Accretion in a Dynamical Spacetime and the Spinning Up of the Black Hole in the Gamma-Ray Burst Central Engine
We compute the evolution of a quasi-spherical, slowly rotating accretion flow around a black hole, whose mass and spin evolve adequately to transfer of mass and energy through the horizon. Our model is relevant for a central engine driving a long gamma-ray burst (GRB) that originates from the collap...
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Veröffentlicht in: | The Astrophysical journal 2018-11, Vol.868 (1), p.68 |
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description | We compute the evolution of a quasi-spherical, slowly rotating accretion flow around a black hole, whose mass and spin evolve adequately to transfer of mass and energy through the horizon. Our model is relevant for a central engine driving a long gamma-ray burst (GRB) that originates from the collapse of a massive star. The computations of a GRB engine in a dynamically evolving spacetime metric are important specifically due to the transient nature of the event, in which a huge amount of mass is accreted and changes the fundamental black hole parameters-its mass and spin-during the process. We discuss the results in the context of the angular momentum magnitude of the collapsing star. We also study the possible formation and evolution of shocks in the envelope, which may temporarily affect accretion. Our results are important for the limitations on the mass and spin range of black holes detected independently by electromagnetic observations of GRBs and gravitational waves. We speculate on the possible constraints for the final masses and spins of these astrophysical black holes. It is shown that the most massive black holes are not formed in a powerful GRB explosion if the cores of their progenitors were only weakly rotating. |
doi_str_mv | 10.3847/1538-4357/aae83f |
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Our model is relevant for a central engine driving a long gamma-ray burst (GRB) that originates from the collapse of a massive star. The computations of a GRB engine in a dynamically evolving spacetime metric are important specifically due to the transient nature of the event, in which a huge amount of mass is accreted and changes the fundamental black hole parameters-its mass and spin-during the process. We discuss the results in the context of the angular momentum magnitude of the collapsing star. We also study the possible formation and evolution of shocks in the envelope, which may temporarily affect accretion. Our results are important for the limitations on the mass and spin range of black holes detected independently by electromagnetic observations of GRBs and gravitational waves. We speculate on the possible constraints for the final masses and spins of these astrophysical black holes. It is shown that the most massive black holes are not formed in a powerful GRB explosion if the cores of their progenitors were only weakly rotating.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aae83f</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion ; accretion, accretion disks ; Angular momentum ; Astrophysics ; black hole physics ; Black holes ; Deposition ; Evolution ; Gamma ray bursts ; Gamma rays ; gamma rays: general ; Gravitational collapse ; Gravitational waves ; Gravity waves ; hydrodynamics ; Massive stars ; Progenitors (astrophysics) ; Relativity ; Rotating spheres ; Rotation ; Spacetime ; Stellar evolution</subject><ispartof>The Astrophysical journal, 2018-11, Vol.868 (1), p.68</ispartof><rights>2018. The American Astronomical Society. 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J</addtitle><description>We compute the evolution of a quasi-spherical, slowly rotating accretion flow around a black hole, whose mass and spin evolve adequately to transfer of mass and energy through the horizon. Our model is relevant for a central engine driving a long gamma-ray burst (GRB) that originates from the collapse of a massive star. The computations of a GRB engine in a dynamically evolving spacetime metric are important specifically due to the transient nature of the event, in which a huge amount of mass is accreted and changes the fundamental black hole parameters-its mass and spin-during the process. We discuss the results in the context of the angular momentum magnitude of the collapsing star. We also study the possible formation and evolution of shocks in the envelope, which may temporarily affect accretion. Our results are important for the limitations on the mass and spin range of black holes detected independently by electromagnetic observations of GRBs and gravitational waves. We speculate on the possible constraints for the final masses and spins of these astrophysical black holes. It is shown that the most massive black holes are not formed in a powerful GRB explosion if the cores of their progenitors were only weakly rotating.