Jump to content

Draft:Supermassive star

From Wikipedia, the free encyclopedia

A supermassive star (SMS) is a hypothetical type of extremely massive and luminous star with its mass being on the order of more than a thousand times the mass of the Sun (M☉).[1][2] Such stars may have existed early in the universe (i.e., at high redshift) and may have produced high-mass black hole seeds like direct collapse black holes (DCBHs).[3]

Description

[edit]
  • Proposed subtypes of supermassive stars:
    • Haemmerlé et al. 2020:[3]
    • Zinnecker et al. 2007: Although the term "ultramassive star" ("UMS") is rarely used, it has been once used to refer massive stars between 1,000 and 10,000 M☉.[4]

Formation and properties

[edit]
  • Formation: The environmental physical conditions to form a supermassive star are the following:
  1. Atomic-cooling gas.
  2. Galaxy merger
  3. Sufficiently large flux of Lyman–Werner photons, in order to destroy hydrogen molecules, which are very efficient gas coolants.
  4. A computer simulation reported in July 2022 showed that a halo at the rare convergence of strong, cold accretion flows can create massive black holes seeds without the need for ultraviolet backgrounds, supersonic streaming motions, or even atomic cooling. Cold flows produced turbulence in the halo, which suppressed star formation. In the simulation, no stars formed in the halo until it had grown to 40 million solar masses at a redshift of 25.7 when the halo's gravity was finally able to overcome the turbulence; the halo then collapsed and formed two supermassive stars that died as DCBHs of 31,000 and 40,000 M☉.[5][6]
  • Evolution as "red supergiant protostars": Depending on models, several studies had predicted that supermassive stars could have evolved "red supergiant protostars" as high accretion rates would prevent stars to contract, resulting lower temperatures and radii reaching up to many tens of thousands of R☉, comparable to some of the largest known black holes.[7] Such stars would have been significantly larger than the largest modern red supergiant stars (such as VY Canis Majoris and Mu Cephei) found in the Local Group.[8][9]
  • Metal-rich: Research predicted that metal-rich supermassive stars may have been able to form from the merging of metal-rich protogalaxies.[10][11]
  • Overall summary of the stellar structure:
  • Extremely early epoch:
  • Modern era, globular clusters:
  • Brief talk about formation of stars like R136a1:

End of stellar life

[edit]

Direct collapse

[edit]
Main article: Direct collapse black hole
  • A 2018 study proposed a new model for the direct collapse route.[13]
  • A scenario whereas a DCBH is formed without stellar phase is called "dark collapse".[14]

Various other researchers have proposed alternative scenarios for the fate of a supermassive star, although this depends directly on the star's properties.

General relativistic supernova

[edit]

Quasi-star phase

[edit]
Main article: Quasi-star
  • Short summary:
  • After the QS phase per old models and studies:
  • Coughlin et al. 2024 model:
  • Objections, to be shortened: Models from a 2023 paper, although they did not follow the collapse of supermassive stars to late times, predicted that X-rays from the central black hole is unlikely to halt the collapse of stars with final masses of (3.5–370)×103 M☉ due to too large infall velocities (that enclose most of the stellar mass), thus instead resulting a direct collapse black hole.[10]

Bar-mode instability

[edit]

Although thermal emission from a rotating supermassive star will cause the configuration to contract slowly and spin up, the contracting and cooling star may rotate differentially if internal viscosity and magnetic fields are weak enough and will likely encounter the dynamical bar mode instability, which may trigger the growth of nonaxisymmetric bars.[15]

Post-main sequence

[edit]
  • Mass loss until becoming a few 100-solar-masses sub-Eddington star:[12]

Difference from supermassive nuclear-powered stars and dark stars

[edit]
Main article: Dark star (dark matter)
  • Will also mention the dark star formation:

