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[Ne II] and X-ray emission from ρ Ophiuchi young stellar objects

Published online by Cambridge University Press:  21 October 2010

E. Flaccomio ,
B. Stelzer ,
S. Sciortino ,
I. Pillitteri  and
G. Micela
E. Flaccomio
Affiliation:
INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento, 1, 90134, Italy
B. Stelzer
Affiliation:
INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento, 1, 90134, Italy
S. Sciortino
Affiliation:
INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento, 1, 90134, Italy
I. Pillitteri
Affiliation:
INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento, 1, 90134, Italy
G. Micela
Affiliation:
INAF - Osservatorio Astronomico di Palermo Piazza del Parlamento, 1, 90134, Italy
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Circumstellar disks are mostly made of gas. Constraining the spatial and thermal structure of the gas, and its time evolution, is crucial to understand the star- and planet-formation processes. Models predict that the gas is affected by UV and X-ray radiation from the central young stellar object (YSO), but many uncertainties remain, e.g. whether the EUV emission actually reaches the disk or is absorbed by disk winds. The infrared [Ne II] and [Ne III] fine structure lines at 12.81μm and 15.55μm have been theoretically predicted to trace the circumstellar disk gas subject to X-ray heating and ionization.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 745
Copyright
Copyright © International Astronomical Union 2010