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3D YSO accretion shock simulations: a study of the magnetic, chromospheric and stochastic flow effects

Published online by Cambridge University Press:  07 August 2014

T. Matsakos ,
J.-P. Chièze ,
C. Stehlé ,
M. González ,
L. Ibgui ,
L. de Sá ,
T. Lanz ,
S. Orlando ,
R. Bonito  and
C. Argiroffi
...Show all authors
T. Matsakos
Affiliation:
CEA, IRAMIS, Service Photons, Atomes et Molécules, 91191 Gif-sur-Yvette, France email: titos.matsakos@cea.fr Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, IRFU/Service d'Astrophysique, CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France LERMA, Observatoire de Paris, Université Pierre et Marie Curie and CNRS, 5 Place J. Janssen, 92195 Meudon, France
J.-P. Chièze
Affiliation:
Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, IRFU/Service d'Astrophysique, CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France
C. Stehlé
Affiliation:
LERMA, Observatoire de Paris, Université Pierre et Marie Curie and CNRS, 5 Place J. Janssen, 92195 Meudon, France
M. González
Affiliation:
Université Paris Diderot, Sorbonne Paris Cité, AIM, UMR 7158, CEA, CNRS, 91191 Gif-sur-Yvette, France
L. Ibgui
Affiliation:
LERMA, Observatoire de Paris, Université Pierre et Marie Curie and CNRS, 5 Place J. Janssen, 92195 Meudon, France
L. de Sá
Affiliation:
Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, IRFU/Service d'Astrophysique, CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France LERMA, Observatoire de Paris, Université Pierre et Marie Curie and CNRS, 5 Place J. Janssen, 92195 Meudon, France
T. Lanz
Affiliation:
Laboratoire Lagrange, Université de Nice-Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, 06304 Nice cedex 4, France
S. Orlando
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
R. Bonito
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy Dipartimento di Fisica e Chimica, Universitá degli Studi di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
C. Argiroffi
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy Dipartimento di Fisica e Chimica, Universitá degli Studi di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
F. Reale
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy Dipartimento di Fisica e Chimica, Universitá degli Studi di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
G. Peres
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy Dipartimento di Fisica e Chimica, Universitá degli Studi di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
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Abstract

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The structure and dynamics of young stellar object (YSO) accretion shocks depend strongly on the local magnetic field strength and configuration, as well as on the radiative transfer effects responsible for the energy losses. We present the first 3D YSO shock simulations of the interior of the stream, assuming a uniform background magnetic field, a clumpy infalling gas, and an acoustic energy flux flowing at the base of the chromosphere. We study the dynamical evolution and the post-shock structure as a function of the plasma-beta (thermal pressure over magnetic pressure). We find that a strong magnetic field (~hundreds of Gauss) leads to the formation of fibrils in the shocked gas due to the plasma confinement within flux tubes. The corresponding emission is smooth and fully distinguishable from the case of a weak magnetic field (~tenths of Gauss) where the hot slab demonstrates chaotic motion and oscillates periodically.

Keywords

accretionmagnetohydrodynamics (MHD)radiative transfershock wavesinstabilities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 66 - 69
Copyright
Copyright © International Astronomical Union 2014 

References

Argiroffi, C., Maggio, A., & Peres, G. 2005, A&A, 465, L5Google Scholar
Drake, J. J., Ratzlaff, P. W., Laming, J. M., & Raymond, J., ApJ, 703, 1224Google Scholar
Günther, H. M., Lewandowska, N., Hundertmark, M. P. G., et al. 2010, A&A, 518, 54Google Scholar
Koldoba, A. V., Ustyugova, G. V., Romanova, M. M., & Lovelace, R. V. E. 2008, MNRAS, 388, 357CrossRefGoogle Scholar
Johns-Krull, C. M. 2007, ApJ, 664, 975Google Scholar
Matsakos, T., Chièze, J. P., Stehlé, C., et al. 2013, A&A, 557, 69Google Scholar
Orlando, S., Bonito, R., Argiroffi, C., et al. 2013, A&A, in pressGoogle Scholar
Mignone, A., Bodo, G., Massaglia, S., et al. 2007, ApJS, 170Google Scholar
Orlando, S., Sacco, G. G., Argiroffi, C., et al. 2010, A&A, 510, 71Google Scholar
de Sá, L. in preparationGoogle Scholar
Sacco, G. G., Argiroffi, C., Orlando, S., et al. 2008, A&A, 491, L17Google Scholar
Sacco, G. G., Orlando, S., Argiroffi, C., et al. 2010, A&A, 522, 55Google Scholar