Journal
ASTROPHYSICAL JOURNAL
Volume 818, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/0004-637X/818/2/162
Keywords
accretion, accretion disks; black hole physics; magnetohydrodynamics (MHD); methods: numerical; radiative transfer
Categories
Funding
- JSPS KAKENHI [24740127, 15K05036]
- Center for the Promotion of Integrated Sciences (CPIS) of Sokendai
- MEXT HPCI STRATEGIC PROGRAM
- Grants-in-Aid for Scientific Research [24740127, 15K05036] Funding Source: KAKEN
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We develop a numerical scheme for solving the equations of fully special relativistic, radiation magnetohydrodynamics (MHDs), in which the frequency-integrated, time-dependent radiation transfer equation is solved to calculate the specific intensity. The radiation energy density, the radiation flux, and the radiation stress tensor are obtained by the angular quadrature of the intensity. In the present method, conservation of total mass, momentum, and energy of the radiation magnetofluids is guaranteed. We treat not only the isotropic scattering but also the Thomson scattering. The numerical method of MHDs is the same as that of our previous work. The advection terms are explicitly solved, and the source terms, which describe the gas-radiation interaction, are implicitly integrated. Our code is suitable for massive parallel computing. We present that our code shows reasonable results in some numerical tests for propagating radiation and radiation hydrodynamics. Particularly, the correct solution is given even in the optically very thin or moderately thin regimes, and the special relativistic effects are nicely reproduced.
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