2016A&A...596A..99U


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST20:49:03

2016A&A...596A..99U - Astronomy and Astrophysics, volume 596A, 99-99 (2016/12-1)

Formation of X-ray emitting stationary shocks in magnetized protostellar jets.

USTAMUJIC S., ORLANDO S., BONITO R., MICELI M., GOMEZ DE CASTRO A.I. and LOPEZ-SANTIAGO J.

Abstract (from CDS):

Context. X-ray observations of protostellar jets show evidence of strong shocks heating the plasma up to temperatures of a few million degrees. In some cases, the shocked features appear to be stationary. They are interpreted as shock diamonds.
Aims. We investigate the physics that guides the formation of X-ray emitting stationary shocks in protostellar jets; the role of the magnetic field in determining the location, stability, and detectability in X-rays of these shocks; and the physical properties of the shocked plasma.
Methods. We performed a set of 2.5-dimensional magnetohydrodynamic numerical simulations that modelled supersonic jets ramming into a magnetized medium and explored different configurations of the magnetic field. The model takes into account the most relevant physical effects, namely thermal conduction and radiative losses. We compared the model results with observations, via the emission measure and the X-ray luminosity synthesized from the simulations.
Results. Our model explains the formation of X-ray emitting stationary shocks in a natural way. The magnetic field collimates the plasma at the base of the jet and forms a magnetic nozzle there. After an initial transient, the nozzle leads to the formation of a shock diamond at its exit which is stationary over the time covered by the simulations (∼40-60yr; comparable with timescales of the observations). The shock generates a point-like X-ray source located close to the base of the jet with luminosity comparable with that inferred from X-ray observations of protostellar jets. For the range of parameters explored, the evolution of the post-shock plasma is dominated by the radiative cooling, whereas the thermal conduction slightly affects the structure of the shock.

Abstract Copyright: © ESO, 2016

Journal keyword(s): ISM: jets and outflows - magnetohydrodynamics (MHD) - ISM: magnetic fields - stars: protostars - ISM: structure - X-rays: ISM

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 649 1
2 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
3 RAFGL 5123 FU* 04 31 34.07736 +18 08 04.9020           K3V/M3III 811 0
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3479 0
5 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 708 0
6 HH 2 HH 05 36.4 -06 47           ~ 335 1
7 HH 248 HH 05 41 26.5 -02 23 03           ~ 7 0
8 HH 80 HH 18 19 06.1 -20 51 49           ~ 95 0
9 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 697 2
10 HH 168 HH 22 56 18.0 +62 01 47           ~ 89 0

    Equat.    Gal    SGal    Ecl

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2020.07.11-20:49:03

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