Stellar black hole

A stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a massive star.[1] They have masses ranging from about 5 to several tens of solar masses.[2] The process is observed as a hypernova explosion[3] or as a gamma ray burst.[4] These black holes are also referred to as collapsars.

Properties

By the no-hair theorem, a black hole can only have three fundamental properties: mass, electric charge and angular momentum (spin). It is believed that black holes formed in nature all have some spin. The spin of a stellar black hole is due to the conservation of angular momentum of the star or objects that produced it.

The gravitational collapse of a star is a natural process that can produce a black hole. It is inevitable at the end of the life of a star, when all stellar energy sources are exhausted. If the mass of the collapsing part of the star is below the Tolman–Oppenheimer–Volkoff (TOV) limit for neutron-degenerate matter, the end product is a compact star — either a white dwarf (for masses below the Chandrasekhar limit) or a neutron star or a (hypothetical) quark star. If the collapsing star has a mass exceeding the TOV limit, the crush will continue until zero volume is achieved and a black hole is formed around that point in space.

The maximum mass that a neutron star can possess (without becoming a black hole) is not fully understood. In 1939, it was estimated at 0.7 solar masses, called the TOV limit. In 1996, a different estimate put this upper mass in a range from 1.5 to 3 solar masses.[5]

In the theory of general relativity, a black hole could exist of any mass. The lower the mass, the higher the density of matter has to be in order to form a black hole. (See, for example, the discussion in Schwarzschild radius, the radius of a black hole.) There are no known processes that can produce black holes with mass less than a few times the mass of the Sun. If black holes that small exist, they are most likely primordial black holes. Until 2016, the largest known stellar black hole was 15.65±1.45 solar masses.[6] In September 2015, a rotating black hole of 62±4 solar masses was discovered by gravitational waves as it formed in a merger event of two smaller black holes.[7] As of April 2008, XTE J1650-500 was reported by NASA[8] and others[9][10] to be the smallest-mass black hole currently known to science, with a mass 3.8 solar masses and a diameter of only 24 kilometers (15 miles). However, this claim was subsequently retracted. The more likely mass is 5–10 solar masses.

There is observational evidence for two other types of black holes, which are much more massive than stellar black holes. They are intermediate-mass black holes (in the centre of globular clusters) and supermassive black holes in the centre of the Milky Way and other galaxies.

X-ray compact binary systems

Stellar black holes in close binary systems are observable when matter is transferred from a companion star to the black hole. The energy release in the fall toward the compact star is so large that the matter heats up to temperatures of several hundred million degrees and radiates in X-rays (X-ray astronomy). The black hole therefore is observable in X-rays, whereas the companion star can be observed with optical telescopes. The energy release for black holes and neutron stars are of the same order of magnitude. Black holes and neutron stars are often difficult to distinguish.

However, neutron stars may have additional properties. They show differential rotation, and can have a magnetic field and exhibit localized explosions (thermonuclear bursts). Whenever such properties are observed, the compact object in the binary system is revealed as a neutron star.

The derived masses come from observations of compact X-ray sources (combining X-ray and optical data). All identified neutron stars have a mass below 2.0 solar masses. None of the compact systems with a mass above 2.0 solar masses display the properties of a neutron star. The combination of these facts make it more and more likely that the class of compact stars with a mass above 2.0 solar masses are in fact black holes.

Note that this proof of existence of stellar black holes is not entirely observational but relies on theory: We can think of no other object for these massive compact systems in stellar binaries besides a black hole. A direct proof of the existence of a black hole would be if one actually observes the orbit of a particle (or a cloud of gas) that falls into the black hole.

Black hole kicks

The large distances above the galactic plane achieved by some binaries are the result of black hole natal kicks. The velocity distribution of black hole natal kicks seems similar to that of neutron star kick velocities. One might have expected that it would be the momenta that were the same with black holes receiving lower velocity than neutron stars due to their higher mass but that doesn't seem to be the case,[11] which may be due to the fall-back of asymmetrically expelled matter increasing the momentum of the resulting black hole.[12]

Candidates

Our Milky Way galaxy contains several stellar-mass Black Hole Candidates (BHCs) which are closer to us than the supermassive black hole in the Galactic center region. Most of these candidates are members of X-ray binary systems in which the compact object draws matter from its partner via an accretion disk. The probable black holes in these pairs range from three to more than a dozen solar masses.[13][14][15]

NameBHC mass
(solar masses)		Companion mass
(solar masses )		Orbital period
(days)		Distance from Earth
(light years)		Location [16]
A0620-00/V616 Mon11 ± 22.6–2.80.33about 350006:22:44 -00:20:45
GRO J1655-40/V1033 Sco6.3 ± 0.32.6–2.82.85000−1100016:54:00 -39:50:45
XTE J1118+480/KV UMa6.8 ± 0.46−6.50.17620011:18:11 +48:02:13
Cyg X-111 ± 2≥185.66000–800019:58:22 +35:12:06
GRO J0422+32/V518 Per4 ± 11.10.21about 850004:21:43 +32:54:27
GRO J1719-24≥4.9~1.6possibly 0.6[17]about 850017:19:37 -25:01:03
GS 2000+25/QZ Vul7.5 ± 0.34.9–5.10.35about 880020:02:50 +25:14:11
V404 Cyg12 ± 26.06.57800±460[18]20:24:04 +33:52:03
GX 339-4/V821 Ara5–61.75about 1500017:02:50 -48:47:23
GRS 1124-683/GU Mus7.0 ± 0.60.43about 1700011:26:27 -68:40:32
XTE J1550-564/V381 Nor9.6 ± 1.26.0–7.51.5about 1700015:50:59 -56:28:36
4U 1543-475/IL Lupi9.4 ± 1.00.251.1about 2400015:47:09 -47:40:10
XTE J1819-254/V4641 Sgr7.1 ± 0.35–82.8224000 – 40000[19]18:19:22 -25:24:25
GRS 1915+105/V1487 Aql14 ± 4.0~133.5about 4000019:15:12 +10:56:44
XTE J1650-5009.7 ± 1.6 [20].0.32[21]16:50:01 -49:57:45
GW150914 (62 ± 4) M☉36 ± 429 ± 4.1.3 billion
GW151226 (21.8 ± 3.5) M☉ 14.2 ± 6 7.5 ± 2.3 . 2.9 billion
GW170104 (48.7 ± 5) M☉ 31.2 ± 7 19.4 ± 6 . 1.4 billion

