On the disk wind mass loss rates in QSOs |
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| Institution: | 1. Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, Tandoğan, TR-06100, Ankara, Turkey;2. Astronomical Observatory, Jagiellonian University, ul. Orla 171, Krakow PL-30-244, Poland;3. Mt Suhora Observatory, Pedagogical University, ul. Podchorazych 2, Krakow PL-30-084, Poland;4. Institute for Astronomy and Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, Penteli, Athens, Greece;5. 1393 Garvin Street, Prince George, BC V2M 3Z1, Canada;6. Department of Astrophysics, Astronomy and Mechanics, National & Kapodistrian University of Athens, Zografos GR-15784, Athens, Greece;1. Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, China;3. University of the Chinese Academy of Sciences, Beijing 100049, China;1. Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, PR China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China;3. Graduate University of Chinese Academy of sciences, Beijing, PR China;1. Department of Bioengineering, The University of Texas at Dallas, Richardson, TX;2. Department of Surgery and Biomechanics, School of Podiatric Medicine, The University of Texas Rio Grande Valley, Harlingen, TX |
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| Abstract: | We derive here a relatively simple expression for the total wind mass loss rates in QSOs within the accretion disk wind scenario. We show that the simple expression derived here for QSO disk wind mass loss rate is in a very good agreement with the more “exact” values obtained through significantly more complex and detailed numerically intensive 2.5D time-dependent simulations. Additionally we show that for typical QSO parameters, the disk itself will be emitting mostly in the UV/optical spectrum, in turn implying that the X-ray emission from QSOs likely is produced through some physical mechanism acting at radii smaller than the inner disk radius (for a standard accretion disk, half of the initially gravitational potential energy of the accreting disk mass is emitted directly by the disk, while the other half “falls” closer towards the black hole than the inner disk radius). We also show that for typical QSO parameters, the disk itself is dominated by continuum radiation pressure (rather than thermal pressure), resulting in a “flat disk” (except for the innermost disk regions). |
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