Open AccessBlack hole accretion discs and jets at super‐Eddington luminosity
Author(s) -
Okuda T.,
Teresi V.,
Toscano E.,
Molteni D.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.08647.x
Subject(s) - physics , astrophysics , outflow , accretion (finance) , eddington luminosity , inflow , luminosity , jet (fluid) , black hole (networking) , anisotropy , mechanics , optics , galaxy , computer network , routing protocol , routing (electronic design automation) , meteorology , computer science , link state routing protocol
Super‐Eddington accretion discs with and around black holes with mass 10 M ⊙ are examined by two‐dimensional radiation hydrodynamical calculations extending from the inner disc edge to 5 × 10 4 r g and lasting up to ∼10 6 r g / c . The dominant radiation pressure force in the inner region of the disc accelerates the gas vertically to the disc plane, and jets with 0.2–0.4 c are formed along the rotational axis. In the case of the lower accretion rate, the initially anisotropic high‐velocity jet expands outward and becomes gradually isotropic flow in the distant region. The mass‐outflow rate from the outer boundary is as large as ∼10 19 –10 23 g s −1 , but it is variable and intermittent with time; that is, the outflow switches occasionally to inflow in the distant region. The luminosity also varies as ∼10 40 –10 42 erg s −1 on a long time‐scale. On the other hand, the jet in the case of the higher accretion rate maintains its initial anisotropic shape even after it goes far away. The mass‐outflow rate and the luminosity attain steady values of 3 × 10 19 g s −1 and 1.3 × 10 40 erg s −1 , respectively. In accordance with the local analysis of the slim accretion disc model, the disc is thermally unstable in the case of but stable in the case of . The super‐Eddington model with promises to explain the small collimation degree of the jet and the large mass‐outflow rate observed in the X‐ray source SS 433.