TY - GEN
T1 - 3D gray radiative properties of accretion shocks in young stellar objects
AU - Ibgui, L.
AU - Orlando, S.
AU - Stehlé, C.
AU - Chièze, J. P.
AU - Hubeny, I.
AU - Lanz, T.
AU - De Sá, L.
AU - Matsakos, T.
AU - González, M.
AU - Bonito, R.
PY - 2014
Y1 - 2014
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=84893554593&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84893554593&partnerID=8YFLogxK
U2 - 10.1051/epjconf/20136404005
DO - 10.1051/epjconf/20136404005
M3 - Conference contribution
AN - SCOPUS:84893554593
SN - 9782759811434
T3 - EPJ Web of Conferences
BT - Physics at the Magnetospheric Boundary
T2 - Physics at the Magnetospheric Boundary Conference
Y2 - 25 June 2013 through 28 June 2013
ER -