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from III - Convection, Rotation and Activity
Published online by Cambridge University Press: 04 August 2010
The new generation of X-ray missions to be launched by the end of this century will provide excellent opportunities for the study of very-low mass stars and brown dwarfs as well as of cool stars in open clusters and star forming regions. AXAF and XMM will be highly complementary in this respect, with AXAF leading the field for the detection of very faint objects and the study of crowded regions, and XMM allowing medium to high resolution spectroscopy to fainter limits for a large number of stars in open clusters and nearby star forming regions. With the help of simulations of AXAF and XMM spectra, and estimates of the sensitivity limits for typical imaging and spectroscopic observations, I discuss the prospects offered by these two missions for the study of low-mass stars and cluster stars.
Introduction
The next few years will be a marvellous time for X-ray astronomy, with the launch of AXAF (Advanced X-ray Astrophysics Facility) in spring 1999 and of XMM (X-ray Multi Mirror Mission) and ASTRO-E (the new Japanese X-ray mission) in early 2000. These new powerful missions will produce a great leap forward in all fields of X-ray astronomy, from nearby stars to the most distant objects in the Universe. They will be far more sensitive than past and ongoing X-ray missions and will be equipped with new detectors (CCD and microchannel plate cameras, transmission and reflection gratings, and X-ray microcalorimeters) that will allow detection of fainter objects as well as detailed medium to high-resolution spectroscopy of the brightest sources.
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