Sun black hole formation
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Black Hole Formation from Massive Stars at Solar Metallicity
Research shows that black holes can form from the collapse of massive stars, even at solar metallicity. For example, simulations of a 40 solar mass star with solar metallicity demonstrate that after a supernova explosion, a black hole can form within about 1.5 seconds. The resulting black hole initially has a mass of around 2.3 solar masses, and it can continue to grow as it accretes more material. The explosion is highly asymmetrical, and the black hole can receive a significant "kick" velocity. This process is one of several channels for black hole formation from stars with solar-like composition, and it suggests that about 20% of such massive stars could end their lives as black holes rather than neutron stars. The final mass and velocity of the black hole depend on the details of the explosion and subsequent accretion .
Formation of Massive Black Holes in Binary Systems
At solar and sub-solar metallicities, especially in binary star systems, black holes with masses between 50 and 80 solar masses can form if a large fraction of matter is accreted onto a low-mass black hole during a merger event. This process, involving a so-called "black hole Thorne-Zytkow object," is more likely if more than 70% of the available matter is accreted. In environments with lower metallicity, such as globular clusters, black holes can reach even higher masses, up to 100 solar masses. The spin of these black holes can vary, and in some cases, they may have low spin if formed through this merger process .
Primordial Black Holes and the Sun
Some theories propose that primordial black holes, formed shortly after the Big Bang, could be captured by stars like the Sun. If a small primordial black hole were present at the Sun's center, it could slowly accrete material and potentially affect the Sun's evolution. However, current models suggest that the lightest primordial black holes would have little to no effect on the Sun, while more massive ones could eventually consume the star, leading to observable changes such as a dimming of the Sun and changes in its structure and luminosity. These scenarios remain speculative, and there is no evidence that the Sun currently harbors a black hole Bellinger2023Caplan2023.
Dark Matter, Black Holes, and Solar System Bodies
Dark matter could accumulate in the centers of stars and planets, potentially forming small black holes if certain conditions are met. If a black hole formed in this way is large enough, it could grow and eventually destroy the host star or planet. Alternatively, smaller black holes could evaporate via Hawking radiation, producing detectable heat or high-energy neutrinos. These processes provide constraints on dark matter properties and offer potential observational signatures, such as unusual heat flows or neutrino emissions from the Sun Acevedo2020Riofrio2024.
Conclusion
Black hole formation in solar-like environments can occur through the collapse of massive stars, especially in binary systems, and may also involve exotic scenarios such as the capture of primordial black holes or the accumulation of dark matter. While the Sun itself is not expected to form a black hole under normal circumstances, these processes are important for understanding the life cycles of stars and the possible role of black holes in stellar and planetary evolution Banerjee2019Bellinger2023Burrows2023+3 MORE.
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