rHARM : accretion and ejection in resistive GR-MHD

Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numeri...
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Gespeichert in:

Autor*in:	Qian, Qian [verfasserIn] Fendt, Christian - 1962- [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2017

Anmerkung:	Published 2016 December 28 Gesehen am 22.01.2019
Umfang:	20

Übergeordnetes Werk:	Enthalten in: The astrophysical journal - London : Institute of Physics Publ., 1995, 834(2017), 1, Artikel-ID 29
Übergeordnetes Werk:	volume:834 ; year:2017 ; number:1 ; elocationid:29 ; extent:20

Links:	Volltext Volltext

DOI / URN:	10.3847/1538-4357/834/1/29

Katalog-ID:	1582238502

Internformat


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912			\|a GBV_ILN_63
912			\|a GBV_ILN_65
912			\|a GBV_ILN_69
912			\|a GBV_ILN_70
912			\|a GBV_ILN_73
912			\|a GBV_ILN_95
912			\|a GBV_ILN_105
912			\|a GBV_ILN_110
912			\|a GBV_ILN_151
912			\|a GBV_ILN_161
912			\|a GBV_ILN_170
912			\|a GBV_ILN_230
912			\|a GBV_ILN_285
912			\|a GBV_ILN_293
912			\|a GBV_ILN_370
912			\|a GBV_ILN_602
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912			\|a GBV_ILN_2088
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Indexfelder

