{"id":16046,"date":"2016-03-01T17:18:36","date_gmt":"2016-03-01T15:18:36","guid":{"rendered":"http:\/\/109.232.216.219\/~bilimvegelecek\/?p=16046"},"modified":"2018-01-05T17:30:57","modified_gmt":"2018-01-05T14:30:57","slug":"evrenin-deniz-feneri-pulsarlar","status":"publish","type":"post","link":"https:\/\/bilimvegelecek.com.tr\/index.php\/2016\/03\/01\/evrenin-deniz-feneri-pulsarlar","title":{"rendered":"Evrenin deniz feneri: Pulsarlar"},"content":{"rendered":"

Pulsarlar, kendi etraf\u0131nda \u00e7ok h\u0131zl\u0131 periyotlarda d\u00f6nen ve belirli bir eksende \u0131\u015f\u0131ma yapan n\u00f6tron y\u0131ld\u0131zlar\u0131d\u0131r. Bu mekanizma hen\u00fcz tam olarak anla\u015f\u0131lm\u0131\u015f de\u011fildir, ancak y\u0131ld\u0131zla birlikte d\u00f6nen \u00e7ok g\u00fc\u00e7l\u00fc manyetik alanla do\u011frudan ili\u015fkilidir. E\u011fer y\u0131ld\u0131z\u0131n \u0131\u015f\u0131ma yapt\u0131\u011f\u0131 eksen D\u00fcnya\u2019ya y\u00f6nelmi\u015f ise \u2013y\u0131ld\u0131z d\u00f6nd\u00fc\u011f\u00fc i\u00e7in- kesikli bir \u0131\u015f\u0131k vuru\u015fu g\u00f6zlemlenir. Bu kesikli\u011fin periyodu ise y\u0131ld\u0131za ba\u011fl\u0131 olarak saniye mertebeleri ile milisaniye mertebeleri aras\u0131nda de\u011fi\u015febilmektedir.<\/em><\/p>\n

Y\u0131ld\u0131zlar en basit tan\u0131mla k\u00fctle\u00e7ekiminin \u0131\u015f\u0131n\u0131m bas\u0131nc\u0131yla dengelendi\u011fi astrofiziksel nesnelerdir.K\u00fctle\u00e7ekimi y\u0131ld\u0131z\u0131 i\u00e7eri \u00e7\u00f6kmeye zorlarken, y\u0131ld\u0131zda ger\u00e7ekle\u015fen n\u00fckleer tepkimelerin yaratt\u0131\u011f\u0131 \u0131\u015f\u0131ma bas\u0131nc\u0131 bu \u00e7\u00f6k\u00fc\u015fe kar\u015f\u0131 koyar. Ancak y\u0131ld\u0131z\u0131n n\u00fckleer yak\u0131t\u0131 bitti\u011finde, k\u00fctle\u00e7ekimi lehine denge bozulmaya ba\u015flar.Her y\u0131ld\u0131z bu dengesizli\u011fe ka\u00e7\u0131n\u0131lmaz olarak ula\u015f\u0131r ve k\u00fctlesine ba\u011fl\u0131 olarak da farkl\u0131 senaryolarla \u00f6mr\u00fcn\u00fc sonland\u0131r\u0131r.<\/p>\n

N\u00f6tron y\u0131ld\u0131z\u0131 ve pulsarlar<\/strong><\/p>\n

N\u00f6tron y\u0131ld\u0131z\u0131,G\u00fcne\u015f\u2019in 4 ila 8 kat\u0131 k\u00fctleye sahip y\u0131ld\u0131zlar\u0131n ya\u015fam d\u00f6ng\u00fclerinin sonunda olu\u015fan \u00f6l\u00fc y\u0131ld\u0131z kal\u0131nt\u0131s\u0131d\u0131r. N\u00fckleer yak\u0131tlar\u0131n\u0131 yak\u0131p bitiren y\u0131ld\u0131zlar, s\u00fcpernova patlamas\u0131 ile d\u0131\u015f katmanlar\u0131n\u0131 uzaya sa\u00e7ar. Merkez b\u00f6lge ise \u00e7ekimsel etkiyle kendi i\u00e7ine \u00e7\u00f6ker. Bu \u00e7\u00f6k\u00fc\u015f o kadar g\u00fc\u00e7l\u00fcd\u00fcr ki, proton ve elektronlar birle\u015ferek n\u00f6tronlar\u0131 meydana getirir. Sonu\u00e7 olarak n\u00f6tronlardan olu\u015fan, son derece yo\u011fun bir \u201cn\u00f6tron y\u0131ld\u0131z\u0131\u201d olu\u015fur. Karadeliklerden sonra, evrendeki en yo\u011fun cisimler n\u00f6tron y\u0131ld\u0131zlar\u0131d\u0131r.<\/p>\n

