Generation of radiative knots in a randomly pulsed protostellar jet

II. X-ray emission

¹ Dip. Scienze Fisiche ed Astronomiche, Sez. Astronomia, Università di Palermo, P.zza del Parlamento 1, 90134 Palermo, Italy e-mail: sbonito@astropa.unipa.it
² INAF – Osservatorio Astronomico di Palermo, P.zza del Parlamento 1, 90134 Palermo, Italy
³ Thüringer Landessternwarte, Sternwarte 5, 07778 Tautenburg, Germany
⁴ European Space Agency Community Coordination and Planning Office, 8–10 rue Mario Nikis, 75738 Paris Cedex 15, France

Received: 2 April 2010
Accepted: 11 May 2010

Abstract

Context. Protostellar jets are known to emit in a wide range of bands, from radio to IR to optical bands, and to date about ten jets that also emit X-rays have been detected, with a rate of discovery of about one per year.

Aims. We aim at investigating the mechanism leading to the X-ray emission detected in protostellar jets and in particular at constraining the physical parameters that describe the jet/ambient interaction by comparing our model predictions with observations available from the literature.

Methods. We perform 2D axisymmetric hydrodynamic simulations of the interaction between a supersonic jet and the ambient medium. The jet is described as a train of plasma blobs randomly ejected by the stellar source along the jet axis. We explore the parameter space by varying the ejection rate, the initial Mach number of the jet, and the initial density contrast between the ambient medium and the jet. We synthesize the X-ray emission from the model as it would be observed with the current X-ray telescopes.

Results. The mutual interactions among the ejected blobs themselves and of the blobs with the ambient medium lead to complex X-ray-emitting structures within the jet. The X-ray sources consist of several components: irregular chains of knots, isolated knots with measurable proper motion, apparently stationary knots, and reverse shocks. The predicted X-ray luminosity strongly depends on the ejection rate and on the initial density contrast between the ambient medium and the jet, with a lesser dependence on the jet Mach number.

Conclusions. Our model represents the first attempt to describe the X-ray properties of all X-ray-emitting protostellar jets discovered so far. The comparison between our model predictions and the observations can provide a useful diagnostic tool, which is necessary for a proper interpretation of the observations. We specifically suggest that the observable quantities derived from the spectral analysis of X-ray observations can be used to constrain the ejection rate, a parameter explored in our model that is not measurable by current observations in all wavelength bands.