1. Radiation Pressure:
* As a star grows more massive, its core temperature and pressure also increase. This leads to an increase in the rate of nuclear fusion, generating more energy.
* This energy is released as radiation, which exerts outward pressure on the star's outer layers.
* If the radiation pressure becomes too strong, it can overcome the inward gravitational pull, leading to instability and preventing further accretion of matter.
2. Eddington Limit:
* The Eddington Limit describes the maximum luminosity a star can achieve before radiation pressure overwhelms gravity.
* This limit is determined by the balance between the outward force of radiation pressure and the inward force of gravity.
* Stars exceeding the Eddington Limit will lose mass through powerful stellar winds.
3. Stellar Wind:
* Massive stars have extremely strong stellar winds, which continuously blow away material from their surface.
* This mass loss is exacerbated by radiation pressure and can limit the star's ability to accrete more matter.
4. Instability in Nuclear Fusion:
* The fusion processes within a star's core can become unstable if the mass is too large.
* This instability can lead to the star rapidly ejecting large amounts of matter.
5. Pair-Instability Supernova:
* For stars with masses exceeding about 100 solar masses, a phenomenon known as "pair-instability" can occur.
* This instability results in the production of electron-positron pairs, which weakens the radiation pressure and triggers a runaway collapse leading to a powerful supernova explosion.
The Estimated Maximum Mass:
* The exact maximum mass a star can attain is still a subject of ongoing research.
* However, current estimates suggest that the upper limit is somewhere between 150 and 300 solar masses.
Important Note:
* These factors are interconnected, and their influence on a star's mass limit is complex and not fully understood.
* Further research is needed to refine our understanding of the processes that determine the maximum mass a star can attain.
