On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation
Three-dimensional steady state transport equation of galactic cosmic rays with drift included is solved by means of newly achieved Fortran code in two cases: 1) Fisk’s type of heliospheric magnetic field dominates in the heliosphere; 2) standard Parker field fills the interplanetary space. The spher...
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| Опубліковано в: : | Кинематика и физика небесных тел |
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| Дата: | 2005 |
| Автори: | , , |
| Формат: | Стаття |
| Мова: | Англійська |
| Опубліковано: |
Головна астрономічна обсерваторія НАН України
2005
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| Теми: | |
| Онлайн доступ: | https://nasplib.isofts.kiev.ua/handle/123456789/79633 |
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| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Цитувати: | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation / Z. Kobylinski, A. Ajabshirizadeh, A. Wysokinski // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 159-164. — Бібліогр.: 26 назв. — англ. |
Репозитарії
Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862735687098302464 |
|---|---|
| author | Kobylinski, Z. Ajabshirizadeh, A. Wysokinski, A. |
| author_facet | Kobylinski, Z. Ajabshirizadeh, A. Wysokinski, A. |
| citation_txt | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation / Z. Kobylinski, A. Ajabshirizadeh, A. Wysokinski // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 159-164. — Бібліогр.: 26 назв. — англ. |
| collection | DSpace DC |
| container_title | Кинематика и физика небесных тел |
| description | Three-dimensional steady state transport equation of galactic cosmic rays with drift included is solved by means of newly achieved Fortran code in two cases: 1) Fisk’s type of heliospheric magnetic field dominates in the heliosphere; 2) standard Parker field fills the interplanetary space. The spherically symmetric heliosphere bounded at a distance of 100 AU is assumed. In the calculations the parallel and perpendicular diffusion coefficients are proportional to 1/B, anti-symmetric element of the diffusion tensor has the form derived under the assumption of week-scattering. The computed modulated spectra are presented and compared with experimental data (IMP3, IMP8, balloons, and CAPRICE) for the minimum period of solar activity. The best fit is obtained when the index of the power of rigidity in diffusion coefficient formula is less than 0.8.
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| first_indexed | 2025-12-07T19:50:09Z |
| format | Article |
| fulltext | |
| id | nasplib_isofts_kiev_ua-123456789-79633 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 0233-7665 |
| language | English |
| last_indexed | 2025-12-07T19:50:09Z |
| publishDate | 2005 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Kobylinski, Z. Ajabshirizadeh, A. Wysokinski, A. 2015-04-03T16:43:15Z 2015-04-03T16:43:15Z 2005 On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation / Z. Kobylinski, A. Ajabshirizadeh, A. Wysokinski // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 159-164. — Бібліогр.: 26 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79633 Three-dimensional steady state transport equation of galactic cosmic rays with drift included is solved by means of newly achieved Fortran code in two cases: 1) Fisk’s type of heliospheric magnetic field dominates in the heliosphere; 2) standard Parker field fills the interplanetary space. The spherically symmetric heliosphere bounded at a distance of 100 AU is assumed. In the calculations the parallel and perpendicular diffusion coefficients are proportional to 1/B, anti-symmetric element of the diffusion tensor has the form derived under the assumption of week-scattering. The computed modulated spectra are presented and compared with experimental data (IMP3, IMP8, balloons, and CAPRICE) for the minimum period of solar activity. The best fit is obtained when the index of the power of rigidity in diffusion coefficient formula is less than 0.8. Z. K. acknowledges the Main Astronomical Observatory, Kyiv, Ukraine, for the financial support which has enabled him to participate in the MAO-2004 Conference. The calculations were performed at the WCSS, Wroclaw. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS2: Physics of Solar Atmosphere On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation Article published earlier |
| spellingShingle | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation Kobylinski, Z. Ajabshirizadeh, A. Wysokinski, A. MS2: Physics of Solar Atmosphere |
| title | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation |
| title_full | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation |
| title_fullStr | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation |
| title_full_unstemmed | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation |
| title_short | On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation |
| title_sort | on the consequences of fisk's type magnetic field configuration for galactic cosmic ray modulation |
| topic | MS2: Physics of Solar Atmosphere |
| topic_facet | MS2: Physics of Solar Atmosphere |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/79633 |
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