Quasi-star

"Black hole star" redirects here. For black holes created from stars, see Stellar black hole. For stars that become black holes, see Supernova. For types of stars denser than neutron stars, see Exotic star. For the 1994 Soundgarden song, see Black Hole Sun.

Not to be confused with a quasi-stellar object or quasar.

Size comparison of a hypothetical quasi-star to some of the largest known stars.

A quasi-star rendered with Celestia

A quasi-star or quasistar (QS), also called a 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. The formation of such an object would have resulted from the core of a large supermassive protostar collapsing into a stellar-mass 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 supernovae. They are dubbed as such as they would resemble red giants in structure to an external observer, but scaled-up and powered by an accreting central black hole with luminosities comparable to a Seyfert nucleus.

Quasi-stars were first hypothesized in 2006; although a confirmed observation has not yet been made, potential sightings of these objects have been reported by the James Webb Space Telescope since its launch. The study of quasi-stars would provide valuable insight into the early universe, galaxy formation, and the behavior of black holes, namely because they are considered as possible progenitors of the modern supermassive black holes that formed soon after the Big Bang, such as the one in the center of the Galaxy. Little red dots, such as one called The Cliff are possible examples.

Structure

Although different models exist for the structure of a quasi-star, it is generally thought to consist of a photospheric star-like envelope (which contains the bulk of the star's mass) surrounded by a radiative layer and an innermost region as the core, which includes a black hole embryo within. This overlying envelope is highly convective and supported by radiation pressure. According to recent models, it may also become adiabatic during a quasi-star's late stage, with an inner saturated-convection region forming by that time, thereby conforming to a convection-dominated accretion flow around the black hole. The quasi-star would also have a porous atmosphere around the convective envelope, where convection becomes inefficient. In a 2011 model for the structure of a super-Eddington quasi-star with masses over a million M_☉ where it would suffer substantial mass loss due to its extreme luminosity, its strong stellar wind appears as optically thick surface and hence appears as a cooler extended pseudo-photosphere above the porous atmosphere, where the optical density of the wind drops to near zero, typically measured at a particular Rossland opacity value such as 2⁄3. Photon tired winds appear between both.

A thin pre-galactic disk also surrounds the quasi-star, in which the star feeds it at rates from 2×10⁻³ to a few of tens of M_☉ per year. The black hole within the core would accrete rapidly the surrounding gas from the envelope through a convectively or advectively dominated thick accretion disc or via quasi-spherical accretion, with at least 10⁻⁴ to several M_☉ per year, possibly up to a highly super-Eddington accretion rate. The accretion rate onto the black hole energetically sustains the gaseous envelope, but its limit is often set by the Eddington limit of the entire object, which is initially much larger than that of the black hole alone. The excess energy is carried away by convection. Analogous to active galactic nuclei and gamma-ray bursts, the rotation of the quasi-star alongside the poloidal magnetic fields in the black hole or disk magnetosphere (or both) may mediate the production of a relativistic jet, and they may be transported from the outer regions to the center only thanks to thick accretion flows. This would produce gamma rays in the reconfinement shocks formed within one-hundredth to one times the quasi-star's radius.

Formation and properties

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. A quasi-star would have resulted from the core of a protostar of at least 1,000 solar masses (2.0×10³³ kg) collapsing into a black hole, where the outer layers of the protostar are massive enough to absorb the resulting supernova without being blown away. 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. In either case, quasi-stars would have ballooned to enormous sizes, dwarfing the largest known modern stars and approaching the Solar System in size. They are predicted to have had surface temperatures higher than 10,000 K (9,700 °C). At these temperatures, each one would be about as luminous as a small galaxy.

Once the black hole had formed at the core of a new quasi-star, 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. Quasi-stars would have had a short maximum lifespan, approximately 7 to 10 million years, during which the core black hole would have grown to about 1,000–10,000 solar masses (2×10³³–2×10³⁴ kg).

As a quasi-star cooled over time, its outer envelope would become transparent, until further cooling to a limiting temperature of 4,000 K (3,730 °C). This would mark the end of the quasi-star's life since there is no hydrostatic equilibrium at or below this limiting temperature. It would then dissipate without a supernova, leaving behind an intermediate-mass black hole. These intermediate-mass black holes are theorized as the progenitors of modern supermassive black holes, and would help explain how supermassive black holes formed so early in the history of the universe.

See also

• Accretion (astrophysics) – Accumulation of particles into a massive object by gravitationally attracting more matter
• Accretion disk – Structure formed by diffuse material in orbital motion around a massive central body
• Blitzar – Hypothetical type of neutron star
• Thorne–Żytkow object – Hypothetical hybrid star type
• Neutron star – Collapsed core of a massive star
• Quasar – Active galactic nucleus (AGN) containing a supermassive black hole
• Direct collapse black hole – High-mass black hole seeds

Further reading

• Ball, Warrick H. (2012). "Quasi-stars and the Schönberg-Chandrasekhar limit". arXiv:1207.5972 [astro-ph.SR].
• 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. arXiv:1604.03936. 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. arXiv:2208.00008. doi:10.1093/mnras/stad572.

External links

• "Quasi-Stars: Black Holes at the Core of the Universe's Largest Stars". 16 May 2020.
• Kurzgesagt (15 December 2022), Black Hole Star – The Star That Shouldn't Exist