\"\"1934\u2019de Walter Baade ve Fritz Zwicky, n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n varl\u0131\u011f\u0131n\u0131 \u00f6ng\u00f6rd\u00fcler. Bu denli k\u00fc\u00e7\u00fck g\u00f6kcisimlerinin D\u00fcnya\u2019daki teleskoplarla tespit edilebilmesinin m\u00fcmk\u00fcn olmad\u0131\u011f\u0131 d\u00fc\u015f\u00fcn\u00fclmekteydi.Ancak bug\u00fcn biliyoruz ki, n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n manyetik alan\u0131 boyunca hareket eden y\u00fckl\u00fc par\u00e7ac\u0131klar, manyetik kutuplardan \u0131\u015f\u0131n\u0131ma yol a\u00e7ar.Bu \u0131\u015f\u0131n\u0131m da onlar\u0131n g\u00f6zlenebilmesine.<\/p>\n

N\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n sahip oldu\u011fu yo\u011fun manyetik alan D\u00fcnya\u2019n\u0131nkinden yakla\u015f\u0131k bir trilyon kat daha b\u00fcy\u00fckt\u00fcr.Y\u0131ld\u0131z\u0131n d\u00f6nme ekseni ile manyetik ekseni aras\u0131nda -D\u00fcnya\u2019da oldu\u011fu gibi- bir a\u00e7\u0131 olmas\u0131ndan dolay\u0131 da, y\u0131ld\u0131z d\u00f6nd\u00fck\u00e7e \u00e7ok b\u00fcy\u00fck miktarlarda elektrik alan \u00fcretilir ve elektriksel potansiyel 1 trilyon volt gibi inan\u0131lmaz mertebelere ula\u015f\u0131r. Yenge\u00e7 pulsar\u0131n\u0131n manyetik alan\u0131n\u0131n yaln\u0131zca bir metrek\u00fcp\u00fcnde \u00fcretilen enerji, insanl\u0131\u011f\u0131n \u015fimdiye dek \u00fcretmi\u015f oldu\u011fu enerjiden daha fazlad\u0131r. Manyetik alan boyunca ivmelenen y\u00fcksek enerjili elektronlar, iki farkl\u0131 yolla \u0131\u015f\u0131ma yapar.Bunlardan ilki detaylar\u0131 hen\u00fcz tam olarak bilinmese de koherent plazma gibi davranan elektronlar\u0131n radyo \u0131\u015f\u0131n\u0131m\u0131 yapmas\u0131yla olu\u015furken, ikincisi ise elektronlar\u0131nfotonlar veya manyetik alanlaetkile\u015fime girerek optik, X-\u0131\u015f\u0131n\u0131 ve gama-\u0131\u015f\u0131n\u0131 dalgaboylar\u0131nda \u0131\u015f\u0131ma yapmas\u0131yla ger\u00e7ekle\u015fir.<\/p>\n

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Tipik bir pulsar.<\/figcaption><\/figure>\n

