Nigri fore

Un nigri fore es un region de spacie-témpor u gravitation es talmen fort que necós, includent lúmine o altri undes electromagnetic, posse escapar it.^[2] Li teorie de relativitá general predi que un suficientmen compact masse posse deformar spacie-tempor de formar un nigri fore.^[3]^[4] Li limite de null escapada es nominat li horizonte de eventus. Benque it have un grand efecte sur li cosa que passa it, li horizonte de eventus have null localmen detectibil trates, secun general relativitá.^[5] In multi aspectes, un fore nigri acte quam un perfect córpor nigri, pro que it reflecte null luce.^[6]^[7]

Animat simulation de un Schwarzschild nigri fore con un galaxe passar in detra. Circa li tempor de alineament, extrem gravitational linsation del galaxe es observat.

Nigri fores de stellic masse forma quande massiv stelles implode al fine de lor evolution stellari. Pos un nigri fore ha format, it posse crescer per absorpter masse de su circumité. Supermassiv nigri fores de milliones de solari masses posse formar per absorpter altri stelles e coalescer con altri nigri fores. Astronomes concorda que supermassiv nigri fores existe in li centres de max galaxes.

Li presentie de un nigri fore es inferer per su interaction con altri materie e con radiation electromagnetic, quam visibil lúmine. Omni materie que cade sur un nigri fore posse formar un extern acretion disco calentat per friction. To forma quasares, alcun del max brilliant objectes in li universe. Stelles passar tro proxim a un supermassiv nigri fore posse esser dispezzat ad-in banderoles que brilliar tre clarmen ante li fore "ingloti" les.^[8] Si atrie stelles orbita un nigri fore, lor orbites posse esser usat de determinar li masse e loco del fore. Tal observationes es usat de excluder possibil alternatives quam neutronic stelles. Per ti metodes, astronomes ha identificat numerosi possibil stellari nigri fores in duplic sistemes e constatat que li fonte de radio-undes savet quam Sagittario A*, al cordie de nor galaxe, contene un supermassiv nigri fore de circa 4,3 million solari masses.

Vide anc

Referenties

↑ Oldham, L. J.: Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales. In: Monthly Notices of the Royal Astronomical Society. 457, Nr. 1, March 2016, S. 421–439
↑ Avise:Harvnb
↑ Wald, R. M. (1997). "Gravitational Collapse and Cosmic Censorship", Black Holes, Gravitational Radiation and the Universe. Dordrecht: Springer, 69–86. doi:10.1007/978-94-017-0934-7. ISBN 978-9401709347.
↑ Avise:Cite news
↑ Hamilton, A.. "Journey into a Schwarzschild black hole."
↑ (2003) Gravity from the ground up. Cambridge University Press, 110. ISBN 978-0-521-45506-0.
↑ P. C. W. Davies: Thermodynamics of Black Holes. In: Reports on Progress in Physics. 41, Nr. 8, 1978, S. 1313–1355
↑ Clery D: Black holes caught in the act of swallowing stars. In: Science. 367, Nr. 6477, 2020

[1] Oldham, L. J.: Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales. In: Monthly Notices of the Royal Astronomical Society. 457, Nr. 1, March 2016, S. 421–439

[2] Avise:Harvnb

[wald_1997-3] Wald, R. M. (1997). "Gravitational Collapse and Cosmic Censorship", Black Holes, Gravitational Radiation and the Universe. Dordrecht: Springer, 69–86. doi:10.1007/978-94-017-0934-7. ISBN 978-9401709347.

[NYT-20150608-4] Avise:Cite news

[HamiltonA-5] Hamilton, A.. "Journey into a Schwarzschild black hole."

[6] (2003) Gravity from the ground up. Cambridge University Press, 110. ISBN 978-0-521-45506-0.

[7] P. C. W. Davies: Thermodynamics of Black Holes. In: Reports on Progress in Physics. 41, Nr. 8, 1978, S. 1313–1355

[pmid32001633-8] Clery D: Black holes caught in the act of swallowing stars. In: Science. 367, Nr. 6477, 2020

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