The disappearance of N6946-BH1 following a failed supernova in NGC 6946 may have resulted in the formation of a black hole.[22]

See also

References

  1. ↑ Celotti, A.; Miller, J.C.; Sciama, D.W. (1999). "Astrophysical evidence for the existence of black holes". Classical and Quantum Gravity. 16 (12A): A3–A21. arXiv:astro-ph/9912186. doi:10.1088/0264-9381/16/12A/301.
  2. ↑ Hughes, Scott A. (2005). "Trust but verify: The case for astrophysical black holes". arXiv:hep-ph/0511217.
  3. ↑ "HubbleSite: Black Holes: Gravity's Relentless Pull interactive: Encyclopedia". hubblesite.org. Retrieved 2018-02-09.
  4. ↑ "HubbleSite: Black Holes: Gravity's Relentless Pull interactive: Encyclopedia". hubblesite.org. Retrieved 2018-02-09.
  5. ↑ I. Bombaci (1996). "The Maximum Mass of a Neutron Star". Astronomy and Astrophysics. 305: 871–877. Bibcode:1996A&A...305..871B. .
  6. ↑ Nature 449, 799–801 (18 October 2007)
  7. ↑ Abbott, BP; et al. (2016). "Observation of Gravitational Waves from a Binary Black Hole Merger". Phys. Rev. Lett. 116 (6): 061102. arXiv:1602.03837. Bibcode:2016PhRvL.116f1102A. doi:10.1103/PhysRevLett.116.061102. PMID 26918975.
  8. ↑ "NASA - NASA Scientists Identify Smallest Known Black Hole". nasa.gov.
  9. ↑ "HOUSTON, WE'VE HAD A PROBLEM". Astronomy.com.
  10. ↑ "Smallest, lightest black hole ever is identified". 1 April 2008.
  11. ↑ Investigating stellar-mass black hole kicks, Serena Repetto, Melvyn B. Davies, Steinn Sigurdsson, (Submitted on 14 Mar 2012 (v1), last revised 19 Jun 2012 (this version, v2))
  12. ↑ Natal Kicks of Stellar-Mass Black Holes by Asymmetric Mass Ejection in Fallback Supernovae, H.-Thomas Janka (Max Planck Institute for Astrophysics, Garching) (Submitted on 31 May 2013)
  13. ↑ J. Casares: Observational evidence for stellar-mass black holes. Preprint
  14. ↑ Garcia, M.R.; et al. "Resolved Jets and Long Period Black Hole Novae". arXiv:astro-ph/0302230.
  15. ↑ J.E. McClintock and R.A. Remillard: Black Hole Binaries. Preprint
  16. ↑ ICRS coordinates obtained from SIMBAD. Format: right ascension (hh:mm:ss) ±declination (dd:mm:ss).
  17. ↑ Masetti, N.; Bianchini, A.; Bonibaker, J.; della Valle, M.; Vio, R. (1996), "The superhump phenomenon in GRS 1716-249 (=X-Ray Nova Ophiuchi 1993)", Astronomy and Astrophysics, 314
  18. ↑ Miller-Jones, J. A. C.; Jonker; Dhawan (2009). "The first accurate parallax distance to a black hole". The Astrophysical Journal Letters. 706 (2): L230. arXiv:0910.5253. Bibcode:2009ApJ...706L.230M. doi:10.1088/0004-637X/706/2/L230.
  19. ↑ Orosz; et al. "A Black Hole in the Superluminal source SAX J1819.3-2525 (V4641 Sgr)". arXiv:astro-ph/0103045v1.
  20. ↑ Shaposhnikov, N.; Titarchuk, L. (2009). "Determination of Black Hole Masses in Galactic Black Hole Binaries using Scaling of Spectral and Variability Characteristics" (PDF). The Astrophysical Journal. 699 (1). doi:10.1088/0004-637X/699/1/453.
  21. ↑ Orosz, J.A.; et al. (2004). "Orbital Parameters for the Black Hole Binary XTE J1650–500". The Astrophysical Journal. 616 (1): 376–382. Bibcode:2004ApJ...616..376O. doi:10.1086/424892.
  22. ↑ Adams, S. M.; Kochanek, C. S; Gerke, J. R.; Stanek, K. Z.; Dai, X. (9 September 2016). "The search for failed supernovae with the Large Binocular Telescope: conformation of a disappearing star". arXiv:1609.01283v1 [astro-ph.SR].

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.