Time-dependent two dimensional radiation hydrodynamics of accreting matter onto highly magnetized neutron stars

Details Time-dependent two dimensional radiation hydrodynamics of accreting matter onto highly magnetized neutron stars Time-dependent two dimensional radiation hydrodynamics of accreting matter onto highly magnetized neutron stars

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296...89k&link_type=abstract

In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 1: X Ray Binaries p 89-98 (SEE N90-25711 19-89)

Astronomy and Astrophysics

Astronomy

13

Magnetohydrodynamics, Neutron Stars, Stellar Luminosity, Stellar Mass Accretion, Stellar Spectra, Hydrodynamic Equations, Plasma Dynamics, Stellar Structure, Time Dependence, Two Dimensional Models

Scientific paper

The self-consistent solution of the two dimensional, time dependent equations of radiation hydrodynamics governing the accretion of matter onto the highly magnetized polar caps of luminous X-ray pulsars is presented. The calculations show a structure in the accretion column very different from previous one zone uniform models. The relevant magnetic field corrections to both the hydrodynamics and the radiative transport are included. A new theory for the diffusion and advection of both radiation energy density and photon number density is presented. For initially uniformly accreting models with super-Eddington flows, evidence of strong radiation-driven outflowing optically thin radiation filled regions of the accretion column embedded in optically-thick inflowing plasma is found. The development of these photon bubbles have growth times on the order of a millisecond and show fluctuations on sub-millisecond timescales. The photon bubbles are likely to be a consequence of convective overstability and may result in observable fluctuations in the emitted luminosity leading to luminosity dependent changes in the pulse profile.

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