THERMAL EQUILIBRIA OF MAGNETICALLY SUPPORTED BLACK HOLE ACCRETION DISKS

Journal Article · Wed May 20 00:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/697/1/16; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21300595

Oda, H ^[1]; Machida, M ^[2]; Nakamura, K E ^[3]

---

1. Graduate School of Science and Technology, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522 (Japan)
2. Division of Theoretical Astronomy, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
3. Department of Sciences, Matsue National College of Technology, 14-4 Nishiikuma-cho, Matsue, Shimane 690-8515 (Japan)

We present new thermal equilibrium solutions for optically thin and optically thick disks incorporating magnetic fields. The purpose of this paper is to explain the bright hard state and the bright/slow transition observed in the rising phases of outbursts in black hole candidates. On the basis of the results of three-dimensional magnetohydrodynamic simulations, we assume that magnetic fields inside the disk are turbulent and dominated by the azimuthal component and that the azimuthally averaged Maxwell stress is proportional to the total (gas, radiation, and magnetic) pressure. We prescribe the magnetic flux advection rate to determine the azimuthal magnetic flux at a given radius. Local thermal equilibrium solutions are obtained by equating the heating, radiative cooling, and heat advection terms. We find magnetically supported ({beta} = (p {sub gas} + p {sub rad})/p {sub mag} < 1), thermally stable solutions for both optically thin disks and optically thick disks, in which the heating enhanced by the strong magnetic field balances the radiative cooling. The temperature in a low-{beta} disk (T {approx} 10{sup 7}-10{sup 11}K) is lower than that in an advection-dominated accretion flow (or radiatively inefficient accretion flow) but higher than that in a standard disk. We also study the radial dependence of the thermal equilibrium solutions. The optically thin, low-{beta} branch extends to M-dot{approx}>0.1 M-dot{sub Edd}, where M-dot is the mass accretion rate and M-dot{sub Edd} is the Eddington mass accretion rate, in which the temperature anticorrelates with the mass accretion rate. Thus, optically thin low-{beta} disks can explain the bright hard state. Optically thick, low-{beta} disks have the radial dependence of the effective temperature T {sub eff} {proportional_to} piv{sup -3/4}. Such disks will be observed as staying in a high/soft state. Furthermore, limit cycle oscillations between an optically thick low-{beta} disk and a slim disk will occur because the optically thick low-{beta} branch intersects with the radiation pressure dominated standard disk branch. These limit cycle oscillations will show a smaller luminosity variation than that between a standard disk and a slim disk.

• OSTI ID: 21300595
• Journal Information: Astrophysical Journal, Vol. 697, Issue 1; Other Information: DOI: 10.1088/0004-637X/697/1/16; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE
ACCRETION DISKS
ADVECTION
BLACK HOLES
HEATING
LIMIT CYCLE
LUMINOSITY
MAGNETIC FIELDS
MAGNETIC FLUX
MASS
MATHEMATICAL SOLUTIONS
OSCILLATIONS
RADIATION PRESSURE
RADIATIVE COOLING
SIMULATION
THERMAL EQUILIBRIUM
THREE-DIMENSIONAL CALCULATIONS
X RADIATION