Self-consistent models of spherical accretion onto black holes. I - One-temperature solutions. II - Two-temperatures solutions with pairs

Details Self-consistent models of spherical accretion onto black holes. I - One-temperature solutions. II - Two-temperatures solutions with pairs Self-consistent models of spherical accretion onto black holes. I - One-temperature solutions. II - Two-temperatures solutions with pairs

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...354...64p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 354, May 1, 1990, p. 64-97.

Statistics

Computation

27

Accretion Disks, Astronomical Models, Black Holes (Astronomy), Computational Astrophysics, Quasars, Temperature Effects, Active Galactic Nuclei, Coulomb Collisions, Emission Spectra, Iterative Solution, Luminosity, Pair Production, Radiative Transfer, Stellar Mass Accretion, Black Holes, Hydrodynamics, Radiation Mechanisms, Quasars

Scientific paper

Spherically symmetric, steady state accretion onto a black hole is considered for various dimensionless accretion rates mṡ (≡ Mṡc2/LE, where Mṡ is the accretion rate and LE is the Eddington luminosity). Models are constructed by iteratively integrating relativistic hydrodynamic and radiation moment equations with bremsstrahlung and Comptonization as the main radiative processes. Electrons and ions are assumed to be coupled completely. The effects of preheating, and the shock that may result, are also considered.
At least one type of self-consistent model is found for any mṡ, self-consistency meaning that the gas at all radii is heated by the radiation it produces. Two sets of models (characterized by different temperatures) were found in the range 3 ≲ mṡ ≲ 100. The dimensionless luminosity l (≡L/LE) is 5.8 × 10-5mṡ2 for mṡ ≪ 1. Low-temperature models (T ≃ 104 K), which exist for mṡ 0.1, have l ˜ 7 × 10-10mṡln(108/mṡ); high-temperature models, which exist for 3 ≲ mṡ ≲ 100, have 3 × 10-4 ≲ l ≲ 3 × 10-2. The mṡ = 100 model has the highest luminosity of all: l = 2.6 × 10-2. High-mṡ models have correct mean photon energies for AGNs.
Because of the effects of preheating, no steady state high-temperature self-consistent solution exists for 0.1 ≲ mṡ ≲ 3 without a shock, and none exists for mṡ ≳ 100 regardless of the presence or absence of a shock. The calculations also suggest that the high-temperature mṡ > 1 model is unstable at a fixed accretion rate.

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