Spectral and Temporal Characteristics of X-Ray--bright Stars in the Pleiades

Details Spectral and Temporal Characteristics of X-Ray--bright Stars in the Pleiades Spectral and Temporal Characteristics of X-Ray--bright Stars in the Pleiades

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...450..217g&link_type=abstract

Astrophysical Journal v.450, p.217

Astronomy and Astrophysics

Astronomy

71

Galaxy: Open Clusters And Associations: Individual Name: Pleiades, Stars: Coronae, Stars: Late-Type, Stars: Rotation, X-Rays: Stars

Scientific paper

We follow up our deep ROSAT imaging survey of the Pleiades (Stauffer et al. 1994) with an analysis of the spectral and temporal characteristics of the X-ray-bright stars in the Pleiades. Raymond & Smith (1977) one-and two-temperature models have been used to fit the position-sensitive proportional counter (PS PC) pulse-height spectra of the dozen or so brightest sources associated with late-type Pleiades members. The best-fit temperatures suggest hot coronal temperatures for K, M, and rapidly rotating G stars, and cooler temperatures for F and slowly rotating G stars. In order to probe the many less X-ray-luminous stars, we have generated composite spectra by combining net counts from all Pleiades members according to spectral type and rotational velocity. Model fits to the composite spectra confirm the trend seen in the individual spectral fits. Particularly interesting is the apparent dependence of coronal temperature on LX/Lbol. A hardness-ratio analysis also confirms some of these trends. The PSPC data have also revealed a dozen or so strong X-ray flares with peak X-ray luminosities in excess of ˜1030 ergs s-1. We have modeled the brightest of these flares with a simple quasi-static cooling loop model. The peak temperature and emission measure and the inferred electron density and plasma volume suggest a very large scale flaring event. The PSPC data were collected over a period of ˜18 months, allowing us to search for source variability on timescales ranging from less than a day (in the case of flares) to more than a year between individual exposures. On approximately year-long timescales, roughly 25% of the late-type stars are variable. Since the Pleiades was also intensively monitored by the imaging instruments on the Einstein Observatory, we have examined X-ray luminosity variations on the 10 yr timescale between Einstein and ROSAT and find that up to 40% of the late-type stars are X-ray variable. Since there is only marginal evidence for increased variability on decade-long timescales, the variability observed on long and short timescales may have a common physical origin.

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