Global Energetics of Solar Flares. X. Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows
We investigate physical scaling laws for magnetic energy dissipation in solar flares, in the framework of the Sweet-Parker model and the Petschek model. We find that the total dissipated magnetic energy Ediss in a flare depends on the mean magnetic field component Bf associated with the free energy...
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| Veröffentlicht in: | The Astrophysical journal 2020-06, Vol.895 (2), p.134 |
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| description | We investigate physical scaling laws for magnetic energy dissipation in solar flares, in the framework of the Sweet-Parker model and the Petschek model. We find that the total dissipated magnetic energy Ediss in a flare depends on the mean magnetic field component Bf associated with the free energy Ef, the length scale L of the magnetic area, the hydrostatic density scale height λ of the solar corona, the Alfvén Mach number MA = v1/vA (the ratio of the inflow speed v1 to the Alfvénic outflow speed vA), and the flare duration τf, i.e., , where the Alfvén speed depends on the nonpotential field strength Bnp and the mean electron density ne in the reconnection outflow. Using MDI/Solar Dynamics Observatory (SDO) and AIA/SDO observations and 3D magnetic field solutions obtained with the vertical-current approximation non-linear force-free field code we measure all physical parameters necessary to test scaling laws, which represents a new method to measure Alfvén Mach numbers MA, the reconnection rate, and the total free energy dissipated in solar flares. |
| doi_str_mv | 10.3847/1538-4357/ab8aec |
| format | Article |
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Using MDI/Solar Dynamics Observatory (SDO) and AIA/SDO observations and 3D magnetic field solutions obtained with the vertical-current approximation non-linear force-free field code we measure all physical parameters necessary to test scaling laws, which represents a new method to measure Alfvén Mach numbers MA, the reconnection rate, and the total free energy dissipated in solar flares.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab8aec</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Corona ; Electron density ; Energy dissipation ; Field strength ; Free energy ; Mach number ; Magnetic fields ; Magnetic reconnection ; Outflow ; Physical properties ; Scale height ; Scaling laws ; Solar activity ; Solar corona ; Solar coronal heating ; Solar coronal loops ; Solar energy ; Solar flares ; Solar magnetic fields ; Solar magnetic reconnection ; Solar observatories</subject><ispartof>The Astrophysical journal, 2020-06, Vol.895 (2), p.134</ispartof><rights>2020. 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X. Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We investigate physical scaling laws for magnetic energy dissipation in solar flares, in the framework of the Sweet-Parker model and the Petschek model. We find that the total dissipated magnetic energy Ediss in a flare depends on the mean magnetic field component Bf associated with the free energy Ef, the length scale L of the magnetic area, the hydrostatic density scale height λ of the solar corona, the Alfvén Mach number MA = v1/vA (the ratio of the inflow speed v1 to the Alfvénic outflow speed vA), and the flare duration τf, i.e., , where the Alfvén speed depends on the nonpotential field strength Bnp and the mean electron density ne in the reconnection outflow. Using MDI/Solar Dynamics Observatory (SDO) and AIA/SDO observations and 3D magnetic field solutions obtained with the vertical-current approximation non-linear force-free field code we measure all physical parameters necessary to test scaling laws, which represents a new method to measure Alfvén Mach numbers MA, the reconnection rate, and the total free energy dissipated in solar flares.