Pulsarlar,basit\u00e7e d\u00f6nen n\u00f6tron y\u0131ld\u0131zlar\u0131 olarak tan\u0131mlan\u0131r. Pulsar ad\u0131 verilmesini sa\u011flayan at\u0131mlar\u0131n sebebiy\u0131ld\u0131z\u0131n d\u00f6nmesinden kaynaklan\u0131r. Manyetik kutuplar\u0131ndan uzaya do\u011fru \u0131\u015f\u0131k h\u0131z\u0131na yak\u0131n h\u0131zlarda par\u00e7ac\u0131k at\u0131mlar\u0131 yapan bu y\u0131ld\u0131zlar, kendi etraflar\u0131nda da \u00e7ok y\u00fcksek h\u0131zlarla d\u00f6nerler. Pulsar kendi etraf\u0131nda d\u00f6nerken, manyetik ekseni uzay boyunca bir alan\u0131 deniz feneri misali s\u00fcrekli olarak tarar. Okyanustaki bir geminin deniz fenerinden gelen \u0131\u015f\u0131\u011f\u0131n k\u0131rp\u0131\u015fmas\u0131n\u0131 g\u00f6rd\u00fc\u011f\u00fc gibi, pulsarlar\u0131n manyetik eksenleri D\u00fcnya\u2019ya y\u00f6neldi\u011finde \u0131\u015f\u0131k at\u0131m\u0131 g\u00f6zlenir. Pulsarlar\u0131n kendi ekseni etraf\u0131ndaki d\u00f6n\u00fc\u015fleri \u00e7ok h\u0131zl\u0131 oldu\u011fundan, bu at\u0131mlar k\u0131sa periyotlarla kendini g\u00f6sterir.<\/p>\n

Manyetik ekseni D\u00fcnya\u2019ya bakacak \u015fekilde d\u00f6nen bu y\u0131ld\u0131zlar, kesikli elektromanyetik at\u0131m yapan kaynaklar \u015feklinde g\u00f6zlemlenir.Esas\u0131nda n\u00f6tron y\u0131ld\u0131z\u0131n\u0131n yapt\u0131\u011f\u0131 \u0131\u015f\u0131ma s\u00fcreklidir, ancak y\u0131ld\u0131z\u0131n kendi etraf\u0131nda d\u00f6nmesinden dolay\u0131 sadece D\u00fcnya ve manyetik eksenin kesi\u015fti\u011fi noktalarda at\u0131m(pulse) yakalanabilir.<\/p>\n

En gen\u00e7 pulsarlar (atarcalar da denir), n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n do\u011fum yerleri olan s\u00fcpernova kal\u0131nt\u0131lar\u0131n\u0131n merkezinde bulunur. \u00d6rne\u011fin Yenge\u00e7 Nebulas\u0131n\u0131n merkezinde, Yenge\u00e7 Pulsar\u0131 bulunur. Bu gen\u00e7 pulsarlar uzayda \u00e7ok h\u0131zl\u0131 hareket ederler. Yeterince h\u0131zl\u0131 olanlar galaksiden d\u0131\u015far\u0131 \u00e7\u0131karak galaksileraras\u0131 ortamda yol al\u0131rken, galaksiden ka\u00e7acak kadar h\u0131zl\u0131 olmayanlar ise galaksi d\u00fczleminde sal\u0131n\u0131mlar yapar.<\/p>\n

Pulsarlar, \u00e7ok h\u0131zl\u0131 d\u00f6nen ve manyetik ekseni boyunca \u0131\u015f\u0131ma yapan n\u00f6tron y\u0131ld\u0131zlar\u0131 olarak tan\u0131mlansa da, manyetik eksenleri D\u00fcnya\u2019ya y\u00f6nelmeyen n\u00f6tron y\u0131ld\u0131zlar\u0131, pulsar olarak kendini g\u00f6stermez. Bunun d\u0131\u015f\u0131nda ge\u00e7mi\u015fte pulsar \u00f6zelli\u011fi g\u00f6steren baz\u0131 n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n radyasyon at\u0131mlar\u0131 tespit edilemeyecek kadar zay\u0131flam\u0131\u015f veya durmu\u015f olabilir. I\u015f\u0131ma at\u0131m mekanizmalar\u0131 hen\u00fcz tam olarak anla\u015f\u0131lm\u0131\u015f de\u011fildir.<\/p>\n

\"\"
Yenge\u00e7 Nebulan\u0131n merkezindeki Yenge\u00e7 Pulsar\u0131. Sol taraftaki g\u00f6rsel manyetik eksenin D\u00fcnya\u2019ya y\u00f6nelip at\u0131m\u0131n g\u00f6zlendi\u011fi, sa\u011f taraftaki ise manyetik eksenin D\u00fcnya\u2019ya y\u00f6nlenmedi\u011fi durumu g\u00f6steriyor.<\/figcaption><\/figure>\n

