Volume 424, Number 2, September III 2004
|Page(s)||L1 - L4|
|Published online||23 August 2004|
Letter to the Editor
The X-ray emission mechanism in the protostellar jet HH 154
Dip. Scienze Fisiche ed Astronomiche, Sez. Astronomia, Università di Palermo, P.zza del Parlamento 1, 90134 Palermo, Italy e-mail: email@example.com
2 INAF - Osservatorio Astronomico di Palermo, P.zza del Parlamento 1, 90134 Palermo, Italy
3 Astrophys. Div. – Res. and Science Support Dept. of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
4 Dept. of Astronomy and Astrophysics, Univ. of Chicago, Chicago, IL 60637, USA
5 Center for Astrophysical Thermonuclear Flashes, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA
Accepted: 24 June 2004
We study the mechanism causing the X-ray emission recently detected in protostellar jets, by performing a detailed modeling of the interaction between a supersonic jet originating from a young stellar object and the ambient medium, for various values of density contrast, ν, between the ambient density and the jet, and of Mach number, M; radiative losses and thermal conduction have been taken into account. Here we report a representative case which reproduces, without any ad hoc assumption, the characteristics of the X-ray emission recently observed in the protostellar jet HH 154. We find that the X-ray emission originates from a localized blob, consistent with observations, which moves with velocity km s-1; we therefore predict the X-ray source to have a detectable proper motion.
Key words: ISM: Herbig-Haro objects / ISM: individual objects: HH 154 / ISM: jets and outflows / X-rays: ISM
© ESO, 2004
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