Timeline for Why does the Chandrasekhar limit affect white dwarfs differently?
Current License: CC BY-SA 3.0
7 events
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| Jul 26, 2023 at 20:26 | comment | added | blademan9999 | Another explanation physics.stackexchange.com/a/666799/263465 | |
| Apr 13, 2017 at 12:59 | history | edited | CommunityBot |
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| May 2, 2016 at 13:17 | comment | added | ProfRob | If a WD is rotating at an appreciable fraction of its Keplerian breakup speed, then the Chandrasekhar mass can be increased by a few percent, and have lower densities at the same mass. arxiv.org/abs/1204.2070 | |
| May 2, 2016 at 12:49 | comment | added | Sir Cumference | @RobJeffries So what happens if it's rotating? Why would it be different? | |
| May 2, 2016 at 12:48 | comment | added | ProfRob | The "vanilla" Chandrasekhar mass is not 1.44 solar masses for any kind of white dwarf. It is set by GR at between 1,38 and 1,39 solar masses for (non-rotating) C/O and O/Ne/Mg white dwarfs, if you define it as the maximum possible mass supportable and ignore the possibility of electron capture (which can lead to instability at marginally lower masses in the case of O/Ne/Mg WDs). | |
| May 2, 2016 at 11:41 | comment | added | Sir Cumference | The link I added also mentions neutronization in binaries. Why does that happen? | |
| May 2, 2016 at 8:58 | history | answered | James K | CC BY-SA 3.0 |