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Active Galactic Nuclei Feedback at the Parsec Scale
We perform simulations to study the effects of active galactic nuclei (AGNs) radiation and wind feedback on the properties of slowly rotating accretion flow at the parsec scale. We find that when only radiative feedback is considered, outflows can be produced by the radiation pressure due to Thomson...
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Published in: | The Astrophysical journal 2019-09, Vol.882 (1), p.55 |
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description | We perform simulations to study the effects of active galactic nuclei (AGNs) radiation and wind feedback on the properties of slowly rotating accretion flow at the parsec scale. We find that when only radiative feedback is considered, outflows can be produced by the radiation pressure due to Thomson scattering. The mass flux of outflow is comparable to that of inflow. Although strong outflow is present, the luminosity of the AGN can be easily super-Eddington. When wind feedback is also taken into account, the mass flux of outflow does not change much. Consequently, the luminosity of the central AGN can still be super-Eddington. However, observations show that the luminosity of most AGNs is sub-Eddington. Some other mechanisms are needed to reduce the AGNs' luminosity. Although the mass outflow rate is not changed much by wind feedback, other properties of outflow (the density, temperature, velocity, and kinetic power) can be significantly changed by wind feedback. In the presence of wind feedback, the density of outflow becomes significantly lower, the temperature of outflow becomes significantly higher, the velocity of outflow is increased by one order of magnitude, and the kinetic power of outflow is increased by a factor of 40-100. |
doi_str_mv | 10.3847/1538-4357/ab31a1 |
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We find that when only radiative feedback is considered, outflows can be produced by the radiation pressure due to Thomson scattering. The mass flux of outflow is comparable to that of inflow. Although strong outflow is present, the luminosity of the AGN can be easily super-Eddington. When wind feedback is also taken into account, the mass flux of outflow does not change much. Consequently, the luminosity of the central AGN can still be super-Eddington. However, observations show that the luminosity of most AGNs is sub-Eddington. Some other mechanisms are needed to reduce the AGNs' luminosity. Although the mass outflow rate is not changed much by wind feedback, other properties of outflow (the density, temperature, velocity, and kinetic power) can be significantly changed by wind feedback. In the presence of wind feedback, the density of outflow becomes significantly lower, the temperature of outflow becomes significantly higher, the velocity of outflow is increased by one order of magnitude, and the kinetic power of outflow is increased by a factor of 40-100.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab31a1</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion ; accretion, accretion disks ; Active galactic nuclei ; Astrophysics ; black hole physics ; Density ; Deposition ; Feedback ; galaxies: active ; galaxies: nuclei ; Luminosity ; Mass flux ; Outflow ; Radiation ; Radiation pressure ; Stellar winds ; Temperature ; Thomson scattering ; Velocity ; Wind</subject><ispartof>The Astrophysical journal, 2019-09, Vol.882 (1), p.55</ispartof><rights>2019. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Sep 01, 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c379t-1f13e637b45856b4c6b6f22a999987e1859ad8fe1ae7b9899f8fc77da5cdd63b3</citedby><cites>FETCH-LOGICAL-c379t-1f13e637b45856b4c6b6f22a999987e1859ad8fe1ae7b9899f8fc77da5cdd63b3</cites><orcidid>0000-0002-2419-9590 ; 0000-0002-0427-520X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,786,790,27957,27958</link.rule.ids></links><search><creatorcontrib>Bu, De-Fu</creatorcontrib><creatorcontrib>Yang, Xiao-Hong</creatorcontrib><title>Active Galactic Nuclei Feedback at the Parsec Scale</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We perform simulations to study the effects of active galactic nuclei (AGNs) radiation and wind feedback on the properties of slowly rotating accretion flow at the parsec scale. We find that when only radiative feedback is considered, outflows can be produced by the radiation pressure due to Thomson scattering. The mass flux of outflow is comparable to that of inflow. Although strong outflow is present, the luminosity of the AGN can be easily super-Eddington. When wind feedback is also taken into account, the mass flux of outflow does not change much. Consequently, the luminosity of the central AGN can still be super-Eddington. However, observations show that the luminosity of most AGNs is sub-Eddington. Some other mechanisms are needed to reduce the AGNs' luminosity. Although the mass outflow rate is not changed much by wind feedback, other properties of outflow (the density, temperature, velocity, and kinetic power) can be significantly changed by wind feedback. In the presence of wind feedback, the density of outflow becomes significantly lower, the temperature of outflow becomes significantly higher, the velocity of outflow is increased by one order of magnitude, and the kinetic power of outflow is increased by a factor of 40-100.