The formation of radiation driven winds in bursting neutron stars

Details The formation of radiation driven winds in bursting neutron stars The formation of radiation driven winds in bursting neutron stars

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..359y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 359-367. Research supported by the Minerva Foundatio

Astronomy and Astrophysics

Astrophysics

10

Neutron Stars, Stellar Mass Accretion, Stellar Winds, X Ray Sources, Bursts, Heat Transfer Coefficients, Momentum Transfer, Radiation Pressure

Scientific paper

The authors discuss the conditions for the formation of radiation driven wind around accreting neutron stars during a helium flash. Time-dependent dynamical models of the star atmosphere suggest that the total luminosity during the mass loss phase is oscillating around a mean value that is limited to a few times (2 - 3) the Eddington luminosity. The authors also consider effects of a dipole-like superstrong magnetic field (1012 - 1013G) on the formation of a radiation-driven wind. In particular, they obtain modified heat transport coefficients and show that the efficiency of momentum transfer from the radiation field to the gas depends crucially on the ratio of the cyclotron energy to the mean thermal energy.

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