Astronomy:Quasi-star

From HandWiki
Short description: Hypothetical early-universe star with a black hole core
Size comparison of a hypothetical quasi-star to some of the largest known stars.
A quasi-star rendered with Celestia

A quasi-star (also called black hole star) is a hypothetical type of extremely massive and luminous star that may have existed early in the history of the Universe. Unlike modern stars, which are powered by nuclear fusion in their cores, a quasi-star's energy would come from material falling into a black hole at its core.[1]

Formation and properties

A quasi-star would have resulted from the core of a large protostar collapsing into a black hole, where the outer layers of the protostar are massive enough to absorb the resulting burst of energy without being blown away or falling into the black hole, as occurs with modern supernovae. Such a star would have to be at least 1,000 solar masses (2.0×1033 kg).[2] Quasi-stars may have also formed from dark matter halos drawing in enormous amounts of gas via gravity, which can produce supermassive stars with tens of thousands of solar masses.[3][4] Formation of quasi-stars could only happen early in the development of the Universe, before hydrogen and helium were contaminated by heavier elements; thus, they may have been very massive Population III stars.[5] Such stars would dwarf Mu Cephei, VV Cephei A, and VY Canis Majoris, three among the largest known modern stars.

Once the black hole had formed at the core of the protostar, it would continue generating a large amount of radiant energy from the infall of stellar material. This constant outburst of energy would counteract the force of gravity, creating an equilibrium similar to the one that supports modern fusion-based stars.[6] Quasi-stars would have had a short maximum lifespan, approximately 7 million years,[7] during which the core black hole would have grown to about 1,000–10,000 solar masses (2×1033–2×1034 kg).[1][6] These intermediate-mass black holes have been suggested as the progenitors of modern supermassive black holes such as the one in the center of the Galaxy.

Quasi-stars are predicted to have had surface temperatures higher than 10,000 K (9,700 °C).[6] At these temperatures, each one would be about as luminous as a small galaxy.[1] As a quasi-star cools over time, its outer envelope would become transparent, until further cooling to a limiting temperature of 4,000 K (3,730 °C).[6] This limiting temperature would mark the end of the quasi-star's life since there is no hydrostatic equilibrium at or below this limiting temperature.[6] The object would then quickly dissipate, leaving behind the intermediate mass black hole.[6]

See also


References

  1. ↑ 1.0 1.1 1.2 Battersby, Stephen (29 November 2007). "Biggest black holes may grow inside 'quasistars'". NewScientist.com news service. https://www.newscientist.com/article/dn12982-biggest-black-holes-may-grow-inside-quasistars.html#.Ut1FCftwHs0. 
  2. ↑ https://arxiv.org/abs/1102.5098
  3. ↑ Yasemin Saplakoglu (September 29, 2017). "Zeroing In on How Supermassive Black Holes Formed". Scientific American. https://www.scientificamerican.com/article/zeroing-in-on-how-supermassive-black-holes-formed1/. 
  4. ↑ Mara Johnson-Goh (November 20, 2017). "Cooking up supermassive black holes in the early universe". Astronomy. http://www.astronomy.com/news/2017/11/cooking-up-supermassive-black-holes. 
  5. ↑ Ball, Warrick H.; Tout, Christopher A.; Żytkow, Anna N.; Eldridge, John J. (2011-07-01). "The structure and evolution of quasi-stars: The structure and evolution of quasi-stars" (in en). Monthly Notices of the Royal Astronomical Society 414 (3): 2751–2762. doi:10.1111/j.1365-2966.2011.18591.x. Bibcode: 2011MNRAS.414.2751B. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Begelman, Mitch; Rossi, Elena; Armitage, Philip (2008). "Quasi-stars: accreting black holes inside massive envelopes". MNRAS 387 (4): 1649–1659. doi:10.1111/j.1365-2966.2008.13344.x. Bibcode: 2008MNRAS.387.1649B. 
  7. ↑ Schleicher, Dominik R. G.; Palla, Francesco; Ferrara, Andrea; Galli, Daniele; Latif, Muhammad (25 May 2013). "Massive black hole factories: Supermassive and quasi-star formation in primordial halos". Astronomy & Astrophysics 558: A59. doi:10.1051/0004-6361/201321949. Bibcode: 2013A&A...558A..59S. 

Further reading

  • Ball, Warrick H.; Tout, Christopher A.; Żytkow, Anna N.; Eldridge, John J. (2011). "The structure and evolution of quasi-stars". Monthly Notices of the Royal Astronomical Society 414 (3): 2751–2762. doi:10.1111/j.1365-2966.2011.18591.x. Bibcode: 2011MNRAS.414.2751B. 
  • Ball, Warrick H. (2012). "Quasi-stars and the Schönberg-Chandrasekhar limit". arXiv:1207.5972.
  • Czerny, Bozena; Janiuk, Agnieszka; Sikora, Marek; Lasota, Jean-Pierre (2012). "Quasi-Star Jets as Unidentified Gamma-Ray Sources". The Astrophysical Journal 755 (1): L15. doi:10.1088/2041-8205/755/1/L15. Bibcode: 2012ApJ...755L..15C. 
  • Fiacconi, Davide; Rossi, Elena M. (2017). "Light or heavy supermassive black hole seeds: The role of internal rotation in the fate of supermassive stars". Monthly Notices of the Royal Astronomical Society 464 (2): 2259–2269. doi:10.1093/mnras/stw2505. 
  • Herrington, Nicholas P.; Whalen, Daniel J.; Woods, Tyrone E. (2023). "Modelling supermassive primordial stars with <SCP>mesa</SCP>". Monthly Notices of the Royal Astronomical Society 521: 463–473. doi:10.1093/mnras/stad572. 
  • Dotan, Calanit; Rossi, Elena M.; Shaviv, Nir J. (2011). "A lower limit on the halo mass to form supermassive black holes". Monthly Notices of the Royal Astronomical Society 417 (4): 3035–3046. doi:10.1111/j.1365-2966.2011.19461.x. Bibcode: 2011MNRAS.417.3035D. 

External links



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Quasi-star&oldid=3426127"