author_variant	q q qq c f cf
matchkey_str	article:15384357:20172016::h
oclc_num	1341021748
hierarchy_sort_str	2017
publishDate	2017
allfields	10.3847/1538-4357/834/1/29 doi (DE-627)1582238502 (DE-576)512238502 (DE-599)BSZ512238502 (OCoLC)1341021748 DE-627 ger DE-627 rda eng Qian, Qian verfasserin (DE-588)1135751803 (DE-627)890793727 (DE-576)490100023 aut rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli 2017 20 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Published 2016 December 28 Gesehen am 22.01.2019 Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. 2016 Fendt, Christian 1962- verfasserin (DE-588)124964915 (DE-627)369234243 (DE-576)29459261X aut Enthalten in The astrophysical journal London : Institute of Physics Publ., 1995 834(2017), 1, Artikel-ID 29 Online-Ressource (DE-627)269019219 (DE-600)1473835-1 (DE-576)077662733 1538-4357 nnns volume:834 year:2017 number:1 elocationid:29 extent:20 http://dx.doi.org/10.3847/1538-4357/834/1/29 Verlag Resolving-System Volltext http://stacks.iop.org/0004-637X/834/i=1/a=29 Verlag Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 834 2017 1 29 20 2013 01 DE-16-250 3029606708 00 --%%-- --%%-- --%%-- --%%-- l01 24-10-18 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_4 2013 01 DE-16-250 03 s s_20 2013 01 DE-16-250 04 p (DE-627)1560108894 Qian, Qian 2013 01 DE-16-250 04 k (DE-627)1471138844 Dekanat der Fakultät für Physik und Astronomie 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_1 2013 01 DE-16-250 05 p (DE-627)1582238316 Fendt, Christian 2013 01 DE-16-250 05 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_2
spelling	10.3847/1538-4357/834/1/29 doi (DE-627)1582238502 (DE-576)512238502 (DE-599)BSZ512238502 (OCoLC)1341021748 DE-627 ger DE-627 rda eng Qian, Qian verfasserin (DE-588)1135751803 (DE-627)890793727 (DE-576)490100023 aut rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli 2017 20 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Published 2016 December 28 Gesehen am 22.01.2019 Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. 2016 Fendt, Christian 1962- verfasserin (DE-588)124964915 (DE-627)369234243 (DE-576)29459261X aut Enthalten in The astrophysical journal London : Institute of Physics Publ., 1995 834(2017), 1, Artikel-ID 29 Online-Ressource (DE-627)269019219 (DE-600)1473835-1 (DE-576)077662733 1538-4357 nnns volume:834 year:2017 number:1 elocationid:29 extent:20 http://dx.doi.org/10.3847/1538-4357/834/1/29 Verlag Resolving-System Volltext http://stacks.iop.org/0004-637X/834/i=1/a=29 Verlag Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 834 2017 1 29 20 2013 01 DE-16-250 3029606708 00 --%%-- --%%-- --%%-- --%%-- l01 24-10-18 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_4 2013 01 DE-16-250 03 s s_20 2013 01 DE-16-250 04 p (DE-627)1560108894 Qian, Qian 2013 01 DE-16-250 04 k (DE-627)1471138844 Dekanat der Fakultät für Physik und Astronomie 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_1 2013 01 DE-16-250 05 p (DE-627)1582238316 Fendt, Christian 2013 01 DE-16-250 05 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_2
allfields_unstemmed	10.3847/1538-4357/834/1/29 doi (DE-627)1582238502 (DE-576)512238502 (DE-599)BSZ512238502 (OCoLC)1341021748 DE-627 ger DE-627 rda eng Qian, Qian verfasserin (DE-588)1135751803 (DE-627)890793727 (DE-576)490100023 aut rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli 2017 20 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Published 2016 December 28 Gesehen am 22.01.2019 Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. 2016 Fendt, Christian 1962- verfasserin (DE-588)124964915 (DE-627)369234243 (DE-576)29459261X aut Enthalten in The astrophysical journal London : Institute of Physics Publ., 1995 834(2017), 1, Artikel-ID 29 Online-Ressource (DE-627)269019219 (DE-600)1473835-1 (DE-576)077662733 1538-4357 nnns volume:834 year:2017 number:1 elocationid:29 extent:20 http://dx.doi.org/10.3847/1538-4357/834/1/29 Verlag Resolving-System Volltext http://stacks.iop.org/0004-637X/834/i=1/a=29 Verlag Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 834 2017 1 29 20 2013 01 DE-16-250 3029606708 00 --%%-- --%%-- --%%-- --%%-- l01 24-10-18 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_4 2013 01 DE-16-250 03 s s_20 2013 01 DE-16-250 04 p (DE-627)1560108894 Qian, Qian 2013 01 DE-16-250 04 k (DE-627)1471138844 Dekanat der Fakultät für Physik und Astronomie 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_1 2013 01 DE-16-250 05 p (DE-627)1582238316 Fendt, Christian 2013 01 DE-16-250 05 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_2
allfieldsGer	10.3847/1538-4357/834/1/29 doi (DE-627)1582238502 (DE-576)512238502 (DE-599)BSZ512238502 (OCoLC)1341021748 DE-627 ger DE-627 rda eng Qian, Qian verfasserin (DE-588)1135751803 (DE-627)890793727 (DE-576)490100023 aut rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli 2017 20 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Published 2016 December 28 Gesehen am 22.01.2019 Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. 2016 Fendt, Christian 1962- verfasserin (DE-588)124964915 (DE-627)369234243 (DE-576)29459261X aut Enthalten in The astrophysical journal London : Institute of Physics Publ., 1995 834(2017), 1, Artikel-ID 29 Online-Ressource (DE-627)269019219 (DE-600)1473835-1 (DE-576)077662733 1538-4357 nnns volume:834 year:2017 number:1 elocationid:29 extent:20 http://dx.doi.org/10.3847/1538-4357/834/1/29 Verlag Resolving-System Volltext http://stacks.iop.org/0004-637X/834/i=1/a=29 Verlag Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 834 2017 1 29 20 2013 01 DE-16-250 3029606708 00 --%%-- --%%-- --%%-- --%%-- l01 24-10-18 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_4 2013 01 DE-16-250 03 s s_20 2013 01 DE-16-250 04 p (DE-627)1560108894 Qian, Qian 2013 01 DE-16-250 04 k (DE-627)1471138844 Dekanat der Fakultät für Physik und Astronomie 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_1 2013 01 DE-16-250 05 p (DE-627)1582238316 Fendt, Christian 2013 01 DE-16-250 05 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_2
allfieldsSound	10.3847/1538-4357/834/1/29 doi (DE-627)1582238502 (DE-576)512238502 (DE-599)BSZ512238502 (OCoLC)1341021748 DE-627 ger DE-627 rda eng Qian, Qian verfasserin (DE-588)1135751803 (DE-627)890793727 (DE-576)490100023 aut rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli 2017 20 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Published 2016 December 28 Gesehen am 22.01.2019 Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. 2016 Fendt, Christian 1962- verfasserin (DE-588)124964915 (DE-627)369234243 (DE-576)29459261X aut Enthalten in The astrophysical journal London : Institute of Physics Publ., 1995 834(2017), 1, Artikel-ID 29 Online-Ressource (DE-627)269019219 (DE-600)1473835-1 (DE-576)077662733 1538-4357 nnns volume:834 year:2017 number:1 elocationid:29 extent:20 http://dx.doi.org/10.3847/1538-4357/834/1/29 Verlag Resolving-System Volltext http://stacks.iop.org/0004-637X/834/i=1/a=29 Verlag Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 834 2017 1 29 20 2013 01 DE-16-250 3029606708 00 --%%-- --%%-- --%%-- --%%-- l01 24-10-18 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_4 2013 01 DE-16-250 03 s s_20 2013 01 DE-16-250 04 p (DE-627)1560108894 Qian, Qian 2013 01 DE-16-250 04 k (DE-627)1471138844 Dekanat der Fakultät für Physik und Astronomie 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_1 2013 01 DE-16-250 05 p (DE-627)1582238316 Fendt, Christian 2013 01 DE-16-250 05 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_2
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source	Enthalten in The astrophysical journal 834(2017), 1, Artikel-ID 29 volume:834 year:2017 number:1 elocationid:29 extent:20
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authorswithroles_txt_mv	Qian, Qian @@aut@@ Fendt, Christian @@aut@@
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title	rHARM accretion and ejection in resistive GR-MHD
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title_full	rHARM accretion and ejection in resistive GR-MHD Qian Qian(钱前), Christian Fendt, Scott Noble, and Matteo Bugli
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title_auth	rHARM accretion and ejection in resistive GR-MHD
abstract	Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. Published 2016 December 28 Gesehen am 22.01.2019
abstractGer	Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. Published 2016 December 28 Gesehen am 22.01.2019
abstract_unstemmed	Turbulent magnetic diffusivity plays an important role for accretion disks and the launching of disk winds. We have implemented magnetic diffusivity and respective resistivity in the general relativistic MHD code HARM. This paper describes the theoretical background of our implementation, its numerical realization, our numerical tests, and preliminary applications. The test simulations of the new code rHARM are compared to an analytic solution of the diffusion equation and a classical shock tube problem. We have further investigated the evolution of the magnetorotational instability (MRI) in tori around black holes (BHs) for a range of magnetic diffusivities. We find an indication for a critical magnetic diffusivity (for our setup) beyond which no MRI develops in the linear regime and for which accretion of torus material to the BH is delayed. Preliminary simulations of magnetically diffusive thin accretion disks around Schwarzschild BHs that are threaded by a large-scale poloidal magnetic field show the launching of disk winds with mass fluxes of about 50% of the accretion rate. The disk magnetic diffusivity allows for efficient disk accretion that replenishes the mass reservoir of the inner disk area and thus allows for long-term simulations of wind launching for more than 5000 time units. Published 2016 December 28 Gesehen am 22.01.2019
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rHARM : accretion and ejection in resistive GR-MHD

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