Abstract
The status and implications of recent X-ray studies of pre-main sequence (PMS) stars are reviewed in detail. Images of nearby star formation regions including the Orion, Taurus-Auriga, ρ Ophiuchi and Chamaeleon clouds obtained with the Einstein X-ray Observatory have revealed more than 150 X-ray luminous PMS stars to date. Some are classical strong emission line T Tauri stars while others are late-type PMS stars with weak or absent lines. The soft X-ray luminosities range from ≲ 1029 erg/s to several 1031 erg/s, or ∼103 times that of local main sequence stars. The X-ray emission is highly variable; most show large amplitude variations on timescales of days, and a few exhibit flares on timescales of 102–104 seconds. The rapid variations, hard spectra, and lack of correlation with wind-produced optical emission lines all point to a flare origin of the enhanced X-ray emission. Solar-type stars thus exhibit their most violent surface activity during their PMS stage of evolution. Implications for the conditions in PMS stars, stellar activity-rotation age relation, for the chemistry and evolution of molecular clouds, and for various chemical and isotopic anomalies in the ancient solar system are discussed.
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Feigelson, E.D. (1984). X-ray emission from pre-main sequence stars. In: Baliunas, S.L., Hartmann, L. (eds) Cool Stars, Stellar Systems, and the Sun. Lecture Notes in Physics, vol 193. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-12907-3_176
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DOI: https://doi.org/10.1007/3-540-12907-3_176
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