Multi-wavelength observations of phase changes in X Persei

Details Multi-wavelength observations of phase changes in X Persei Multi-wavelength observations of phase changes in X Persei

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26as...97..277r&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 97, no. 1, p. 277-279.

Astronomy and Astrophysics

Astrophysics

2

Neutron Stars, O Stars, Pulsars, Stellar Mass Accretion, Stellar Spectrophotometry, X Ray Sources, H Alpha Line, Light Curve, Stellar Envelopes, Stellar Evolution, Stellar Winds

Scientific paper

X Persei is the optical counterpart to the pulsating X-ray source 4U0352+30. The system consists of a neutron star secondary accreting from an O9.5IIIe primary via stellar wind processes. IN mid-1990, X Per underwent a dramatic phase change, losing its circumstellar shell, infrared excess and H alpha emission line. Detailed optical and infrared measurements throughout this change are presented and compared with earlier, archival material which suggests that a similar event took place in 1974-1977. We examine the X-ray data available from this earlier phase change, and discuss the X-ray behavior of the system during and after the event. We find a clear correlation between the optical, infrared and X-ray behavior during the 1974-1977 phase change, followed by an extended period where the X-ray behavior appears to be unrelated to that in the optical or infrared. Based on this we expect X Per to have undergone a period of spin-up during 1990-1991.

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