New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons
Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes lead...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Logachev, Yu. I. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2018 |
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| Anmerkung: |
© Pleiades Publishing, Ltd. 2018 |
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| Übergeordnetes Werk: |
Enthalten in: Physics of atomic nuclei - Pleiades Publishing, 1993, 81(2018), 3 vom: Mai, Seite 384-389 |
|---|---|
| Übergeordnetes Werk: |
volume:81 ; year:2018 ; number:3 ; month:05 ; pages:384-389 |
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| DOI / URN: |
10.1134/S106377881803016X |
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| 520 | |a Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. | ||
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10.1134/S106377881803016X doi (DE-627)OLC2049929285 (DE-He213)S106377881803016X-p DE-627 ger DE-627 rakwb eng 530 VZ Logachev, Yu. I. verfasserin aut New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons 2018 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Pleiades Publishing, Ltd. 2018 Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. Bazilevskaya, G. A. aut Daibog, E. I. aut Ishkov, V. N. aut Lazutin, L. L. aut Surova, G. M. aut Enthalten in Physics of atomic nuclei Pleiades Publishing, 1993 81(2018), 3 vom: Mai, Seite 384-389 (DE-627)131188437 (DE-600)1146378-8 (DE-576)032622155 1063-7788 nnns volume:81 year:2018 number:3 month:05 pages:384-389 https://doi.org/10.1134/S106377881803016X lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OPC-AST GBV_ILN_70 AR 81 2018 3 05 384-389 |
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10.1134/S106377881803016X doi (DE-627)OLC2049929285 (DE-He213)S106377881803016X-p DE-627 ger DE-627 rakwb eng 530 VZ Logachev, Yu. I. verfasserin aut New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons 2018 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Pleiades Publishing, Ltd. 2018 Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. Bazilevskaya, G. A. aut Daibog, E. I. aut Ishkov, V. N. aut Lazutin, L. L. aut Surova, G. M. aut Enthalten in Physics of atomic nuclei Pleiades Publishing, 1993 81(2018), 3 vom: Mai, Seite 384-389 (DE-627)131188437 (DE-600)1146378-8 (DE-576)032622155 1063-7788 nnns volume:81 year:2018 number:3 month:05 pages:384-389 https://doi.org/10.1134/S106377881803016X lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OPC-AST GBV_ILN_70 AR 81 2018 3 05 384-389 |
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10.1134/S106377881803016X doi (DE-627)OLC2049929285 (DE-He213)S106377881803016X-p DE-627 ger DE-627 rakwb eng 530 VZ Logachev, Yu. I. verfasserin aut New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons 2018 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Pleiades Publishing, Ltd. 2018 Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. Bazilevskaya, G. A. aut Daibog, E. I. aut Ishkov, V. N. aut Lazutin, L. L. aut Surova, G. M. aut Enthalten in Physics of atomic nuclei Pleiades Publishing, 1993 81(2018), 3 vom: Mai, Seite 384-389 (DE-627)131188437 (DE-600)1146378-8 (DE-576)032622155 1063-7788 nnns volume:81 year:2018 number:3 month:05 pages:384-389 https://doi.org/10.1134/S106377881803016X lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OPC-AST GBV_ILN_70 AR 81 2018 3 05 384-389 |
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Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. © Pleiades Publishing, Ltd. 2018 |
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Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. © Pleiades Publishing, Ltd. 2018 |
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Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined. © Pleiades Publishing, Ltd. 2018 |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">OLC2049929285</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230504110729.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200820s2018 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1134/S106377881803016X</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2049929285</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)S106377881803016X-p</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Logachev, Yu. I.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Pleiades Publishing, Ltd. 2018</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, Eqm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of Eqm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Bazilevskaya, G. A.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Daibog, E. 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M.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Physics of atomic nuclei</subfield><subfield code="d">Pleiades Publishing, 1993</subfield><subfield code="g">81(2018), 3 vom: Mai, Seite 384-389</subfield><subfield code="w">(DE-627)131188437</subfield><subfield code="w">(DE-600)1146378-8</subfield><subfield code="w">(DE-576)032622155</subfield><subfield code="x">1063-7788</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:81</subfield><subfield code="g">year:2018</subfield><subfield code="g">number:3</subfield><subfield code="g">month:05</subfield><subfield code="g">pages:384-389</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1134/S106377881803016X</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">81</subfield><subfield code="j">2018</subfield><subfield code="e">3</subfield><subfield code="c">05</subfield><subfield code="h">384-389</subfield></datafield></record></collection>
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