Variability in OB Star X-ray Emission Lines: Analysis Techniques

Details Variability in OB Star X-ray Emission Lines: Analysis Techniques Variability in OB Star X-ray Emission Lines: Analysis Techniques

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715410n&link_type=abstract

American Astronomical Society, AAS Meeting #217, #154.10; Bulletin of the American Astronomical Society, Vol. 43, 2011

Biology

Quantitative Biology

Quantitative Methods

2

Scientific paper

X-ray emission lines in the spectra of hot stars are expected to vary over short or long periods due to a number of phenomena related to the wind, a companion, or the star itself. Such variations are difficult to quantify due to the comparatively low signal-to-noise in the existing data and the lack of extensive temporal coverage. We utilize several quantitative methods, including a Monte Carlo technique and KS tests, to evaluate emission lines in X-ray spectra for short-term variability based on time-sliced spectra. Our sample of test spectra includes several co-added spectra of multiple observations of a target, as well as four O stars that were serendipitously observed during observations of other targets. We discuss the probability of detecting short-term variations in the He-like emission lines of several hot stars in HETG Chandra data and the need for deeper exposures.

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