References

[edit]
  1. ^ Gieles, Mark; Charbonnel, Corinne (2019). "Supermassive stars as the origin of the multiple populations in globular clusters". Proceedings of the International Astronomical Union. 14: 297–301. arXiv:1908.02075. doi:10.1017/S1743921319007658. S2CID 199452725.
  2. ^ Pasachoff, Jay M. (2018). "Supermassive star". Access Science. doi:10.1036/1097-8542.669400.
  3. ^ a b Haemmerlé, Lionel; Heger, Alexander; Woods, Tyrone E. (2020). "On monolithic supermassive stars". Monthly Notices of the Royal Astronomical Society. 494 (2): 2236–2243. arXiv:2003.10467. doi:10.1093/mnras/staa763.
  4. ^ Zinnecker, Hans; Yorke, Harold W. (2007). "Toward Understanding Massive Star Formation". Annual Review of Astronomy and Astrophysics. 45 (1): 481–563. arXiv:0707.1279. Bibcode:2007ARA&A..45..481Z. doi:10.1146/annurev.astro.44.051905.092549.
  5. ^ "Revealing the origin of the first supermassive black holes". Nature. 6 July 2022. doi:10.1038/d41586-022-01560-y. PMID 35794378. State-of-the-art computer simulations show that the first supermassive black holes were born in rare, turbulent reservoirs of gas in the primordial Universe without the need for finely tuned, exotic environments — contrary to what has been thought for almost two decades.
  6. ^ "Scientists discover how first quasars in universe formed". phys.org. Provided by University of Portsmouth. 6 July 2022. Retrieved 2 August 2022.
  7. ^ Haemmerlé, Lionel; Woods, T. E.; Klessen, Ralf S.; Heger, Alexander; Whalen, Daniel J. (2018). "The evolution of supermassive Population III stars". Monthly Notices of the Royal Astronomical Society. 474 (2): 2757–2773. arXiv:1705.09301. doi:10.1093/mnras/stx2919.
  8. ^ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. ISSN 0004-637X. S2CID 15109583.
  9. ^ El-Badry, Kareem (22 April 2024). "On the formation of a 33 solar-mass black hole in a low-metallicity binary". The Open Journal of Astrophysics. 7: 38. arXiv:2404.13047. Bibcode:2024OJAp....7E..38E. doi:10.33232/001c.117652.
  10. ^ a b 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.
  11. ^ Haemmerlé, L.; Klessen, R. S.; Mayer, L.; Zwick, L. (2021). "Maximum accretion rate of supermassive stars". Astronomy & Astrophysics. 652: L7. arXiv:2105.13373. Bibcode:2021A&A...652L...7H. doi:10.1051/0004-6361/202141376. S2CID 235247984.
  12. ^ a b c d e f g h i Dotan, C.; Shaviv, N. J. (2012). "The super-Eddington nature of supermassive stars". Monthly Notices of the Royal Astronomical Society. 427 (4): 3071–3080. arXiv:1203.4372. Bibcode:2012MNRAS.427.3071D. doi:10.1111/j.1365-2966.2012.22020.x.
  13. ^ Mayer, Lucio; Bonoli, Silvia (2019). "The route to massive black hole formation via merger-driven direct collapse: A review". Reports on Progress in Physics. 82 (1): 016901. arXiv:1803.06391. Bibcode:2019RPPh...82a6901M. doi:10.1088/1361-6633/aad6a5. PMID 30057369. S2CID 51865966.
  14. ^ Mayer, Lucio; Bonoli, Silvia (2019). "The route to massive black hole formation via merger-driven direct collapse: A review". Reports on Progress in Physics. 82 (1): 016901. arXiv:1803.06391. Bibcode:2019RPPh...82a6901M. doi:10.1088/1361-6633/aad6a5. PMID 30057369.
  15. ^ New, Kimberly C. B.; Shapiro, Stuart L. (2001). "Evolution of Differentially Rotating Supermassive Stars to the Onset of Bar Instability". The Astrophysical Journal. 548 (1): 439–446. arXiv:astro-ph/0010172. Bibcode:2001ApJ...548..439N. doi:10.1086/318662.

Further reading

[edit]
[edit]
Retrieved from "https://en.wikipedia.org/w/index.php?title=Draft:Supermassive_star&oldid=1291355419"