Pulsarlar\u0131n ke\u015ffi<\/strong><\/p>\n

Pulsarlar ilk olarak 1967\u2019de uzak galaksi ara\u015ft\u0131rmalar\u0131 yaparkenJocelyn Bell taraf\u0131ndan\u015fans eserike\u015ffedildi. Bell, teleskobun uzay\u0131n belirli bir b\u00f6lgesine bakt\u0131\u011f\u0131 s\u0131rada d\u00fczenli radyo \u0131\u015f\u0131k at\u0131mlar\u0131n\u0131n fark\u0131na vard\u0131.Bu d\u00fczenli radyo at\u0131mlar\u0131n\u0131n -k\u0131sa s\u00fcreli\u011fine de olsa- D\u00fcnya d\u0131\u015f\u0131 medeniyetlerden gelme olas\u0131l\u0131\u011f\u0131 bilim camias\u0131 taraf\u0131ndan g\u00f6z ard\u0131 edilmedi. Hatta ke\u015ffedilen bu at\u0131mlar-\u015fakayla kar\u0131\u015f\u0131k- \u201cK\u00fc\u00e7\u00fck Ye\u015fil Adam 1\u201d (Little Green Man 1, LGM1) olarak kodlanm\u0131\u015ft\u0131. Kayna\u011f\u0131 bilinmeyen bu radyo at\u0131m kaynaklar\u0131, daha sonra pulsar olarak adland\u0131r\u0131ld\u0131. Bell\u2019in ke\u015ffetmi\u015f oldu\u011fu ilk pulsar \u015fimdi \u201cPSR B1919+21\u201d olarak kodlanmaktad\u0131r. PSR, radyo at\u0131m\u0131 kayna\u011f\u0131(pulsating source of radio) oldu\u011funu i\u015faret ederken, B1919+21 ise g\u00f6ky\u00fcz\u00fcndeki konumunu tarif eder. Pulsarlar ilk olarak radyo \u0131\u015f\u0131n\u0131m kayna\u011f\u0131 olarak ke\u015ffedilse de, g\u00fcn\u00fcm\u00fczde optik, X-\u0131\u015f\u0131n\u0131 ve gama-\u0131\u015f\u0131n\u0131 teleskoplar\u0131nda da pulsarlar g\u00f6zlenmektedir.<\/p>\n

\"\"
Jocelyn Bell. Jocelyn Bell pulsarlar\u0131 hen\u00fcz 24 ya\u015f\u0131nda gen\u00e7 bir biliminsan\u0131yken ke\u015ffetti, ama bu ke\u015ffe verilen Nobel \u00d6d\u00fcl\u00fcn\u00fc o de\u011fil, tez dan\u0131\u015fman\u0131 Anthony Hewish ald\u0131.<\/figcaption><\/figure>\n

Jocelyn Bell, Cambridge\u2019deki teleskop ile ba\u015fka pulsar ke\u015fifleri de yapt\u0131. \u015eimdiye dek 1500\u2019\u00fcn \u00fczerinde pulsar g\u00f6zlendi ve gelecek y\u0131llarda binlercesi daha g\u00f6zlenmeyi bekliyor. G\u00f6zlenen pulsarlar\u0131n \u00fc\u00e7te ikisinden fazlas\u0131 Parkes Radyo Teleskobu ile tespit edildi. Parkes\u2019in yan\u0131 s\u0131ra Puerto Rico\u2019daki Arecibo Teleskobu, Amerika\u2019daki Green Bank Teleskobu ve Avustralya\u2019daki Molonglo Teleskobu ve \u0130ngiltere\u2019deki Jodrell Bank Teleskobu, pulsar ke\u015ffinde \u00f6nemli katk\u0131lar sa\u011flad\u0131.<\/p>\n

