Accretion onto magnetized neutron stars - X-ray pulsars with intermediate rotation rates

Details Accretion onto magnetized neutron stars - X-ray pulsars with intermediate rotation rates Accretion onto magnetized neutron stars - X-ray pulsars with intermediate rotation rates

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..175b&link_type=abstract

Astrophysical Journal, Part 1, vol. 266, Mar. 1, 1983, p. 175-187. Research supported by the John Simon Guggenheim Foundatio

Astronomy and Astrophysics

Astrophysics

37

Magnetic Stars, Neutron Stars, Pulsars, Stellar Mass Accretion, Stellar Rotation, X Ray Sources, Angular Momentum, Binary Stars, Kelvin-Helmholtz Instability, Magnetohydrodynamic Flow, Magnetopause

Scientific paper

Assuming that the accreting material originates in a wind or envelope and therefore carried no net angular momentum, the Kevin-Helmholtz instability is applied to the transport of accreting plasma across the magnetopause of a rotating and magnetized neutron star for the case in which this surface is interchange-stable. Magnetopause location is determined, and the blackbody emission temperature is estimated. A possible period-dependence is noted in the X-ray temperature data which is in approximate agreement with the present model calculations. The magnetopause is found to be insufficiently stable to support an optically thick sheath of plasma surrounding the source, so that neither shrouding of the X-ray source nor significant reprocessing of the radiation field is possible in the model presented. It is concluded that while the flow structure at the magnetopause can control accretion column geometry, the emerging pulse profile and spectra are only indirectly altered, through a dynamical influence on emission region geometry.

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