EPJ Web of Conferences
Volume 64, 2014Physics at the Magnetospheric Boundary
|Number of page(s)||4|
|Section||Physics at the Magnetospheric Boundary in Young Stellar Objects|
|Published online||08 January 2014|
3D Gray Radiative Properties of Accretion Shocks in Young Stellar Objects
1 LERMA, Observatoire de Paris, CNRS et UPMC, 5 Place J. Janssen, 92195 Meudon, France
2 INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90134, Palermo, Italy
3 Laboratoire AIM, IRFU / Service d’Astrophysique - CEA/DSM - CNRS - Université Paris Diderot, Bât. 709 CEA-Saclay, F-91191
4 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
5 Laboratoire J.-L. Lagrange, Université de Nice-Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice, France
6 CEA, IRAMIS, Service Photons, Atomes et Molécules, 91191 Gif-sur-Yvette, France
7 Dip. di Fisica e Chimica, Università degli Studi di Palermo, Piazza del Parlamento, 1, 90134, Palermo, Italy
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Published online: 8 January 2014
We address the problem of the contribution of radiation to the structure and dynamics of accretion shocks on Young Stellar Objects. Solving the 3D RTE (radiative transfer equation) under our “gray LTE approach”, i.e., using appropriate mean opacities computed in local thermodynamic equilibrium, we post-process the 3D MHD (magnetohydrodynamic) structure of an accretion stream impacting the stellar chromosphere. We find a radiation flux of ten orders of magnitude larger than the accreting energy rate, which is due to a large overestimation of the radiative cooling. A gray LTE radiative transfer approximation is therefore not consistent with the given MHD structure of the shock. Further investigations are required to clarify the role of radiation, by relaxing both the gray and LTE approximations in RHD (radiation hydrodynamics) simulations. Post-processing the obtained structures through the resolution of the non-LTE monochromatic RTE will provide reference radiation quantities against which RHD approximate solutions will be compared.
© Owned by the authors, published by EDP Sciences, 2014
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 2.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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