Pulsar ke\u015ffi yapmak isteyen bir astronom, radyo teleskobunu uzay\u0131n belirli bir noktas\u0131na birka\u00e7 dakikadan 12 saate kadar odaklar(Daha uzun g\u00f6zlemler zay\u0131f pulsarlar\u0131n yakalanmas\u0131n\u0131 sa\u011flayabilir, ancak ara\u015ft\u0131rmac\u0131lara b\u00fcy\u00fck bir i\u015f y\u00fck\u00fcn\u00fc de beraberinde getirir). Teleskoptan elde edilen veriler s\u00fcrekli olarak bilgisayara kaydedilir ve kay\u0131tlar detayl\u0131 analiz edilerek periyodik sinyaller aran\u0131r.<\/p>\n

Milisaniye pulsarlar\u0131 ve s\u0131radan pulsarlar<\/strong><\/p>\n

Art arda iki at\u0131m aras\u0131nda ge\u00e7en zaman, pulsar\u0131n periyodu olarak tan\u0131mlan\u0131r.1 saniye civar\u0131ndaki periyotlar, tipik pulsar periyotlar\u0131 olsa da, birka\u00e7 milisaniyelik k\u00fc\u00e7\u00fck periyotlardan 8 saniye gibi g\u00f6rece y\u00fcksek periyotlara sahip pulsarlar g\u00f6zlenmi\u015ftir.Pulsarlar\u0131n at\u0131mlar\u0131 aras\u0131ndaki zaman aral\u0131klar\u0131 son derece d\u00fczenli oldu\u011fundan periyot \u00f6l\u00e7\u00fcmleri hassas yap\u0131labilir. \u00d6rne\u011fin, PSR J1603-7202 pulsar\u0131n\u0131n periyodu tam olarak0,0148419520154668 saniyedir. Ancak milyon y\u0131lda 0,0000005 saniye kadar k\u00fc\u00e7\u00fck de olsa t\u00fcm radyo pulsarlar\u0131n\u0131n periyotlar\u0131 artmaktad\u0131r. Pulsarlar,birka\u00e7 milisaniyelik periyoda sahip ve periyodu \u00e7ok yava\u015f de\u011fi\u015fen milisaniye pulsarlar\u0131<\/strong>ve geri kalan s\u0131radan pulsarlar<\/strong> olmak \u00fczere ikiye ayr\u0131l\u0131r.<\/p>\n

Y\u0131ld\u0131zlar\u0131n bir\u00e7o\u011fu e\u015flik\u00e7i bir y\u0131ld\u0131z ile birlikte \u00e7ift y\u0131ld\u0131z sistemi olu\u015fturur. Benzer \u015fekilde bir\u00e7ok pulsar -\u00f6zellikle milisaniye pulsarlar\u0131- ikili sistem halindedir. \u0130kili sistemlerdeki pulsarlar\u0131n ara\u015ft\u0131r\u0131lmas\u0131, astronomlara pulsarlar hakk\u0131nda bir\u00e7ok bilgi verir. Pulsar tipleri, t\u00fcm milisaniye pulsarlar\u0131n\u0131n ba\u015fka bir y\u0131ld\u0131zla(veya y\u0131ld\u0131zlarla) y\u00f6r\u00fcngede olmas\u0131yla a\u00e7\u0131klanabilir. E\u015flik\u00e7i y\u0131ld\u0131zdan pulsara madde \u00e7ekildik\u00e7e pulsar daha h\u0131zl\u0131 d\u00f6nmeye ba\u015flar ve pulsar\u0131n at\u0131m frekanslar\u0131 milisaniye seviyelerine iner. Daha sonra e\u015flik\u00e7i y\u0131ld\u0131z ya\u015fam \u00f6mr\u00fcn\u00fc tamamlay\u0131p, ilk k\u00fctlesine ba\u011fl\u0131 olarak beyaz c\u00fcce, n\u00f6tron y\u0131ld\u0131z\u0131 veya kara deli\u011fe d\u00f6n\u00fc\u015f\u00fcr.E\u011fer e\u015flik\u00e7i y\u0131ld\u0131z kal\u0131nt\u0131s\u0131 pulsar ile y\u00f6r\u00fcngede kalmaya devam ederse, ikili milisaniye pulsar sistemi meydana gelebilir.<\/p>\n

