Coordinated Chandra/HST Studies of Stellar Wind X-ray Binaries

Details Coordinated Chandra/HST Studies of Stellar Wind X-ray Binaries Coordinated Chandra/HST Studies of Stellar Wind X-ray Binaries

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002xrb..confe..48v&link_type=abstract

X-ray Binaries in the Chandra and XMM-Newton Era (with an emphasis on Targets of Opportunity), Abstracts of the conference held

Physics

Optical Monitoring, The Optical/X-Ray Connection

Scientific paper

Chandra (ACIS-S) and HST Observations of SMC X-1 and LMC X-4 during both high and low states will be discussed. The X-ray spectra are dominated by continuum emission in the X-ray high state. A new analysis, incorporating corrections for pile up of the high state data, will be presented. During eclipse and during the X-ray low state the continuum emission largely disappears and we see line emission from O, Ne, Mg, and Fe and possibly from Si and S. The emission lines are consistent with recombination lines from mostly hydrogenic and helium-like species which could be produced by photoionization in an extended stellar wind. The ultraviolet P-Cygni lines show strong broad absorption near X-ray eclipse and only narrow interstellar absorption when the X-ray source is in the line-of-sight. We interpret this as a result of X-ray photoionization of the stellar wind which renders the wind transparent in the vicinity of the X-ray source. The UV continuum fluxes remain roughly constant in spite of more than an order of magnitude change in X-ray flux between high and low-states, as would be expected if the X-ray flux reduction is due to occultation of the X-ray source (e.g., by a precessing disk) rather than to an intrinsic change in X-ray luminosity.

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