8th HEAD Meeting, 8-11 September, 2004
Session 5 Stars and the Sun
Poster, Wednesday, September 8, 2004, 9:00am-10:00pm

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[5.08] First Results from a Chandra Observation of Spica

N.A. Miller (University of Wisconsin-Eau Claire), J.P. Cassinelli (University of Wisconsin-Madison), J.J. MacFarlane (Prism Computational Sciences), R.J. Reynolds (University of Wisconsin-Madison)

We present the first results of an 89.0 kilosecond observation of Spica (B1III-IV+B2V) using Chandra in the LETG-ACIS-S configuration. The first and negative first order grating spectra recorded a total of roughly 3100 counts. A number of strong emission lines are detected, ranging from Ne X at 12.13 Angstroms up to at least Si XII at roughly 44 Angstroms. The forbidden, intercombination, and resonance lines of O VII and Ne IX are particularly interesting because they are sensitive to the amount of far ultraviolet photospheric flux in the region of X-ray emission. The X-ray emission lines appear rather narrow, and research is continuing into whether or not all of the observed line width is attributable to the line response function of the LETG. This is an interesting issue for this early B star, because while O stars such as Zeta Pup and Zeta Ori have shown Doppler-broadened X-ray emission lines, the emission lines of B stars such as Tau Sco have been surprisingly narrow. An X-ray light curve of Spica is presented to test for any effects which Spica’s 0.17 day pulsational period might have on its X-ray emission properties. This work is supported by NASA’s Chandra Guest Observer program and the UW-Eau Claire Office of Research and Sponsored Programs.

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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.