</description><subject>Accretion</subject><subject>accretion, accretion disks</subject><subject>Angular momentum</subject><subject>Astrophysics</subject><subject>black hole physics</subject><subject>Black holes</subject><subject>Deposition</subject><subject>Evolution</subject><subject>Gamma ray bursts</subject><subject>Gamma rays</subject><subject>gamma rays: general</subject><subject>Gravitational collapse</subject><subject>Gravitational waves</subject><subject>Gravity waves</subject><subject>hydrodynamics</subject><subject>Massive stars</subject><subject>Progenitors (astrophysics)</subject><subject>Relativity</subject><subject>Rotating spheres</subject><subject>Rotation</subject><subject>Spacetime</subject><subject>Stellar evolution</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kDFPwzAQhS0EEqWwM1qCkVAnjhNnbEtpkSohQZHYrKtzLi6NE5x06L8nIQgWWM66z--9kx4hlyG75TJOR6HgMoi5SEcAKLk5IoMfdEwGjLE4SHj6ekrO6nrbrVGWDYgba-2xsaWj1lGgdwcHhdWwo88V6PajQAoup80btsQ6Z92GvlS0NF9osgP9ThflDjt7R-ZQFBA8wYFO9r5u6BRd49u4mdtYh-fkxMCuxovvd0hW97PVdBEsH-cP0_Ey0DzNmgAh1EbkyTrmKDLNBArQWbo2USJigIwzkBnHVGiu48QYDI0UEUvykOUScj4kV31s5cuPPdaN2pZ779qLKuKJkCmTUrQq1qu0L-vao1GVtwX4gwqZ6kpVXYOqa1D1pbaW695iy-o3E6qtkolUoWpHlXeymz9k_6Z-Arz4hSY</recordid><startdate>20181120</startdate><enddate>20181120</enddate><creator>Janiuk, Agnieszka</creator><creator>Sukova, Petra</creator><creator>Palit, Ishika</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></search><sort><creationdate>20181120</creationdate><title>Accretion in a Dynamical Spacetime and the Spinning Up of the Black Hole in the Gamma-Ray Burst Central Engine</title><author>Janiuk, Agnieszka ; Sukova, Petra ; Palit, Ishika</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c379t-ea1cf5d6b43e59c05e5ac97bf2654aa930a893e75c3c46ffe1f85206d10d8ad3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Accretion</topic><topic>accretion, accretion disks</topic><topic>Angular momentum</topic><topic>Astrophysics</topic><topic>black hole physics</topic><topic>Black holes</topic><topic>Deposition</topic><topic>Evolution</topic><topic>Gamma ray bursts</topic><topic>Gamma rays</topic><topic>gamma rays: general</topic><topic>Gravitational collapse</topic><topic>Gravitational waves</topic><topic>Gravity waves</topic><topic>hydrodynamics</topic><topic>Massive stars</topic><topic>Progenitors (astrophysics)</topic><topic>Relativity</topic><topic>Rotating spheres</topic><topic>Rotation</topic><topic>Spacetime</topic><topic>Stellar evolution</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Janiuk, Agnieszka</creatorcontrib><creatorcontrib>Sukova, Petra</creatorcontrib><creatorcontrib>Palit, Ishika</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_linktorsrc</fulltext></delivery><addata><au>Janiuk, Agnieszka</au><au>Sukova, Petra</au><au>Palit, Ishika</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Accretion in a Dynamical Spacetime and the Spinning Up of the Black Hole in the Gamma-Ray Burst Central Engine</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-11-20</date><risdate>2018</risdate><volume>868</volume><issue>1</issue><spage>68</spage><pages>68-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We compute the evolution of a quasi-spherical, slowly rotating accretion flow around a black hole, whose mass and spin evolve adequately to transfer of mass and energy through the horizon. Our model is relevant for a central engine driving a long gamma-ray burst (GRB) that originates from the collapse of a massive star. The computations of a GRB engine in a dynamically evolving spacetime metric are important specifically due to the transient nature of the event, in which a huge amount of mass is accreted and changes the fundamental black hole parameters-its mass and spin-during the process. We discuss the results in the context of the angular momentum magnitude of the collapsing star. We also study the possible formation and evolution of shocks in the envelope, which may temporarily affect accretion. Our results are important for the limitations on the mass and spin range of black holes detected independently by electromagnetic observations of GRBs and gravitational waves. We speculate on the possible constraints for the final masses and spins of these astrophysical black holes. It is shown that the most massive black holes are not formed in a powerful GRB explosion if the cores of their progenitors were only weakly rotating.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aae83f</doi><tpages>15</tpages><oa>free_for_read</oa></addata></record> |
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subjects | Accretion accretion, accretion disks Angular momentum Astrophysics black hole physics Black holes Deposition Evolution Gamma ray bursts Gamma rays gamma rays: general Gravitational collapse Gravitational waves Gravity waves hydrodynamics Massive stars Progenitors (astrophysics) Relativity Rotating spheres Rotation Spacetime Stellar evolution |
title | Accretion in a Dynamical Spacetime and the Spinning Up of the Black Hole in the Gamma-Ray Burst Central Engine |
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