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Power law burst lifetime distribution of the SYM‐H index
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| Zeitschriftentitel: | Geophysical Research Letters |
|---|---|
| Personen und Körperschaften: | , |
| In: | Geophysical Research Letters, 34, 2007, 4 |
| Format: | E-Article |
| Sprache: | Englisch |
| veröffentlicht: |
American Geophysical Union (AGU)
|
| Schlagwörter: |
| author_facet |
Wanliss, J. A. Weygand, J. M. Wanliss, J. A. Weygand, J. M. |
|---|---|
| author |
Wanliss, J. A. Weygand, J. M. |
| spellingShingle |
Wanliss, J. A. Weygand, J. M. Geophysical Research Letters Power law burst lifetime distribution of the SYM‐H index General Earth and Planetary Sciences Geophysics |
| author_sort |
wanliss, j. a. |
| spelling |
Wanliss, J. A. Weygand, J. M. 0094-8276 1944-8007 American Geophysical Union (AGU) General Earth and Planetary Sciences Geophysics http://dx.doi.org/10.1029/2006gl028235 <jats:p>We have examined the burst lifetime distribution functions of solar wind <jats:italic>VB</jats:italic><jats:sub><jats:italic>s</jats:italic></jats:sub> and ɛ for 1995–2005 and compared them with the same for contemporaneous <jats:italic>SYM‐H.</jats:italic> The analysis yields clear power‐law exponents of the lifetime probability distributions. When we analyzed three years around solar minimum we found similar scaling behavior for all the variables, including <jats:italic>SYM‐H</jats:italic>. However, for the three years around solar maximum the difference between solar wind and <jats:italic>SYM‐H</jats:italic> scaling was very clear. The fact that power laws were consistently observed for different activity thresholds show that these features are robust and repeatable, although scaling can vary depending on solar cycle. During solar maximum it appears that the scaling properties of the low‐latitude magnetosphere, whose output is recorded by <jats:italic>SYM‐H</jats:italic>, are not purely a direct response to the scale‐free properties of the solar wind but are due to inherent properties of the magnetosphere. Since <jats:italic>SYM‐H</jats:italic> scaling is remarkably robust, irrespective of solar cycle, it could be that the solar wind <jats:italic>never</jats:italic> acts as a direct driver for the <jats:italic>SYM‐H</jats:italic> scaling.</jats:p> Power law burst lifetime distribution of the SYM‐H index Geophysical Research Letters |
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10.1029/2006gl028235 |
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American Geophysical Union (AGU), 2007 |
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0094-8276 1944-8007 |
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American Geophysical Union (AGU) |
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Geophysical Research Letters |
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| title |
Power law burst lifetime distribution of the SYM‐H index |
| title_unstemmed |
Power law burst lifetime distribution of the SYM‐H index |
| title_full |
Power law burst lifetime distribution of the SYM‐H index |
| title_fullStr |
Power law burst lifetime distribution of the SYM‐H index |
| title_full_unstemmed |
Power law burst lifetime distribution of the SYM‐H index |
| title_short |
Power law burst lifetime distribution of the SYM‐H index |
| title_sort |
power law burst lifetime distribution of the sym‐h index |
| topic |
General Earth and Planetary Sciences Geophysics |
| url |
http://dx.doi.org/10.1029/2006gl028235 |
| publishDate |
2007 |
| physical |
|
| description |
<jats:p>We have examined the burst lifetime distribution functions of solar wind <jats:italic>VB</jats:italic><jats:sub><jats:italic>s</jats:italic></jats:sub> and ɛ for 1995–2005 and compared them with the same for contemporaneous <jats:italic>SYM‐H.</jats:italic> The analysis yields clear power‐law exponents of the lifetime probability distributions. When we analyzed three years around solar minimum we found similar scaling behavior for all the variables, including <jats:italic>SYM‐H</jats:italic>. However, for the three years around solar maximum the difference between solar wind and <jats:italic>SYM‐H</jats:italic> scaling was very clear. The fact that power laws were consistently observed for different activity thresholds show that these features are robust and repeatable, although scaling can vary depending on solar cycle. During solar maximum it appears that the scaling properties of the low‐latitude magnetosphere, whose output is recorded by <jats:italic>SYM‐H</jats:italic>, are not purely a direct response to the scale‐free properties of the solar wind but are due to inherent properties of the magnetosphere. Since <jats:italic>SYM‐H</jats:italic> scaling is remarkably robust, irrespective of solar cycle, it could be that the solar wind <jats:italic>never</jats:italic> acts as a direct driver for the <jats:italic>SYM‐H</jats:italic> scaling.</jats:p> |