</description><subject>Accretion</subject><subject>accretion, accretion disks</subject><subject>Active galactic nuclei</subject><subject>Astrophysics</subject><subject>black hole physics</subject><subject>Density</subject><subject>Deposition</subject><subject>Feedback</subject><subject>galaxies: active</subject><subject>galaxies: nuclei</subject><subject>Luminosity</subject><subject>Mass flux</subject><subject>Outflow</subject><subject>Radiation</subject><subject>Radiation pressure</subject><subject>Stellar winds</subject><subject>Temperature</subject><subject>Thomson scattering</subject><subject>Velocity</subject><subject>Wind</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp9kEtLxDAUhYMoOI7uXQZ0aZ2kaV7LYXBGYVBBBXfhJk2wY7U16Qz4722p6Ea8m_vg3HPgQ-iUkkumCjmjnKmsYFzOwDIKdA9Nfk77aEIIKTLB5PMhOkppM6y51hPE5q6rdh6voIZ-cvh262pf4aX3pQX3iqHD3YvH9xCTd_jBQe2P0UGAOvmT7z5FT8urx8V1tr5b3Szm68wxqbuMBsp8H2kLrriwhRNWhDwH3ZeSniquoVTBU_DSaqV1UMFJWQJ3ZSmYZVN0Nvq2sfnY-tSZTbON732kyZngSueC5L2KjCoXm5SiD6aN1RvET0OJGdCYgYMZOJgRTf9yMb5UTfvr-Y_8_A85tBujVG6o4dy0ZWBf3_pvhA</recordid><startdate>20190901</startdate><enddate>20190901</enddate><creator>Bu, De-Fu</creator><creator>Yang, Xiao-Hong</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-2419-9590</orcidid><orcidid>https://orcid.org/0000-0002-0427-520X</orcidid></search><sort><creationdate>20190901</creationdate><title>Active Galactic Nuclei Feedback at the Parsec Scale</title><author>Bu, De-Fu ; Yang, Xiao-Hong</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c379t-1f13e637b45856b4c6b6f22a999987e1859ad8fe1ae7b9899f8fc77da5cdd63b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Accretion</topic><topic>accretion, accretion disks</topic><topic>Active galactic nuclei</topic><topic>Astrophysics</topic><topic>black hole physics</topic><topic>Density</topic><topic>Deposition</topic><topic>Feedback</topic><topic>galaxies: active</topic><topic>galaxies: nuclei</topic><topic>Luminosity</topic><topic>Mass flux</topic><topic>Outflow</topic><topic>Radiation</topic><topic>Radiation pressure</topic><topic>Stellar winds</topic><topic>Temperature</topic><topic>Thomson scattering</topic><topic>Velocity</topic><topic>Wind</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bu, De-Fu</creatorcontrib><creatorcontrib>Yang, Xiao-Hong</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bu, De-Fu</au><au>Yang, Xiao-Hong</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Active Galactic Nuclei Feedback at the Parsec Scale</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2019-09-01</date><risdate>2019</risdate><volume>882</volume><issue>1</issue><spage>55</spage><pages>55-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><notes>AAS18021</notes><notes>High-Energy Phenomena and Fundamental Physics</notes><abstract>We perform simulations to study the effects of active galactic nuclei (AGNs) radiation and wind feedback on the properties of slowly rotating accretion flow at the parsec scale. We find that when only radiative feedback is considered, outflows can be produced by the radiation pressure due to Thomson scattering. The mass flux of outflow is comparable to that of inflow. Although strong outflow is present, the luminosity of the AGN can be easily super-Eddington. When wind feedback is also taken into account, the mass flux of outflow does not change much. Consequently, the luminosity of the central AGN can still be super-Eddington. However, observations show that the luminosity of most AGNs is sub-Eddington. Some other mechanisms are needed to reduce the AGNs' luminosity. Although the mass outflow rate is not changed much by wind feedback, other properties of outflow (the density, temperature, velocity, and kinetic power) can be significantly changed by wind feedback. In the presence of wind feedback, the density of outflow becomes significantly lower, the temperature of outflow becomes significantly higher, the velocity of outflow is increased by one order of magnitude, and the kinetic power of outflow is increased by a factor of 40-100.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ab31a1</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0002-2419-9590</orcidid><orcidid>https://orcid.org/0000-0002-0427-520X</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Accretion accretion, accretion disks Active galactic nuclei Astrophysics black hole physics Density Deposition Feedback galaxies: active galaxies: nuclei Luminosity Mass flux Outflow Radiation Radiation pressure Stellar winds Temperature Thomson scattering Velocity Wind |
title | Active Galactic Nuclei Feedback at the Parsec Scale |
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