Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2009-09-16
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
8 pages, 1 figure, 1 table, submitted to MNRAS
Scientific paper
In low-collisionality plasmas, anisotropic heat conduction due to a magnetic field leads to buoyancy instabilities for any nonzero temperature gradient. We study analogous instabilities in degenerate {\it collisional} plasmas, i.e., when the electron collision frequency is large compared to the electron cyclotron frequency. Although heat conduction is nearly isotropic in this limit, the small residual anisotropy ensures that collisional degenerate plasmas are also convectively unstable independent of the sign of the temperature gradient. We show that the range of wavelengths that are unstable is independent of the magnetic field strength, while the growth time increases with decreasing magnetic field strength. We discuss the application of these collisional buoyancy instabilities to white dwarfs and neutron stars. Magnetic tension and the low specific heat of a degenerate plasma significantly limit their effectiveness; the most promising venues for growth are in the liquid oceans of young, weakly magnetized neutron stars ($B \lesssim 10^9$ G) and in the cores of young, high magnetic field white dwarfs ($B \sim 10^9$ G).
Chang Paoti
Quataert Eliot
No associations
LandOfFree
Buoyancy Instabilities in Degenerate, Collisional, Magnetized Plasmas does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Buoyancy Instabilities in Degenerate, Collisional, Magnetized Plasmas, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Buoyancy Instabilities in Degenerate, Collisional, Magnetized Plasmas will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-583388