What mass range generally describes the remaining core that forms a Neutron Star after a supernova?
Answer
Between approximately 1.4 and 3 solar masses
If the remaining core mass falls between approximately 1.4 solar masses (the Chandrasekhar Limit) and roughly 3 solar masses (the TOV Limit), it compresses into a Neutron Star.
Frequently Asked Questions
What single characteristic primarily determines the entire destiny of a star?Approximately what core temperature is required for a protostar to ignite sustained nuclear fusion and enter the Main Sequence?How does the Main Sequence lifespan of a very massive star (20+ times the Sun's mass) compare to that of the Sun?What two opposing pressures maintain hydrostatic equilibrium during a star's Main Sequence phase?What type of stellar body forms if a collapsing core never reaches the temperature threshold required for true stellar ignition?What event triggers the expansion of a Sun-like star into a Red Giant?What is the fate of the outer layers of a star similar to the Sun after core helium fusion ceases?Which element's fusion ultimately causes the core collapse in a high-mass star because it consumes energy instead of releasing it?What mass range generally describes the remaining core that forms a Neutron Star after a supernova?How does the color of a Main Sequence star relate to its initial mass?