2008/09/10 by Ya-Di Xu, Yadi Xu, Xinwu Cao
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #Heat Transfer Mechanisms #astro-ph
paper · pdf · doi:10.1088/1674-4527/9/4/003
10 pages, 2 figures, accepted by ChJAA
arxiv created 2008/09/10 · openalex publication_date 2009/04/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
It was found that advection-dominated accretion flow (ADAF)+thin disk model calculations can reproduce the observed spectral energy distributions (SEDs) of two low-luminosity active galactic nuclei (AGNs), provided they are accreting at ∼ 0.01 – 0.03 Eddington rates and the thin disks are truncated to ADAFs at ∼ 100 R S ( R S is the Schwarzschild radius) for M81 and NGC 4579 (Quataert et al. 1999). However, the black hole masses adopted in their work are about one order of magnitude lower than recent measurements on these two sources. Adopting the well estimated black hole masses, our ADAF+thin disk model calculations can reproduce the observed SEDs of these two low-luminosity AGNs, if the black hole is accreting at 2.5 ' 10 −4 Eddington rates with the thin disk truncated at R tr = 120 R S for M81 ( = 3.3 ' 10 −3 and R tr = 80 R S are required for NGC 4579). The transition zones with temperature from the thin disk with ∼ 10 4 – 10 5 to ∼ 10 9 – 10 10 K in the ADAF will inevitably emit thermal X-ray lines, which provides a useful diagnosis of their physical properties. The observed widths of the thermal X-ray iron lines at ≃ 6.8 keV are consistent with Doppler broadening by Keplerian motion of the gases in the transition zones at ∼ 100 R S . We use the structure of the transition zone between the ADAF and the thin disk derived by assuming the turbulent diffusive heat mechanism to calculate their thermal X-ray line emission with the standard software package Astrophysical Plasma Emission Code (APEC). Comparing them with the equivalent widths of the observed thermal X-ray iron lines in these two sources, we find that the turbulent diffusive heat mechanism seems to be unable to reproduce the observed thermal X-ray line emission. The test of the evaporation model for the accretion mode transition with the observed thermal X-ray line emission is briefly discussed.