High Resolution UV/X-ray Spectroscopy of SMC X-1

Details High Resolution UV/X-ray Spectroscopy of SMC X-1 High Resolution UV/X-ray Spectroscopy of SMC X-1

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8566v&link_type=abstract

HST Proposal ID #8566

Computer Science

Hst Proposal Id #8566 Hot Stars

Scientific paper

We propose simultaneous observations of the X-ray pulsar SMC X-1 and its B0 companion SK160 with HST/STIS, Chandra, and ground-based optical telescopes. We will search for correlation between orbital phase and ``bleaching'' of important P Cygni lines by X-ray photoionization {Hatchett- McCray effect}. We will model the simultaneous X-ray, ultraviolet, and optical continuum emission at different phases of the superorbital period to measure changes in mass accretion rate, disk structure, and disk size. Using the Time- Tag mode, we will search in the ultraviolet for aperiodic variability near 0.1-0.2 Hz throughout the lines and continuum and for the 0.7 second X-ray pulsar period. Using the Chandra ACIS-S in CC mode we will conduct pulse-phased spectroscopy of the X-ray emission. Our multiwavelength observations will enable us to analyze the density structure and composition of the wind; set limits on the size, shape, rotation, and precession of the disk; and determine the effects of X-ray illumination on the disk, the star, and the stellar wind.

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