Warm Disk Coronae in Classical T Tauri Stars

Details Warm Disk Coronae in Classical T Tauri Stars Warm Disk Coronae in Classical T Tauri Stars

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489..284k&link_type=abstract

Astrophysical Journal v.489, p.284

Astronomy and Astrophysics

Astronomy

25

Accretion, Accretion Disks, Stars: Coronae, Stars: Pre-Main-Sequence

Scientific paper

It is proposed that a warm disk corona is a characteristic feature of the accretion process in a classical T Tauri star, based on analyses of the [O I] lambda lambda 6300, 5577 emission and the central absorptions in the Balmer lines of hydrogen. Calculations are presented to determine the physical conditions needed to produce the hydrogen and O I excitation. They indicate that a substantial fraction of the energy released in the accretion of matter through the disk may be dissipated at the disk surface in order to heat the corona.

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