Pulsar saatleri<\/strong><\/p>\n

Pulsarlar\u0131n y\u00fcksek h\u0131zl\u0131 d\u00f6n\u00fc\u015fleri ve \u00e7ok yava\u015f de\u011fi\u015fen periyotlar\u0131, hassas zaman \u00f6l\u00e7\u00fcmleri i\u00e7in de kullan\u0131lmaktad\u0131r. Radyo at\u0131mlar\u0131 aras\u0131ndaki d\u00fczenli zaman aral\u0131klar\u0131, bir saatin tik-taklar\u0131 olarak d\u00fc\u015f\u00fcn\u00fcld\u00fc\u011f\u00fcnde, saniyenin \u00e7ok k\u00fc\u00e7\u00fck kesrindeki zaman aral\u0131klar\u0131 d\u00fczg\u00fcn olarak \u00f6l\u00e7\u00fclebilir. Radyo teleskoplar\u0131 kullan\u0131larak, saniyenin 10 milyonda biri kadar k\u00fc\u00e7\u00fck zaman aral\u0131klar\u0131n\u0131n d\u00fczenli\u00f6l\u00e7\u00fcmleri yap\u0131lm\u0131\u015ft\u0131r. Bunun yan\u0131 s\u0131ra pulsar saatleri, periyotlar\u0131ndaki \u00e7ok yava\u015f de\u011fi\u015fimden \u00f6t\u00fcr\u00fc de biny\u0131llar boyunca geri kalmadan do\u011fru \u00f6l\u00e7\u00fcmler verebilir. Atomlar\u0131n elektronik ge\u00e7i\u015flerindeki frekanslar\u0131 \u00f6l\u00e7meye dayal\u0131 atom saatleri ile pulsar saatleri aras\u0131nda b\u00fcy\u00fck bir rekabet s\u00fcregelmektedir. G\u00fcn\u00fcm\u00fczderekabeti atom saatleri \u00f6nde s\u00fcrd\u00fcrse de\u2013ony\u0131llar gibi- uzun \u00f6l\u00e7\u00fcmler g\u00f6z \u00f6n\u00fcne al\u0131nd\u0131\u011f\u0131nda,pulsar saatleri de en az atom saatleri kadar ba\u015far\u0131l\u0131d\u0131r.<\/p>\n

\"\"
B0329+54 pulsar at\u0131mlar\u0131. Grafi\u011fin s\u0131\u00e7rama yapt\u0131\u011f\u0131 yerler at\u0131mlar; at\u0131mlar aras\u0131nda ge\u00e7en zaman da periyoda kar\u015f\u0131l\u0131k gelir.<\/figcaption><\/figure>\n

Pulsar saatleri, k\u00fctle\u00e7ekim(gravitasyon) dalgalar\u0131n\u0131n tespitinde de kullan\u0131labilecek \u00f6nemli ara\u00e7lardan biridir.Evrenin farkl\u0131 noktalar\u0131ndaki milisaniye pulsarlar\u0131 kullan\u0131larak adeta evrensel bir GPS sistemi kurulabilir. Ancak D\u00fcnya\u2019ya ula\u015fan olas\u0131 k\u00fctle\u00e7ekim dalgalar\u0131 ise pulsarlardan gelen at\u0131m sinyallerinde de\u011fi\u015fiklikler meydana getirir vesistemin senkronizasyonu bozulur. \u0130\u015fte bu bozulmag\u00f6zlemlenerek k\u00fctle\u00e7ekim dalgalar\u0131n\u0131n tespiti yap\u0131labilir. Ancak k\u00fctle\u00e7ekim dalgalar\u0131n\u0131n ke\u015fif yar\u0131\u015f\u0131, ge\u00e7ti\u011fimiz g\u00fcnlerdeLIGO\u2019nun (Laser Interferometer Gravitational-Wave Observatory, Lazer \u0130nterferometre K\u00fctle\u00e7ekim Dalgalar\u0131 G\u00f6zlemevi) k\u00fctle\u00e7ekim dalgalar\u0131n\u0131 yakalamas\u0131yla son bulmu\u015ftur. Yine de bu ve benzeri \u00e7al\u0131\u015fmalar, alan\u0131n ilerlemesi a\u00e7\u0131s\u0131ndan son derece \u00f6nemlidir.<\/p>\n

