Densities of Stellar Flares from Spectral Lines

Details Densities of Stellar Flares from Spectral Lines Densities of Stellar Flares from Spectral Lines

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006hrxs.confe..22m&link_type=abstract

High Resolution X-ray Spectroscopy: towards XEUS and Con-X, Proceedings of the international workshop held at the Mullard Space

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Scientific paper

We present detailed analyses of spectral changes during X-ray flares. During flares the plasma is known to become hotter, but also changes in density are anticipated, as flares will rather be compact and dense than large and tenuous. We search for indications of changes in density in the spectra of Chandra High Energy Transmission Grating Spectrometer (HETGS) data. However, as flares usually last for at most up to one hour, only very bright flares will produce enough photons for a sufficiently well exposed spectrum. We chose long Chandra observations of flare stars which covered periods of time with flare activity that can be combined to compile one quiescent-only spectrum to be compared with a spectrum that is affected by flare activity. We show that with careful data analysis it is possible with the presently available instruments to detect spectral line changes between quiescent and flaring states, notably in the density- and temperature-sensitive lines of the He-like OVII triplet (21.6/21.8/22.1 A). Using cumulative distribution functions, we are also able to give solid statistical confidence limits. We also briefly discuss the diagnostic capabilities of other He-like line triplets and of observations carried out with the XMM-Newton Reflection Grating Spectrometer (RGS).

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