Time profile of solar energetic particles fit using a mean free path considering the radial dependence of both magnetic field strength and fluctuations
The radially dependent mean free path of solar energetic particles was calculated by considering the radially dependent magnetic field fluctuation, its correlation length and the variation of magnetic field strength along an Archimedean interplanetary magnetic field. A longer mean free path can be d...
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| Veröffentlicht in: | Earth, planets, and space planets, and space, 2002-01, Vol.54 (6), p.727-732 |
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| creator | SAKAI, Takasuke |
| description | The radially dependent mean free path of solar energetic particles was calculated by considering the radially dependent magnetic field fluctuation, its correlation length and the variation of magnetic field strength along an Archimedean interplanetary magnetic field. A longer mean free path can be deduced as radial distance approaches the sun. That is, the mean free path at 0.1 AU is increased by 10 times for some typical values of radial dependence of magnetic field fluctuation (e.g., power index of radial dependence = −2), compared to the value at 1 AU. The focused pitch angle transport equation without adiabatic deceleration was solved for the obtained mean free path. The calculated time profiles are compared with observations of solar energetic particles. In some cases, very good matches to observed data for longer periods are obtained with shorter mean free paths than the original authors mentioned. |
| doi_str_mv | 10.1186/BF03351725 |
| format | Article |
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A longer mean free path can be deduced as radial distance approaches the sun. That is, the mean free path at 0.1 AU is increased by 10 times for some typical values of radial dependence of magnetic field fluctuation (e.g., power index of radial dependence = −2), compared to the value at 1 AU. The focused pitch angle transport equation without adiabatic deceleration was solved for the obtained mean free path. The calculated time profiles are compared with observations of solar energetic particles. 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A longer mean free path can be deduced as radial distance approaches the sun. That is, the mean free path at 0.1 AU is increased by 10 times for some typical values of radial dependence of magnetic field fluctuation (e.g., power index of radial dependence = −2), compared to the value at 1 AU. The focused pitch angle transport equation without adiabatic deceleration was solved for the obtained mean free path. The calculated time profiles are compared with observations of solar energetic particles. 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Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>Earth, Atmospheric & Aquatic Science Database</collection><collection>Access via ProQuest (Open Access)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><jtitle>Earth, planets, and space</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>SAKAI, Takasuke</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Time profile of solar energetic particles fit using a mean free path considering the radial dependence of both magnetic field strength and fluctuations</atitle><jtitle>Earth, planets, and space</jtitle><date>2002-01-01</date><risdate>2002</risdate><volume>54</volume><issue>6</issue><spage>727</spage><epage>732</epage><pages>727-732</pages><issn>1343-8832</issn><issn>1880-5981</issn><eissn>1880-5981</eissn><abstract>The radially dependent mean free path of solar energetic particles was calculated by considering the radially dependent magnetic field fluctuation, its correlation length and the variation of magnetic field strength along an Archimedean interplanetary magnetic field. A longer mean free path can be deduced as radial distance approaches the sun. That is, the mean free path at 0.1 AU is increased by 10 times for some typical values of radial dependence of magnetic field fluctuation (e.g., power index of radial dependence = −2), compared to the value at 1 AU. The focused pitch angle transport equation without adiabatic deceleration was solved for the obtained mean free path. The calculated time profiles are compared with observations of solar energetic particles. In some cases, very good matches to observed data for longer periods are obtained with shorter mean free paths than the original authors mentioned.</abstract><cop>Tokyo</cop><pub>Terra</pub><doi>10.1186/BF03351725</doi><tpages>6</tpages><oa>free_for_read</oa></addata></record> |
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| identifier | ISSN: 1343-8832 |
| ispartof | Earth, planets, and space, 2002-01, Vol.54 (6), p.727-732 |
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| language | eng |
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| source | SpringerNature Journals; Springer Nature OA Free Journals; J-STAGE (Japan Science & Technology Information Aggregator, Electronic) Freely Available Titles - Japanese; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astronomy Deceleration Earth, ocean, space Energetic particles Exact sciences and technology Field strength Interplanetary magnetic field Magnetic fields Mathematical analysis Mean free path Particle radiation, solar wind Pitch (inclination) Solar energetic particles Solar physics Solar system Transport equations |
| title | Time profile of solar energetic particles fit using a mean free path considering the radial dependence of both magnetic field strength and fluctuations |
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