</description><subject>Astrophysics</subject><subject>Corona</subject><subject>Electron density</subject><subject>Energy dissipation</subject><subject>Field strength</subject><subject>Free energy</subject><subject>Mach number</subject><subject>Magnetic fields</subject><subject>Magnetic reconnection</subject><subject>Outflow</subject><subject>Physical properties</subject><subject>Scale height</subject><subject>Scaling laws</subject><subject>Solar activity</subject><subject>Solar corona</subject><subject>Solar coronal heating</subject><subject>Solar coronal loops</subject><subject>Solar energy</subject><subject>Solar flares</subject><subject>Solar magnetic fields</subject><subject>Solar magnetic reconnection</subject><subject>Solar observatories</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNp1kNtKw0AQhhdRsB7uvVwQ70zddDeb5LKUtgpqxQP0bplsZ3swzcbdRNE38jl8MRMqiqA3M8zw_98MPyFHIevyRMRnYcSTQPAoPoMsAdRbpPO92iYdxpgIJI-nu2TP-1U79tK0Q97Guc0gp8MC3RyrpfbUGnpnc3B01BT0XTrt0husvF7gI71FbYsCdbW0Bb2FCikUM9rPzfPHe0GvQC_odb3O0LWYK5gXLfO3a1JXJrcv_oDsGMg9Hn71ffIwGt4PzoPLyfhi0L8MNE9YFTR_ykxmsZAmYbOE8TSTUqDIIMIUUEAkWMR4zKQwANoYydBkkBodwSyNNd8nxxtu6exTjb5SK1u7ojmpeiJkcSpDIRoV26i0s947NKp0yzW4VxUy1Sas2jhVG6faJNxYTjaWpS1_mFCuVJJGqqdCLlQ5M43u9A_dv9hPG-SL9w</recordid><startdate>20200601</startdate><enddate>20200601</enddate><creator>Aschwanden, Markus J.</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/0000-0003-0260-2673</orcidid></search><sort><creationdate>20200601</creationdate><title>Global Energetics of Solar Flares. 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Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows</title><author>Aschwanden, Markus J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c380t-4296b6b746f80d8039b664e4ba5e9ae4a5405037064faacff60efba9fc5ad97c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astrophysics</topic><topic>Corona</topic><topic>Electron density</topic><topic>Energy dissipation</topic><topic>Field strength</topic><topic>Free energy</topic><topic>Mach number</topic><topic>Magnetic fields</topic><topic>Magnetic reconnection</topic><topic>Outflow</topic><topic>Physical properties</topic><topic>Scale height</topic><topic>Scaling laws</topic><topic>Solar activity</topic><topic>Solar corona</topic><topic>Solar coronal heating</topic><topic>Solar coronal loops</topic><topic>Solar energy</topic><topic>Solar flares</topic><topic>Solar magnetic fields</topic><topic>Solar magnetic reconnection</topic><topic>Solar observatories</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aschwanden, Markus J.</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>Aschwanden, Markus J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Global Energetics of Solar Flares. X. Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2020-06-01</date><risdate>2020</risdate><volume>895</volume><issue>2</issue><spage>134</spage><pages>134-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We investigate physical scaling laws for magnetic energy dissipation in solar flares, in the framework of the Sweet-Parker model and the Petschek model. We find that the total dissipated magnetic energy Ediss in a flare depends on the mean magnetic field component Bf associated with the free energy Ef, the length scale L of the magnetic area, the hydrostatic density scale height λ of the solar corona, the Alfvén Mach number MA = v1/vA (the ratio of the inflow speed v1 to the Alfvénic outflow speed vA), and the flare duration τf, i.e., , where the Alfvén speed depends on the nonpotential field strength Bnp and the mean electron density ne in the reconnection outflow. Using MDI/Solar Dynamics Observatory (SDO) and AIA/SDO observations and 3D magnetic field solutions obtained with the vertical-current approximation non-linear force-free field code we measure all physical parameters necessary to test scaling laws, which represents a new method to measure Alfvén Mach numbers MA, the reconnection rate, and the total free energy dissipated in solar flares.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ab8aec</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0003-0260-2673</orcidid><oa>free_for_read</oa></addata></record> |
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| language | eng |
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| subjects | Astrophysics Corona Electron density Energy dissipation Field strength Free energy Mach number Magnetic fields Magnetic reconnection Outflow Physical properties Scale height Scaling laws Solar activity Solar corona Solar coronal heating Solar coronal loops Solar energy Solar flares Solar magnetic fields Solar magnetic reconnection Solar observatories |
| title | Global Energetics of Solar Flares. X. Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows |
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