Hydrodynamic modeling of an X-ray flare on Proxima Centauri observed by the Einstein telescope
Hydrodynamic numerical calculations of a flare which occurred on Proxima Centauri and was observed by the Einstein satellite on August 20, 1980 at 12:50 UT are presented. The highlights of the hydrodynamic code are reviewed, and the physical and geometrical parameters necessary for the calculations...
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| Veröffentlicht in: | Astrophys. J.; (United States) 1988-05, Vol.328 (1), p.256-264 |
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| container_title | Astrophys. J.; (United States) |
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| creator | REALE, F PERES, G SERIO, S ROSNER, R SCHMITT, J. H. M. M |
| description | Hydrodynamic numerical calculations of a flare which occurred on Proxima Centauri and was observed by the Einstein satellite on August 20, 1980 at 12:50 UT are presented. The highlights of the hydrodynamic code are reviewed, and the physical and geometrical parameters necessary for the calculations are derived and compared with observations. The results are consistent with the stellar flare being caused by the rapid dissipation of 5.9 x 10 to the 31st ergs, within a magnetic loop structure whose semilength is 7 x 10 to the 9th cm and cross-sectional radius is 7.3 x 10 to the 8th cm. The results provide evidence that flares on late-type stars can be described by a hydrodynamic model with a relatively simple geometry, similar to solar compact flares. 39 references. |
| doi_str_mv | 10.1086/166288 |
| format | Article |
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H. M. M</creator><creatorcontrib>REALE, F ; PERES, G ; SERIO, S ; ROSNER, R ; SCHMITT, J. H. M. M ; Palermo, Osservatorio Astronomico (Italy) ; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA) ; Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany, F.R.)</creatorcontrib><description>Hydrodynamic numerical calculations of a flare which occurred on Proxima Centauri and was observed by the Einstein satellite on August 20, 1980 at 12:50 UT are presented. The highlights of the hydrodynamic code are reviewed, and the physical and geometrical parameters necessary for the calculations are derived and compared with observations. The results are consistent with the stellar flare being caused by the rapid dissipation of 5.9 x 10 to the 31st ergs, within a magnetic loop structure whose semilength is 7 x 10 to the 9th cm and cross-sectional radius is 7.3 x 10 to the 8th cm. The results provide evidence that flares on late-type stars can be described by a hydrodynamic model with a relatively simple geometry, similar to solar compact flares. 39 references.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/166288</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Chicago, IL: University of Chicago Press</publisher><subject>Astronomy ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COMPARATIVE EVALUATIONS ; COSMIC RAY SOURCES ; COSMIC X-RAY SOURCES ; DATA PROCESSING ; Earth, ocean, space ; ENERGY LOSSES ; Exact sciences and technology ; Flare stars (uv ceti, rs canum venaticorum, fu orionis, r coronae borealis variables, etc.) ; HYDRODYNAMIC MODEL ; LOSSES ; MAGNETIC FIELD CONFIGURATIONS ; MAGNETIC FLUX ; MATHEMATICAL MODELS ; PARTICLE MODELS ; PROCESSING ; Stars ; STATISTICAL MODELS ; STELLAR ACTIVITY ; STELLAR FLARES ; TELESCOPES ; THERMODYNAMIC MODEL 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources ; Variable and peculiar stars (including novae)</subject><ispartof>Astrophys. 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H. M. M</creatorcontrib><creatorcontrib>Palermo, Osservatorio Astronomico (Italy)</creatorcontrib><creatorcontrib>Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)</creatorcontrib><creatorcontrib>Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany, F.R.)</creatorcontrib><title>Hydrodynamic modeling of an X-ray flare on Proxima Centauri observed by the Einstein telescope</title><title>Astrophys. J.; (United States)</title><description>Hydrodynamic numerical calculations of a flare which occurred on Proxima Centauri and was observed by the Einstein satellite on August 20, 1980 at 12:50 UT are presented. The highlights of the hydrodynamic code are reviewed, and the physical and geometrical parameters necessary for the calculations are derived and compared with observations. The results are consistent with the stellar flare being caused by the rapid dissipation of 5.9 x 10 to the 31st ergs, within a magnetic loop structure whose semilength is 7 x 10 to the 9th cm and cross-sectional radius is 7.3 x 10 to the 8th cm. The results provide evidence that flares on late-type stars can be described by a hydrodynamic model with a relatively simple geometry, similar to solar compact flares. 39 references.</description><subject>Astronomy</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>COSMIC RAY SOURCES</subject><subject>COSMIC X-RAY SOURCES</subject><subject>DATA PROCESSING</subject><subject>Earth, ocean, space</subject><subject>ENERGY LOSSES</subject><subject>Exact sciences and technology</subject><subject>Flare stars (uv ceti, rs canum venaticorum, fu orionis, r coronae borealis variables, etc.)