rachel 💫
@skiesablaze.bsky.social
she/her. //
PhD student in astrophysics. Amateur gamer. Professional complainer. Mediocre aerial hoopist.
PhD student in astrophysics. Amateur gamer. Professional complainer. Mediocre aerial hoopist.
Without doing a detailed look at the compressibility, most of the properties point to a very fast cooling timescale due to low gas support since it only appears in our hydro cases. I'd be interested in whether radiation would "fix" it, I would think it should based on your results with starforge
January 4, 2024 at 4:50 PM
Without doing a detailed look at the compressibility, most of the properties point to a very fast cooling timescale due to low gas support since it only appears in our hydro cases. I'd be interested in whether radiation would "fix" it, I would think it should based on your results with starforge
Final point I'll put here is that magnetic fields significantly contribute to the pressure, and therefore temperature, of the CNM environment. We find that the lower compressibility of the gas in MHD models prevents overcooling in lower density gas, maintaining ideal averrage temperatures of ~100 K.
January 4, 2024 at 4:22 PM
Final point I'll put here is that magnetic fields significantly contribute to the pressure, and therefore temperature, of the CNM environment. We find that the lower compressibility of the gas in MHD models prevents overcooling in lower density gas, maintaining ideal averrage temperatures of ~100 K.
Additionally, magnetic field orientations are found to be primarily perpendicular to the orientation of a filament denser than ~100 cm^-3, while their densest centers show evidence of a return to parallel alignment. This increases filamentary flow and accretion rates onto filaments, increasing mass.
January 4, 2024 at 4:19 PM
Additionally, magnetic field orientations are found to be primarily perpendicular to the orientation of a filament denser than ~100 cm^-3, while their densest centers show evidence of a return to parallel alignment. This increases filamentary flow and accretion rates onto filaments, increasing mass.
We find velocity dispersions of 8 km/s to be ideal for the formation of structure even in high gas column density environment, expanding the flat relation between the two found by Kim&Ostriker2015. These dispersions necessarily come from the balance of gravitational energy turbulent kinetic energy.
January 4, 2024 at 4:16 PM
We find velocity dispersions of 8 km/s to be ideal for the formation of structure even in high gas column density environment, expanding the flat relation between the two found by Kim&Ostriker2015. These dispersions necessarily come from the balance of gravitational energy turbulent kinetic energy.
Wow omg Anna worm food frogs4girls just like totally gets it, a revolutionary author of our time. Can't believe crusty joker rolling would steal from such a generous mind
November 24, 2023 at 2:13 PM
Wow omg Anna worm food frogs4girls just like totally gets it, a revolutionary author of our time. Can't believe crusty joker rolling would steal from such a generous mind