The effects of nonequilibrium ionization on the radiative losses of the solar corona
The emissivity of the ions of carbon and oxygen has been recalculated for a set of solar coronal loop models with a steady state siphon flow. The ion densities were calculated from the plasma velocities, temperatures, and densities of the models, and large departures from equilibrium were found. For...
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| Veröffentlicht in: | The Astrophysical journal 1990-10, Vol.362 (1), p.370-378 |
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| container_end_page | 378 |
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| container_start_page | 370 |
| container_title | The Astrophysical journal |
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| creator | Spadaro, D. Zappala, R. A. Antiochos, S. K. Lanzafame, G. Noci, G. |
| description | The emissivity of the ions of carbon and oxygen has been recalculated for a set of solar coronal loop models with a steady state siphon flow. The ion densities were calculated from the plasma velocities, temperatures, and densities of the models, and large departures from equilibrium were found. For purposes of comparison, the emissivity was calculated with and without the approximation of ionization equilibrium. Considerable differences in the radiative loss function Lambda(T) curve between equilibrium and nonequilibrium conditions were found. The nonequilibrium Lambda(T) function was then used to solve again the steady state flow equations of the loop models. The differences in the structure of these models with respect to the models calculated adopting the Lambda(T) curve in equilibrium are discussed. |
| doi_str_mv | 10.1086/169273 |
| format | Article |
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A. ; Antiochos, S. K. ; Lanzafame, G. ; Noci, G.</creator><creatorcontrib>Spadaro, D. ; Zappala, R. A. ; Antiochos, S. K. ; Lanzafame, G. ; Noci, G.</creatorcontrib><description>The emissivity of the ions of carbon and oxygen has been recalculated for a set of solar coronal loop models with a steady state siphon flow. The ion densities were calculated from the plasma velocities, temperatures, and densities of the models, and large departures from equilibrium were found. For purposes of comparison, the emissivity was calculated with and without the approximation of ionization equilibrium. Considerable differences in the radiative loss function Lambda(T) curve between equilibrium and nonequilibrium conditions were found. The nonequilibrium Lambda(T) function was then used to solve again the steady state flow equations of the loop models. The differences in the structure of these models with respect to the models calculated adopting the Lambda(T) curve in equilibrium are discussed.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/169273</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Legacy CDMS: University of Chicago Press</publisher><subject>640104 - Astrophysics & Cosmology- Solar Phenomena ; ACCRETION DISKS ; Astronomy ; ATMOSPHERES ; CARBON IONS ; CHARGED PARTICLES ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; Corona. 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A.</creatorcontrib><creatorcontrib>Antiochos, S. K.</creatorcontrib><creatorcontrib>Lanzafame, G.</creatorcontrib><creatorcontrib>Noci, G.</creatorcontrib><title>The effects of nonequilibrium ionization on the radiative losses of the solar corona</title><title>The Astrophysical journal</title><description>The emissivity of the ions of carbon and oxygen has been recalculated for a set of solar coronal loop models with a steady state siphon flow. The ion densities were calculated from the plasma velocities, temperatures, and densities of the models, and large departures from equilibrium were found. For purposes of comparison, the emissivity was calculated with and without the approximation of ionization equilibrium. Considerable differences in the radiative loss function Lambda(T) curve between equilibrium and nonequilibrium conditions were found. The nonequilibrium Lambda(T) function was then used to solve again the steady state flow equations of the loop models. The differences in the structure of these models with respect to the models calculated adopting the Lambda(T) curve in equilibrium are discussed.