Discussion Overview
The discussion revolves around the question of how massive a body can become before it collapses into a black hole. Participants explore various aspects of this topic, including the limits for stars, the role of density, and the implications of different physical principles.
Discussion Character
- Exploratory
- Debate/contested
- Technical explanation
Main Points Raised
- One participant asks about the mass limit for a body to collapse into a black hole, distinguishing it from the weight required to become a black hole.
- Another participant emphasizes that density is crucial, noting that galaxy clusters can be very massive without collapsing.
- A participant mentions a limit of about 150 solar masses for stars due to radiation pressure, contingent on starting from typical interstellar material.
- Clarification is provided that the discussion is specifically about stars, not galaxy clusters.
- One participant points out that fusion cannot be simply turned off and that various factors must be considered when discussing real objects.
- The Chandrasekhar limit is referenced as a boundary for white dwarf formation, with uncertainty about the upper limit for neutron stars due to the unknown equation of state of neutronium.
- Concerns about spelling and clarity in communication arise, with some participants advocating for better citation habits and clearer writing.
Areas of Agreement / Disagreement
Participants express differing views on the limits of mass for stars and the conditions under which collapse occurs. There is no consensus on the exact mass limit or the implications of density and composition.
Contextual Notes
The discussion includes assumptions about the starting conditions for stars and the complexities involved in stellar evolution, which are not fully resolved.