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• W80496947 abstract "Center for Astrophysical Thermonuclear Flashes, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAAbstractPrompted by the recent detection of X-ray emissionfrom Herbig-Haro objects, we studied the interaction be-tween a supersonic jet originating from a young stellarobject and the ambient medium; our aim is to investigatethe mechanisms causing the X-ray emission. Our modeltakes into account the radiative losses from optically thinplasmas and Spitzer’s thermal conduction including satu-ration effects. We explored the parameter space defined bythe density contrast between the ambient medium and thejet and by the Mach number, to infer the configurationswhich can give rise to X-ray emission. From the models,we derived the X-ray emission as it would be observedwith Chandra/ACIS-I and XMM-Newton/EPIC-pn, usingthe MEKAL spectral code and including the absorptionof interstellar medium. Here we discuss a representativecase which produces, without any ad hoc assumption, X-ray emission with characteristics very similar to those ob-served in the protostellar jet, HH 154. We find that theX-ray emission originates from a blob localized just behindthe bow shock, moving with velocity 500 km/s. We pre-dict, therefore, among other features, a detectable propermotion of the X-ray blob, which is interesting for futureobservations.Key words: ISM: Herbig-Haro objects – ISM: individualobjects (HH 154) – ISM: jets and outflows – X-rays: ISM1. IntroductionHerbig-Haro objects are mainly shocks produced at the in-teraction front between the supersonic protostellar jet andthe ambient medium. Optical, radio and infrared studiesof these objects have been carried since HH objects werediscovered (Herbig 1950; Haro 1953). Recently X-ray emis-sion with the XMM-Newton and Chandra satellites hasbeen detected for a few of these HH objects: HH2 in Orion(Pravdo et al. 2001), HH154 in Taurus (Favata et al. 2002;Bally et al. 2003), HH80/81 in the Sagittarius cloud L291(Pravdo et al. 2004), and a protostellar jet in the OMC-3molecular cloud in Orion (Tsujimoto et al. 2004).As an example the left panel of the Fig. 1 shows anoptical image of the protostellar jet HH 154 located at thedistance of 140 pc in Taurus (adapted from Bally et al.2003). This figure shows the position of the X-ray sourcemarked with a cross at the base of the jet.The right panel of Fig. 1 is a close up view of the X-raysource detected with Chandra/ACIS-I (Bally et al. 2003).The X-ray source is not coincident with the position of theprotostar. The protostar suffers a visual extinction of ∼150 mag whereas a small visual extinction of ∼ 7maghasbeen found for the soft X-ray source, with a temperature ofa few million degrees. This makes HH 154 an ideal objectto be studied because the emission from the protostar isobscured.Prompted by these new observations we started a pro-ject devoted to study the mechanism causing the X-rayemission detected in HH objects. This work is part of awider project in which we perform a detailed explorationof the parameter space and we take into account all theimportant physical effects describing the evolution of aprotostellar jet.In this paper we study the X-ray emission from HH154, the nearest and one of the best studied Herbig-Haroobjects emitting X-rays. X-ray emission from HH 154 hasbeen detected with both XMM-Newton and Chandra (Fa-vata et al. 2002; Bally et al. 2003). The aim of our workis to infer the configuration which can give rise to X-rayemission, to derive detailed predictions, to determine therange of parameters consistent with observations and toget insight on the jet physical conditions. To this end weperformed a detailed modeling of the interaction betweena supersonic plasma jet and a uniform ambient mediumusing the FLASH code (Fryxell et al. 2000). FLASH isan accurate and very advanced numerical code which usesthe PARAMESH library to handle adaptive mesh refine-ment (MacNeice et al. 2000). The code uses the MessagePassing Interface (MPI) library to achieve parallelization.For our simulations FLASH included modules that treatoptically thin radiative losses and thermal conduction.The paper is structured as follows: Sect. 2 describesthe proto-stellar jet model; Sect. 3 describes our methodto synthesize, from the numerical simulations, X-ray ob-servations as predicted to be observed with Chandra andXMM-Newton; in Sect. 4 we discuss the results of thenumerical simulations; finally in Sect. 5 we draw our con-clusions.Proc. 13th Cool Stars Workshop, Hamburg, 5–9 July 2004 (ESA SP-560, Jan. 2005, F. Favata, G. Hussain & B. Battrick eds.)" @default.
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• W80496947 date "2005-03-01" @default.
• W80496947 modified "2023-10-16" @default.
• W80496947 title "X-RAY EMISSION MECHANISMS IN PROTOSTELLAR JETS" @default.
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