[[File:Black hole - Messier 87.jpg|thumb|upright=1.35|right|ब्लैक होल के चित्र]]
'''ब्लैक होल''' ({{Lang-en|Black hole}}) एगो ज्यामितीय रूप से परिभाषित, [[स्पेस-टाइम]] के अइसन क्षेत्र बा, जवना के अंदर एतना ढेर गुरुत्वाकर्षण होला के ओह में से कण या इलेक्ट्रो-मैग्नेटिक रेडियेशन (प्रकाश) भी बाहर न निकल सके।<ref>{{harvnb|Wald|1984|pp=299–300}}</ref> The theory of [[generalरिलेटिविटी relativityके जनरल थियरी]] predictsई thatबतावे aले sufficientlyकी compactअगर [[mass]]द्रब्यमान canभरपूर deformमात्रा [[spacetime]]में toकांपैक्ट formहो aजाय blackतब hole.ऊ स्पेस-टाइम के रूप बदल के ब्लैक होल के निर्माण करे में सक्षम हो सके ला।<ref name="wald 1997">{{cite book |last=Wald |first=R. M. |author-link=Robert Wald |title=Black Holes, Gravitational Radiation and the Universe |editor1=Iyer, B. R. |editor2=Bhawal, B. |chapter=Gravitational Collapse and Cosmic Censorship |arxiv=gr-qc/9710068 |date=1997 |pages=69–86 |publisher=Springer |doi=10.1007/978-94-017-0934-7 |isbn=978-9401709347}}</ref><ref name="NYT-20150608">{{cite news |last=Overbye |first=Dennis |authorlink=Dennis Overbye |title=Black Hole Hunters |url=https://www.nytimes.com/2015/06/09/science/black-hole-event-horizon-telescope.html |date=8 June 2015 |work=[[NASA]] |accessdate=8 June 2015 |url-status=live |archiveurl=https://web.archive.org/web/20150609023631/http://www.nytimes.com/2015/06/09/science/black-hole-event-horizon-telescope.html |archivedate=9 June 2015}}</ref> Theअइसन boundaryसीमा ofजहाँ theसे regionकौनों fromचीज whichफिर noबहरें escapeन isनिकल possibleसके isइवेंट calledहोराइजन theकहल [[eventजाला। horizon]].भले Althoughएह theइवेंट eventहोराइजन horizonके hasभारी anपरभाव enormousएकरा effectके onक्रास theकरे fateवाला andचीज circumstancesके of anदशा-दिशा objectपर crossingपड़त itहोखे, noकौनों locallyलोकल detectableफीचर featuresइहाँ appearसे toहमनी beके observed.डिटेक्ट ना हो पावे ला।<ref>{{cite web |url=https://www.socratease.in/chapters/intro-to-black-holes-1 |title=Introduction to Black Holes |access-date=26 September 2017}}</ref> Inकई manyपरकार waysसे, aब्लैक blackहोल holeसभ actsआदर्श likeब्लैकबॉडी anके idealरूप [[blackमें बेहवार body]]करे ला, asमने itकी reflectsकौनों noप्रकाश light.के रिफ्लेक्ट ना करे ला।<ref>{{cite book |title=Gravity from the ground up |edition= |first1=Bernard F. |last1=Schutz |authorlink1=Bernard F. Schutz |publisher=Cambridge University Press |date=2003 |isbn=978-0-521-45506-0 |page=110 |url=https://books.google.com/books?id=P_T0xxhDcsIC |url-status=live |archiveurl=https://web.archive.org/web/20161202222711/https://books.google.com/books?id=P_T0xxhDcsIC |archivedate=2 December 2016}}</ref><ref>{{cite journal |last=Davies |first=P. C. W. |authorlink1=Paul Davies |title=Thermodynamics of Black Holes |url=http://cosmos.asu.edu/publications/papers/ThermodynamicTheoryofBlackHoles%2034.pdf |journal=[[Reports on Progress in Physics]] |volume=41 |date=1978 |issue=8 |pages=1313–1355 |doi=10.1088/0034-4885/41/8/004 |bibcode=1978RPPh...41.1313D |ref=harv |url-status=dead |archiveurl=https://web.archive.org/web/20130510184530/http://cosmos.asu.edu/publications/papers/ThermodynamicTheoryofBlackHoles%2034.pdf |archivedate=10 May 2013 |df=}}</ref> Moreoverहालाँकि, [[quantumवक्राकार fieldस्पेसटाइम theoryके inक्वांटम curvedफ़ील्ड spacetime]]थियरी predictsई thatप्रेडिक्ट eventकरे horizonsले emitकी [[Hawkingइवेंट radiation]],होराइजन withसे [[thermalहॉकिंग radiation|theरेडियेशन sameनिकले spectrum]]ला asजवन aकी [[Black-bodyओही radiation|blackस्पेक्ट्रम body]]में ofहोला aजवन temperatureकी inverselyकौनों proportionalब्लैकबॉडी toअपना itsद्रब्यमान mass.के Thisउल्टा temperatureअनुपात isवाला onतापमान theमें orderकरी। ofअब billionthsचूँकि ofब्लैकहोल aसभ [[kelvin]]में forद्रब्यमान [[stellarएतना blackबेसी hole|blackहोला holesकी ofअइसन stellarतापमान mass]],एक makingकेल्विन itके essentiallyखरबवाँ impossibleहिस्सा toभर होखे ला observe.आ अइसन रेडियेशन के डिटेक्ट कइल लगभग असंभव बाटे।
Objects whose [[gravitational field]]s are too strong for light to escape were first considered in the 18th century by [[John Michell]] and [[Pierre-Simon Laplace]].<ref name=origin /> The first modern solution of general relativity that would characterize a black hole was found by [[Karl Schwarzschild]] in 1916, although its interpretation as a region of space from which nothing can escape was first published by [[David Finkelstein]] in 1958. Black holes were long considered a mathematical curiosity; it was during the 1960s that theoretical work showed they were a generic prediction of general relativity. The discovery of [[neutron star]]s by [[Jocelyn Bell Burnell]] in 1967 sparked interest in [[gravitational collapse|gravitationally collapsed]] compact objects as a possible astrophysical reality.