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| author | Wanliss, J. A., Weygand, J. M. |
| author_facet | Wanliss, J. A., Weygand, J. M., Wanliss, J. A., Weygand, J. M. |
| author_sort | wanliss, j. a. |
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| description | <jats:p>We have examined the burst lifetime distribution functions of solar wind <jats:italic>VB</jats:italic><jats:sub><jats:italic>s</jats:italic></jats:sub> and ɛ for 1995–2005 and compared them with the same for contemporaneous <jats:italic>SYM‐H.</jats:italic> The analysis yields clear power‐law exponents of the lifetime probability distributions. When we analyzed three years around solar minimum we found similar scaling behavior for all the variables, including <jats:italic>SYM‐H</jats:italic>. However, for the three years around solar maximum the difference between solar wind and <jats:italic>SYM‐H</jats:italic> scaling was very clear. The fact that power laws were consistently observed for different activity thresholds show that these features are robust and repeatable, although scaling can vary depending on solar cycle. During solar maximum it appears that the scaling properties of the low‐latitude magnetosphere, whose output is recorded by <jats:italic>SYM‐H</jats:italic>, are not purely a direct response to the scale‐free properties of the solar wind but are due to inherent properties of the magnetosphere. Since <jats:italic>SYM‐H</jats:italic> scaling is remarkably robust, irrespective of solar cycle, it could be that the solar wind <jats:italic>never</jats:italic> acts as a direct driver for the <jats:italic>SYM‐H</jats:italic> scaling.</jats:p> |
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| format_nrw | Article, E-Article |
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| imprint | American Geophysical Union (AGU), 2007 |
| imprint_str_mv | American Geophysical Union (AGU), 2007 |
| institution | DE-Zwi2, DE-D161, DE-Zi4, DE-Gla1, DE-15, DE-Pl11, DE-Rs1, DE-14, DE-105, DE-Ch1, DE-L229, DE-D275, DE-Bn3, DE-Brt1 |
| issn | 0094-8276, 1944-8007 |
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| publisher | American Geophysical Union (AGU) |
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| series | Geophysical Research Letters |
| source_id | 49 |
| spelling | Wanliss, J. A. Weygand, J. M. 0094-8276 1944-8007 American Geophysical Union (AGU) General Earth and Planetary Sciences Geophysics http://dx.doi.org/10.1029/2006gl028235 <jats:p>We have examined the burst lifetime distribution functions of solar wind <jats:italic>VB</jats:italic><jats:sub><jats:italic>s</jats:italic></jats:sub> and ɛ for 1995–2005 and compared them with the same for contemporaneous <jats:italic>SYM‐H.</jats:italic> The analysis yields clear power‐law exponents of the lifetime probability distributions. When we analyzed three years around solar minimum we found similar scaling behavior for all the variables, including <jats:italic>SYM‐H</jats:italic>. However, for the three years around solar maximum the difference between solar wind and <jats:italic>SYM‐H</jats:italic> scaling was very clear. The fact that power laws were consistently observed for different activity thresholds show that these features are robust and repeatable, although scaling can vary depending on solar cycle. During solar maximum it appears that the scaling properties of the low‐latitude magnetosphere, whose output is recorded by <jats:italic>SYM‐H</jats:italic>, are not purely a direct response to the scale‐free properties of the solar wind but are due to inherent properties of the magnetosphere. Since <jats:italic>SYM‐H</jats:italic> scaling is remarkably robust, irrespective of solar cycle, it could be that the solar wind <jats:italic>never</jats:italic> acts as a direct driver for the <jats:italic>SYM‐H</jats:italic> scaling.</jats:p> Power law burst lifetime distribution of the SYM‐H index Geophysical Research Letters |
| spellingShingle | Wanliss, J. A., Weygand, J. M., Geophysical Research Letters, Power law burst lifetime distribution of the SYM‐H index, General Earth and Planetary Sciences, Geophysics |
| title | Power law burst lifetime distribution of the SYM‐H index |
| title_full | Power law burst lifetime distribution of the SYM‐H index |
| title_fullStr | Power law burst lifetime distribution of the SYM‐H index |
| title_full_unstemmed | Power law burst lifetime distribution of the SYM‐H index |
| title_short | Power law burst lifetime distribution of the SYM‐H index |
| title_sort | power law burst lifetime distribution of the sym‐h index |
| title_unstemmed | Power law burst lifetime distribution of the SYM‐H index |
| topic | General Earth and Planetary Sciences, Geophysics |
| url | http://dx.doi.org/10.1029/2006gl028235 |