Discussion Overview
The discussion centers on the differences between neutron stars and black holes, focusing on their formation, characteristics, and the role of progenitor star mass. The scope includes theoretical aspects of stellar evolution and the physical processes involved in the collapse of massive stars.
Discussion Character
- Exploratory
- Technical explanation
- Debate/contested
Main Points Raised
- Some participants explain that the final state of a star depends on its mass, with smaller stars becoming white dwarfs, intermediate mass stars forming neutron stars, and the most massive stars collapsing into black holes.
- One participant notes that neutron stars are formed when gravity is strong enough to convert electrons and protons into neutrons, but not strong enough to create a black hole.
- A participant provides a specific density measurement for neutron stars, indicating their extreme density compared to ordinary matter.
- Another participant discusses the mass thresholds for stellar remnants, suggesting that progenitor stars up to approximately 10.5 solar masses typically become white dwarfs, while those between 10.5 and 20 solar masses usually result in neutron stars, with black holes forming from more massive stars.
- A later reply corrects earlier mass thresholds, stating that smaller stars are those less than about 8 solar masses, with neutron stars forming from stars between 8 and 20 solar masses, and black holes from those exceeding 20 solar masses.
- This participant cites Kip Thorne's work to support their claims about the mass limits and the uncertainties involved in stellar evolution processes.
Areas of Agreement / Disagreement
Participants express differing views on the mass thresholds for the formation of neutron stars and black holes, indicating that there is no consensus on the exact limits and the processes involved in stellar evolution.
Contextual Notes
There are unresolved uncertainties regarding the mass limits for stellar remnants, the effects of relativistic and centrifugal forces, and the implications of observational data on stellar evolution.