Periodic optical line intensity variations in X Persei

Details Periodic optical line intensity variations in X Persei Periodic optical line intensity variations in X Persei

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...155..423a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 155, no. 2, Feb. 1986, p. 423, 424.

Astronomy and Astrophysics

Astrophysics

2

B Stars, Line Spectra, Neutron Stars, Radiant Flux Density, Visible Spectrum, X Ray Binaries, Absorption Spectra, Helium Ions, Spectral Energy Distribution, Stellar Envelopes, Stellar Models

Scientific paper

A model in which a neutron star orbits around the Be star, immersed in a ring of material, is used to calculate the optical line intensities emitted by the ionized region produced by the absorption of X-rays from the neutron star. About 2×1031erg s-1 of Hα emission is found to be produced by this process and varies with the X-ray period as is observed. Most of the He II λ4686 line is produced by the ionized region and varies with the X-ray period, but constitutes about 10-4 of the continuum in this region.

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