \u201csonsuz bir uzay i\u00e7inde sonlu bir evren\u201d g\u00f6r\u00fc\u015f\u00fcne de kar\u015f\u0131 \u00e7\u0131km\u0131\u015ft\u0131r. Kepler\u2019e g\u00f6re \u201cbo\u015f uzay yaln\u0131zca \u2018hi\u00e7bir \u015fey\u2019dir, bir non-ens<\/em>tir\u201d. Bu anlamda uzay var olmad\u0131\u011f\u0131 gibi (hi\u00e7bir \u015fey, nas\u0131l var olabilir?<\/em>) Tanr\u0131 taraf\u0131ndan da yarat\u0131lmam\u0131\u015ft\u0131r. (Koyr\u00e9, 1998: 71) Tanr\u0131 evreni hi\u00e7bir \u015feyden yaratm\u0131\u015f olsa da, \u2018hi\u00e7bir \u015fey\u2019i yaratarak ba\u015flamam\u0131\u015ft\u0131r. Cisim ve uzay birlikte vard\u0131r. \u0130\u00e7inde cisim olmayan uzay, bo\u015f uzay de\u011fildir, hi\u00e7bir \u015feydir. Bu g\u00f6r\u00fc\u015fler asl\u0131nda Kepler\u2019e \u00f6zg\u00fc g\u00f6r\u00fc\u015fler de\u011fildir. Aristoteles\u00e7i Skolastik gelene\u011fe aittir. Kepler bilim anlay\u0131\u015f\u0131nda devrim yaratm\u0131\u015f olsa da varl\u0131k ve hareket anlay\u0131\u015f\u0131nda Aristoteles\u00e7i olarak kalm\u0131\u015ft\u0131r. (Koyr\u00e9, 1998: 72) \nKepler\u2019e g\u00f6re astronomi, alan\u0131 g\u00f6zlemlenebilir verilerle s\u0131n\u0131rl\u0131 empirik bir bilimdir: \u201cAstronominin var olmayan ve g\u00f6r\u00fclemeyen \u015feyler \u00fczerine s\u00f6yleyecek hi\u00e7bir \u015feyi yoktur.\u201d Ona g\u00f6re g\u00f6rme g\u00fcc\u00fcm\u00fcz\u00fc a\u015ft\u0131\u011f\u0131 i\u00e7in, sabit y\u0131ld\u0131zlar\u0131n \u00f6tesinde sonsuz bir uzay\u0131n olup olmad\u0131\u011f\u0131 konusunda bir yarg\u0131ya varamay\u0131z. Kendi deyi\u015fiyle \u201castronomi yaln\u0131zca \u015funu \u00f6\u011fretir: y\u0131ld\u0131zlar\u0131n, giderek en k\u00fc\u00e7\u00fck y\u0131ld\u0131zlar\u0131n g\u00f6r\u00fcld\u00fc\u011f\u00fc kadar\u0131yla, uzay sonludur\u201d. (Koyr\u00e9, 1998: 69) \nKepler, gezegen hareketlerini do\u011fru bir \u015fekilde a\u00e7\u0131klayabildi\u011fi halde, yeni bir hareket teorisine ula\u015famam\u0131\u015ft\u0131r. Bunun nedeni, Kepler\u2019in s\u00f6z konusu teoriye ula\u015fmas\u0131n\u0131 sa\u011flayabilecek olan \u201cuzay\u0131n geometrikle\u015ftirilmesi\u201dne y\u00f6nelik yeterli felsefi \u00e7al\u0131\u015fma yapmam\u0131\u015f olmas\u0131d\u0131r. Hareket konusunda b\u00fcy\u00fck \u00f6l\u00e7\u00fcde Aristoteles fizi\u011fini takip eden Kepler i\u00e7in, durgunlu\u011fun a\u00e7\u0131klanmas\u0131 gerekmiyordu. Eylemsizlik ilkesini g\u00f6rmeyi ba\u015faramayan Kepler\u2019e g\u00f6re kuvvet, ivme de\u011fil h\u0131z yarat\u0131r ve bir hareketin s\u00fcrmesi, bir hareket ettiricinin s\u00fcrekli etkisine ba\u011fl\u0131d\u0131r. Koyr\u00e9\u2019nin belirtti\u011fi gibi Kepler\u2019in s\u0131n\u0131rl\u0131 ve sonlu bir evren anlay\u0131\u015f\u0131na ba\u011fl\u0131 kalm\u0131\u015f olmas\u0131, Aristoteles fizi\u011finin s\u0131n\u0131rlar\u0131n\u0131 a\u015fmas\u0131na izin vermemi\u015ftir. (Koyr\u00e9, 1994: 50-51) \nAncak Kepler\u2019in astronomideki tart\u0131\u015f\u0131lmaz ba\u015far\u0131s\u0131 -gezegenlerin konumlar\u0131n\u0131n \u00f6nceden belirlenmesinin do\u011frulu\u011fundaki \u00e7ok b\u00fcy\u00fck art\u0131\u015f- g\u00f6kbilimcileri Kepler\u2019in d\u00fc\u015f\u00fcncelerini anlamaya ve kabul etmeye zorlam\u0131\u015ft\u0131r. \u00d6nceleri \u00e7ok az say\u0131da g\u00f6kbilimci Kepler\u2019in ba\u015far\u0131s\u0131n\u0131 hemen anlam\u0131\u015f olsa da say\u0131 giderek artm\u0131\u015ft\u0131r. \n17. y\u00fczy\u0131l\u0131n sonuna do\u011fru, Kepler ve Galileo gibi \u201cdevlerin omuzlar\u0131nda oturan\u201d Isaac Newton\u2019\u0131n \u00e7al\u0131\u015fmalar\u0131yla birlikte Kepler\u2019in \u00fc\u00e7 yasas\u0131n\u0131n fiziksel gereklili\u011fi daha anla\u015f\u0131l\u0131r hale gelmi\u015ftir. Mekanik ve \u00e7ekim yasalar\u0131n\u0131 matematiksel olarak birle\u015ftirmeyi ba\u015faran Newton, Kepler\u2019in g\u00f6ksel fizi\u011fini benimsememi\u015f olsa da onun yasalar\u0131n\u0131 G\u00fcne\u015f sisteminin hareketlerini tan\u0131mlamada kulland\u0131. \n\u201cHer ne kadar Kepler d\u00e2hi bir g\u00f6kbilimci ve \u00e7ok temel ke\u015fifler yapm\u0131\u015f biri olarak hi\u00e7bir zaman unutulmad\u0131ysa da -gezegenlerin hareketleriyle ilgili \u00fc\u00e7 yasa h\u00e2l\u00e2 onun ad\u0131n\u0131 ta\u015f\u0131maktad\u0131r- fikirleri ancak bilim adamlar\u0131 dikkatlerini bilimsel bilginin do\u011fas\u0131na ve bilimsel d\u00fc\u015f\u00fcnme tarzlar\u0131na y\u00f6nelttiklerinde ayr\u0131nt\u0131s\u0131yla incelenmeye ba\u015fland\u0131. Bilim adamlar\u0131n\u0131n Kepler\u2019in dehas\u0131n\u0131 tam anlam\u0131yla anlamas\u0131n\u0131n, Albert Einstein\u2019\u0131n dehas\u0131yla tan\u0131\u015fmalar\u0131ndan sonra m\u00fcmk\u00fcn oldu\u011fu s\u00f6ylenebilir.\u201d (Voelkel, 2002: 140-141)<\/p>\nTycho\u2019nun \u00fcnl\u00fc aletlerinden Trigonal Sekstant. Tycho\u2019nun \u00f6l\u00fcm\u00fcnden \u0130mparator II. Rudolf taraf\u0131ndan Kepler\u2019in kullan\u0131m\u0131na verilen aletlerden bir di\u011feri.<\/figcaption><\/figure>\n
Kaynaklar:<\/strong><\/p>\n
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20) Westfall, Richard S. (1995), Modern Bilimin Olu\u015fumu<\/em>, \u00e7ev. \u0130smail Hakk\u0131 Duru, Ankara: T\u00dcB\u0130TAK Kitaplar\u0131.<\/p>\n
21) Whitfield, Peter (2008), Bat\u0131 Biliminde D\u00f6n\u00fcm Noktalar\u0131<\/em>, \u00e7ev. Serdar Uslu, \u0130stanbul: K\u00fcre Yay\u0131nlar\u0131.<\/p>\n","protected":false},"excerpt":{"rendered":"
Bir y\u00f6n\u00fcyle bilim fenomenlerin \u00fczerinde y\u00fckselebilen yarat\u0131c\u0131, cesur teorisyenlere ihtiya\u00e7 duyar; Kepler bu t\u00fcrden biriydi. Di\u011fer bir y\u00f6n\u00fcyle bilim teorik kurgular\u0131n test edilebilmesi i\u00e7in do\u011fru g\u00f6zlemsel verilere ihtiya\u00e7 duyar; Tycho Brahe\u2019nin verileri bu gereksinimi kar\u015f\u0131lad\u0131. Brahe ve Kepler aras\u0131nda kurulan bu s\u0131ra d\u0131\u015f\u0131 ili\u015fkinin \u00e7ok verimli oldu\u011funa ve bilim devrimini h\u0131zland\u0131ran bir etki yaratt\u0131\u011f\u0131na ku\u015fku […]<\/p>\n","protected":false},"author":591,"featured_media":32079,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[4476,38,26],"tags":[4491,639,4492],"class_list":["post-32078","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-180-sayi","category-dergi-sayilari","category-fizik","tag-brahe","tag-kepler","tag-tycho-brahe"],"acf":[],"aioseo_notices":[],"aioseo_head":"\n\t\t\n\t\n\t\n\t\n\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t
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