X-Rays from Young Stellar Objects: Magnetic Structures and Irradiation Effects

Details X-Rays from Young Stellar Objects: Magnetic Structures and Irradiation Effects X-Rays from Young Stellar Objects: Magnetic Structures and Irradiation Effects

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..273m&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

Scientific paper

X-rays, especially in the hard energy range (a few keV) covered by ASCA, which is less sensitive to extinction, offer a powerful diagnosis of the magnetic activity in Young Stellar Objects and of irradiation effects on the surrounding environment. In T Tauri stars (TTS), the X-ray activity is essentially solar, albeit enhanced by several orders of magnitude in LX/Lbol, and ubiquitously in the form of luminous flares. In analogy with solar X-ray flares, the TTS flares are coming from a hot plasma confined in large magnetic loops. In the earlier, embedded protostar phase, the X-ray activity can be even higher, and likely results from magnetic interactions between the forming star and its accretion disk. In the well-documented case of YLW15, a Class I protostar in the ρ Oph cloud core, a triple flare has been discovered by ASCA, giving the first clues on the rotation of this protostar. In addition, the strong X-ray luminosity induces various irradiation effects (ionization, chemistry, etc.) on the surrounding circumstellar and interstellar medium, which are still comparatively poorly known. In particular, specific feedback mechanisms are expected on the accretion from a circumstellar disk.

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