Accretion to Magnetized Stars through the Rayleigh-Taylor Instability: Global Three-Dimensional Simulations
We present results of 3D simulations of MHD instabilities at the accretion disk-magnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues o...
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| description | We present results of 3D simulations of MHD instabilities at the accretion disk-magnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time on the inner-disk dynamical timescale. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator. The instability appears for relatively small misalignment angles, \(\Theta\lesssim30^\circ\), between the star's rotation and magnetic axes, and is associated with higher accretion rates. The hot spots and light curves during accretion through instability are generally much more chaotic than during stable accretion. The unstable state of accretion has possible implications for quasi-periodic oscillations and intermittent pulsations from accreting systems, as well as planet migration. |
| doi_str_mv | 10.48550/arxiv.0802.1759 |
| format | Article |
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The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time on the inner-disk dynamical timescale. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator. The instability appears for relatively small misalignment angles, \(\Theta\lesssim30^\circ\), between the star's rotation and magnetic axes, and is associated with higher accretion rates. The hot spots and light curves during accretion through instability are generally much more chaotic than during stable accretion. The unstable state of accretion has possible implications for quasi-periodic oscillations and intermittent pulsations from accreting systems, as well as planet migration.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.0802.1759</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Accretion disks ; Light curve ; Magnetospheres ; Migration ; Misalignment ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planetary evolution ; Polar environments ; Quasi-Periodic Oscillations ; Stellar magnetic fields ; Stellar rotation ; Taylor instability</subject><ispartof>arXiv.org, 2008-03</ispartof><rights>2008. 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The unstable state of accretion has possible implications for quasi-periodic oscillations and intermittent pulsations from accreting systems, as well as planet migration.</description><subject>Accretion disks</subject><subject>Light curve</subject><subject>Magnetospheres</subject><subject>Migration</subject><subject>Misalignment</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planetary evolution</subject><subject>Polar environments</subject><subject>Quasi-Periodic Oscillations</subject><subject>Stellar magnetic fields</subject><subject>Stellar rotation</subject><subject>Taylor instability</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2008</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkFFLwzAUhYMgOObefZKAz503SdM0vo2pczARXN_LbZutmV07k1acv97M-XTuvRzOuXyE3DCYxqmUcI_u235NIQU-ZUrqCzLiQrAojTm_IhPvdwDAE8WlFCPyMStLZ3rbtbTv6Ctu27D8mIque3Se9rXrhm0d1NB3PDbGbusoC0Pn6LL1PRa2sf3xgS6arsCGZrUzJnq0e9P6kBkua7sfGjwV-GtyucHGm8m_jkn2_JTNX6LV22I5n60ilIxFQsUMWcKFMgLLSmsoE5UUSijJINVapxBjJUAVnINJYMOLSiGgLqXcaG3EmNyeY_9A5Adn9-iO-QlIfgISDHdnw8F1n4Pxfb7rBhee9TkHDXHoTpj4BXB7Y7M</recordid><startdate>20080308</startdate><enddate>20080308</enddate><creator>Kulkarni, Akshay K</creator><creator>Romanova, Marina M</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20080308</creationdate><title>Accretion to Magnetized Stars through the Rayleigh-Taylor Instability: Global Three-Dimensional Simulations</title><author>Kulkarni, Akshay K ; 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The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time on the inner-disk dynamical timescale. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator. The instability appears for relatively small misalignment angles, \(\Theta\lesssim30^\circ\), between the star's rotation and magnetic axes, and is associated with higher accretion rates. The hot spots and light curves during accretion through instability are generally much more chaotic than during stable accretion. The unstable state of accretion has possible implications for quasi-periodic oscillations and intermittent pulsations from accreting systems, as well as planet migration.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.0802.1759</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Accretion disks Light curve Magnetospheres Migration Misalignment Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics Planetary evolution Polar environments Quasi-Periodic Oscillations Stellar magnetic fields Stellar rotation Taylor instability |
| title | Accretion to Magnetized Stars through the Rayleigh-Taylor Instability: Global Three-Dimensional Simulations |
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