</description><subject>640104 - Astrophysics & Cosmology- Solar Phenomena</subject><subject>ACCRETION DISKS</subject><subject>Astronomy</subject><subject>ATMOSPHERES</subject><subject>CARBON IONS</subject><subject>CHARGED PARTICLES</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>Corona. Coronal loops, streamers, and holes</subject><subject>COSMIC RADIO SOURCES</subject><subject>Earth, ocean, space</subject><subject>ENERGY LOSSES</subject><subject>Exact sciences and technology</subject><subject>FLUID FLOW</subject><subject>HOT PLASMA</subject><subject>ION DENSITY</subject><subject>IONIZATION</subject><subject>IONS</subject><subject>LOSSES</subject><subject>OXYGEN IONS</subject><subject>PLASMA</subject><subject>PLASMA DENSITY</subject><subject>RADIATION TRANSPORT</subject><subject>SOLAR CORONA</subject><subject>Solar Physics</subject><subject>Solar system</subject><subject>STEADY FLOW</subject><subject>STEADY-STATE CONDITIONS</subject><subject>STELLAR ACTIVITY</subject><subject>STELLAR ATMOSPHERES</subject><subject>STELLAR CORONAE</subject><subject>STELLAR WINDS</subject><subject>SUPERNOVA REMNANTS</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1990</creationdate><recordtype>article</recordtype><sourceid>CYI</sourceid><recordid>eNpFkEtLAzEQx4MoWKt-Ag-LoLfVZJPN4yjiCwpe9uBtmaYTGtkmNdkK-ulNXUEY-DMzv3kScs7oDaNa3jJpGsUPyIy1XNeCt-qQzCilopZcvR2Tk5zf925jzIx03RordA7tmKvoqhADfuz84JfJ7zaVj8F_w1ikKjYWNsHKl8AnVkPMGX-L9vEcB0iVjSkGOCVHDoaMZ386J93jQ3f_XC9en17u7xa1LbPHugFqlHEWDBUOJVsu-YoiNExQVnLWoJMcpEapjdKtEtRKQN2udCtQNnxOLqe2MY--z9aPaNc2hlCO6SVnkipToOsJsqnsm9D12-Q3kL56Rvv9v_rpXwW8msAtZAuDSxCsz_-0EVwp0RbuYuICZOjDmHLJGUZp0xom-A8wRHHB</recordid><startdate>19901010</startdate><enddate>19901010</enddate><creator>Spadaro, D.</creator><creator>Zappala, R. A.</creator><creator>Antiochos, S. K.</creator><creator>Lanzafame, G.</creator><creator>Noci, G.</creator><general>University of Chicago Press</general><scope>CYE</scope><scope>CYI</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>19901010</creationdate><title>The effects of nonequilibrium ionization on the radiative losses of the solar corona</title><author>Spadaro, D. ; Zappala, R. A. ; Antiochos, S. 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Coronal loops, streamers, and holes</topic><topic>COSMIC RADIO SOURCES</topic><topic>Earth, ocean, space</topic><topic>ENERGY LOSSES</topic><topic>Exact sciences and technology</topic><topic>FLUID FLOW</topic><topic>HOT PLASMA</topic><topic>ION DENSITY</topic><topic>IONIZATION</topic><topic>IONS</topic><topic>LOSSES</topic><topic>OXYGEN IONS</topic><topic>PLASMA</topic><topic>PLASMA DENSITY</topic><topic>RADIATION TRANSPORT</topic><topic>SOLAR CORONA</topic><topic>Solar Physics</topic><topic>Solar system</topic><topic>STEADY FLOW</topic><topic>STEADY-STATE CONDITIONS</topic><topic>STELLAR ACTIVITY</topic><topic>STELLAR ATMOSPHERES</topic><topic>STELLAR CORONAE</topic><topic>STELLAR WINDS</topic><topic>SUPERNOVA REMNANTS</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Spadaro, D.</creatorcontrib><creatorcontrib>Zappala, R. A.</creatorcontrib><creatorcontrib>Antiochos, S. K.</creatorcontrib><creatorcontrib>Lanzafame, G.</creatorcontrib><creatorcontrib>Noci, G.</creatorcontrib><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Spadaro, D.</au><au>Zappala, R. A.</au><au>Antiochos, S. K.</au><au>Lanzafame, G.</au><au>Noci, G.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The effects of nonequilibrium ionization on the radiative losses of the solar corona</atitle><jtitle>The Astrophysical journal</jtitle><date>1990-10-10</date><risdate>1990</risdate><volume>362</volume><issue>1</issue><spage>370</spage><epage>378</epage><pages>370-378</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>The emissivity of the ions of carbon and oxygen has been recalculated for a set of solar coronal loop models with a steady state siphon flow. The ion densities were calculated from the plasma velocities, temperatures, and densities of the models, and large departures from equilibrium were found. For purposes of comparison, the emissivity was calculated with and without the approximation of ionization equilibrium. Considerable differences in the radiative loss function Lambda(T) curve between equilibrium and nonequilibrium conditions were found. The nonequilibrium Lambda(T) function was then used to solve again the steady state flow equations of the loop models. The differences in the structure of these models with respect to the models calculated adopting the Lambda(T) curve in equilibrium are discussed.</abstract><cop>Legacy CDMS</cop><pub>University of Chicago Press</pub><doi>10.1086/169273</doi><tpages>9</tpages></addata></record> |
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| ispartof | The Astrophysical journal, 1990-10, Vol.362 (1), p.370-378 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_osti_scitechconnect_6316079 |
| source | NASA Technical Reports Server; Alma/SFX Local Collection |
| subjects | 640104 - Astrophysics & Cosmology- Solar Phenomena ACCRETION DISKS Astronomy ATMOSPHERES CARBON IONS CHARGED PARTICLES CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Corona. Coronal loops, streamers, and holes COSMIC RADIO SOURCES Earth, ocean, space ENERGY LOSSES Exact sciences and technology FLUID FLOW HOT PLASMA ION DENSITY IONIZATION IONS LOSSES OXYGEN IONS PLASMA PLASMA DENSITY RADIATION TRANSPORT SOLAR CORONA Solar Physics Solar system STEADY FLOW STEADY-STATE CONDITIONS STELLAR ACTIVITY STELLAR ATMOSPHERES STELLAR CORONAE STELLAR WINDS SUPERNOVA REMNANTS |
| title | The effects of nonequilibrium ionization on the radiative losses of the solar corona |
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