Sadece galaksimizde 1300\u2019den fazla n\u00f6tron y\u0131ld\u0131z\u0131 g\u00f6zlendi ve evrende milyarlarca daha oldu\u011fu \u00f6ng\u00f6r\u00fcl\u00fcyor.Pulsar ve n\u00f6tron y\u0131ld\u0131z\u0131 \u00e7al\u0131\u015fmalar\u0131, X-\u0131\u015f\u0131n\u0131 astronomisinden radyo astronomisine kadar geni\u015f bir \u00e7al\u0131\u015fma yelpazesi sunar. Pulsarlar son derece ilgin\u00e7 g\u00f6kcisimleridir. G\u00fcne\u015f\u2019in 1,5 kat\u0131 k\u00fctleye sahip olup \u0131\u015f\u0131k h\u0131z\u0131na yak\u0131n h\u0131zlarda d\u00f6nen bu yo\u011fun g\u00f6kcisimlerinin ortaya \u00e7\u0131kard\u0131\u011f\u0131 fiziksel fenomenler modern fizik ara\u015ft\u0131rmalar\u0131 i\u00e7in e\u015fsiz laboratuvarlard\u0131r.<\/p>\n

Kaynaklar<\/strong><\/p>\n

– https:\/\/people.highline.edu\/iglozman\/classes\/astronotes\/media\/2paths.jpg<\/p>\n

– http:\/\/imagine.gsfc.nasa.gov\/science\/objects\/pulsars1.html<\/p>\n

– http:\/\/www.cv.nrao.edu\/course\/astr534\/Pulsars.html<\/p>\n

– http:\/\/csep10.phys.utk.edu\/astr162\/lect\/pulsars\/pulsars.html<\/p>\n

– http:\/\/www.bbc.co.uk\/science\/space\/universe\/scientists\/jocelyn_bell_burnell<\/p>\n

– http:\/\/imagine.gsfc.nasa.gov\/Images\/basic\/xray\/pulsar.gif<\/p>\n

– http:\/\/www.tad.org.tr\/wp-content\/uploads\/2016\/01\/Discovery-of-Pulsars_detail.jpg<\/p>\n

– https:\/\/www.mpg.de\/7689623\/millisecond-pulsar-trio<\/p>\n

– http:\/\/www.astronomynow.com\/images\/090522millisecondpulsar.jpg<\/p>\n

– http:\/\/campus.pari.edu\/radiosky\/lessons\/pulsars\/10.shtml<\/p>\n

– http:\/\/imagine.gsfc.nasa.gov\/science\/objects\/pulsars2.html<\/p>\n

– http:\/\/www.bbc.com\/earth\/story\/20150805-the-most-accurate-clocks-in-space<\/p>\n","protected":false},"excerpt":{"rendered":"

Pulsarlar, kendi etraf\u0131nda \u00e7ok h\u0131zl\u0131 periyotlarda d\u00f6nen ve belirli bir eksende \u0131\u015f\u0131ma yapan n\u00f6tron y\u0131ld\u0131zlar\u0131d\u0131r. Bu mekanizma hen\u00fcz tam olarak anla\u015f\u0131lm\u0131\u015f de\u011fildir, ancak y\u0131ld\u0131zla birlikte d\u00f6nen \u00e7ok g\u00fc\u00e7l\u00fc manyetik alanla do\u011frudan ili\u015fkilidir. E\u011fer y\u0131ld\u0131z\u0131n \u0131\u015f\u0131ma yapt\u0131\u011f\u0131 eksen D\u00fcnya\u2019ya y\u00f6nelmi\u015f ise \u2013y\u0131ld\u0131z d\u00f6nd\u00fc\u011f\u00fc i\u00e7in- kesikli bir \u0131\u015f\u0131k vuru\u015fu g\u00f6zlemlenir. Bu kesikli\u011fin periyodu ise y\u0131ld\u0131za ba\u011fl\u0131 olarak […]<\/p>\n","protected":false},"author":634,"featured_media":16053,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[182,30,26],"tags":[247,1161,993,1883,404],"class_list":["post-16046","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-145-sayi","category-astronomi","category-fizik","tag-astrofizik","tag-kutlecekim","tag-manyetik-alan","tag-pulsar","tag-yildizlar"],"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