2018/01/05 by De-Fu Bu, Xiao‐Hong Yang, Xiao-Hong Yang
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Bremsstrahlung #Eddington luminosity #Electron #Galaxies: Formation, Evolution, Phenomena #Galaxy #Ionization #Luminosity #Nuclear physics #Photoionization #Physics #Radiative cooling #Thermal wind #Wind profile power law #Wind speed #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.1093/mnras/sty053
9 pages, 6 figures, accepted by MNRAS
arxiv created 2018/01/05 · openalex publication_date 2018/01/06 · arxiv updated 2018/01/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study slowly rotating accretion flow at parsec and subparsec scales irradiated by low-luminosity active galactic nuclei. We take into account the Compton heating, photoionization heating by the central X-rays. The bremsstrahlung cooling, recombination, and line cooling are also included. We find that due to the Compton heating, wind can be thermally driven. The power of wind is in the range (10−6–10−3) LEdd, with LEdd being the Eddington luminosity. The mass flux of wind is in the range |(0.01-1) M\rm Edd| (|M\rm Edd= L\rm Edd/0.1c2| is the Eddington accretion rate, c is speed of light). We define the wind generation efficiency as |ε = P\rm W/M\rm BHc2|, with PW being wind power, |M\rm BH| being the mass accretion rate on to the black hole. ε lies in the range 10−4–1.18. Wind production efficiency decreases with increasing mass accretion rate. The possible role of the thermally driven wind in the active galactic feedback is briefly discussed.