Radiative heat conduction and the magnetorotational instability

Details Radiative heat conduction and the magnetorotational instability Radiative heat conduction and the magnetorotational instability

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mnras.355..345a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 355, Issue 2, pp. 345-351.

Astronomy and Astrophysics

Astronomy

1

Accretion, Accretion Discs, Instabilities, Mhd, Neutrinos, Gamma-Rays: Bursts

Scientific paper

A photon or a neutrino gas, semicontained by a non-diffusive particle species through scattering, comprises a rather peculiar magnetohydrodynamic fluid where the magnetic field is truly frozen only to the comoving volume associated with the mass density. Although radiative diffusion precludes a formal adiabatic treatment of compressive perturbations, we cast the energy equation in quasi-adiabatic form by assuming a negligible rate of energy exchange among species on the time-scale of the perturbation. This leads to a simplified dispersion relation for toroidal, non-axisymmetric magnetorotational modes when the accretion disc has comparable stress contributions from diffusive and non-diffusive components. The properties of the modes of fastest growth are shown to depend strongly on the compressibility of the mode, with a reduction in growth rate consistent with the results of Blaes & Socrates for axisymmetric modes. A clumpy disc structure is anticipated on the basis of the polarization properties of the fastest-growing modes. This analysis is accurate in the near-hole region of locally cooled, hyper-accreting flows if the electron gas becomes moderately degenerate such that non-conductive, thermalizing processes with associated electron-positron release (i.e. neutrino annihilation and neutrino absorption on to nuclei) are effectively blocked by high occupation of the Fermi levels.

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