</subject><subject>HYDRODYNAMIC MODEL</subject><subject>LOSSES</subject><subject>MAGNETIC FIELD CONFIGURATIONS</subject><subject>MAGNETIC FLUX</subject><subject>MATHEMATICAL MODELS</subject><subject>PARTICLE MODELS</subject><subject>PROCESSING</subject><subject>Stars</subject><subject>STATISTICAL MODELS</subject><subject>STELLAR ACTIVITY</subject><subject>STELLAR FLARES</subject><subject>TELESCOPES</subject><subject>THERMODYNAMIC MODEL 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources</subject><subject>Variable and peculiar stars (including novae)</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1988</creationdate><recordtype>article</recordtype><recordid>eNo90E1LAzEQBuAgCtaqvyGIeFvN12aTo5RqhYIeFHpySbMTG9kmJYni_nu3VDwNAw8zvC9Cl5TcUqLkHZWSKXWEJrTmqhK8bo7RhBAiKsmb1Sk6y_lzvzKtJ-h9MXQpdkMwW2_xNnbQ-_CBo8Mm4FWVzIBdbxLgGPBLij9-a_AMQjFfyeO4zpC-ocPrAZcN4LkPuYAPuEAP2cYdnKMTZ_oMF39zit4e5q-zRbV8fnya3S8rywQtFUhtuSZcOMVULUAoCta4TgutqBOMMbKmSumOWWMsNU4aSnhtLIwRG675FF0d7sZcfJutL2A3NoYAtrRS85prMaKbA7Ip5pzAtbs05klDS0m7r649VDfC6wPcmWxN75IJ1ud_3chGq_HpLwY0bJo</recordid><startdate>19880501</startdate><enddate>19880501</enddate><creator>REALE, F</creator><creator>PERES, G</creator><creator>SERIO, S</creator><creator>ROSNER, R</creator><creator>SCHMITT, J. 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M</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c241t-e69c39034f82854e481ecafd94981f42220b1889d2caac1af6a1035ace5387393</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1988</creationdate><topic>Astronomy</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>COSMIC RAY SOURCES</topic><topic>COSMIC X-RAY SOURCES</topic><topic>DATA PROCESSING</topic><topic>Earth, ocean, space</topic><topic>ENERGY LOSSES</topic><topic>Exact sciences and technology</topic><topic>Flare stars (uv ceti, rs canum venaticorum, fu orionis, r coronae borealis variables, etc.)</topic><topic>HYDRODYNAMIC MODEL</topic><topic>LOSSES</topic><topic>MAGNETIC FIELD CONFIGURATIONS</topic><topic>MAGNETIC FLUX</topic><topic>MATHEMATICAL MODELS</topic><topic>PARTICLE MODELS</topic><topic>PROCESSING</topic><topic>Stars</topic><topic>STATISTICAL MODELS</topic><topic>STELLAR ACTIVITY</topic><topic>STELLAR FLARES</topic><topic>TELESCOPES</topic><topic>THERMODYNAMIC MODEL 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources</topic><topic>Variable and peculiar stars (including novae)</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>REALE, F</creatorcontrib><creatorcontrib>PERES, G</creatorcontrib><creatorcontrib>SERIO, S</creatorcontrib><creatorcontrib>ROSNER, R</creatorcontrib><creatorcontrib>SCHMITT, J. H. M. M</creatorcontrib><creatorcontrib>Palermo, Osservatorio Astronomico (Italy)</creatorcontrib><creatorcontrib>Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)</creatorcontrib><creatorcontrib>Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany, F.R.)</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Astrophys. J.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>REALE, F</au><au>PERES, G</au><au>SERIO, S</au><au>ROSNER, R</au><au>SCHMITT, J. H. M. M</au><aucorp>Palermo, Osservatorio Astronomico (Italy)</aucorp><aucorp>Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)</aucorp><aucorp>Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany, F.R.)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Hydrodynamic modeling of an X-ray flare on Proxima Centauri observed by the Einstein telescope</atitle><jtitle>Astrophys. J.; (United States)</jtitle><date>1988-05-01</date><risdate>1988</risdate><volume>328</volume><issue>1</issue><spage>256</spage><epage>264</epage><pages>256-264</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>Hydrodynamic numerical calculations of a flare which occurred on Proxima Centauri and was observed by the Einstein satellite on August 20, 1980 at 12:50 UT are presented. The highlights of the hydrodynamic code are reviewed, and the physical and geometrical parameters necessary for the calculations are derived and compared with observations. The results are consistent with the stellar flare being caused by the rapid dissipation of 5.9 x 10 to the 31st ergs, within a magnetic loop structure whose semilength is 7 x 10 to the 9th cm and cross-sectional radius is 7.3 x 10 to the 8th cm. The results provide evidence that flares on late-type stars can be described by a hydrodynamic model with a relatively simple geometry, similar to solar compact flares. 39 references.</abstract><cop>Chicago, IL</cop><pub>University of Chicago Press</pub><doi>10.1086/166288</doi><tpages>9</tpages><oa>free_for_read</oa></addata></record> |
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| ispartof | Astrophys. J.; (United States), 1988-05, Vol.328 (1), p.256-264 |
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| language | eng |
| recordid | cdi_crossref_primary_10_1086_166288 |
| source | Alma/SFX Local Collection |
| subjects | Astronomy CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COMPARATIVE EVALUATIONS COSMIC RAY SOURCES COSMIC X-RAY SOURCES DATA PROCESSING Earth, ocean, space ENERGY LOSSES Exact sciences and technology Flare stars (uv ceti, rs canum venaticorum, fu orionis, r coronae borealis variables, etc.) HYDRODYNAMIC MODEL LOSSES MAGNETIC FIELD CONFIGURATIONS MAGNETIC FLUX MATHEMATICAL MODELS PARTICLE MODELS PROCESSING Stars STATISTICAL MODELS STELLAR ACTIVITY STELLAR FLARES TELESCOPES THERMODYNAMIC MODEL 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources Variable and peculiar stars (including novae) |
| title | Hydrodynamic modeling of an X-ray flare on Proxima Centauri observed by the Einstein telescope |
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