2001/11/01 by Santabrata Das, Indranil Chattopadhyay, A. Nandi +1 · 2 citations
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Heat Transfer and Numerical Methods #Nanofluid Flow and Heat Transfer #astro-ph
paper · pdf · doi:10.1051/0004-6361:20011307
published as Astron.Astrophys. 379 (2001) 683 · 9 pages, 5 figures
openalex publication_date 2001/11/01 · arxiv created 2004/02/24 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We self-consistently estimate the outflow rate from the accretion rates of an accretion disk around a black hole in which both the Keplerian and the sub-Keplerian matter flows simultaneously. While Keplerian matter supplies soft-photons, hot sub-Keplerian matter supplies thermal electrons. The temperature of the hot electrons is decided by the degree of inverse Comptonization of the soft photons. If we consider only thermally-driven flows from the centrifugal pressure-supported boundary layer around a black hole, we find that when the thermal electrons are cooled down, either because of the absence of the boundary layer (low compression ratio), or when the surface of the boundary layer is formed very far away, the outflow rate is negligible. For an intermediate size of this boundary layer the outflow rate is maximal. Since the temperature of the thermal electrons also decides the spectral state of a black hole, we predict that the outflow rate should be directly related to the spectral state.