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Ion‐scale spectral break of solar wind turbulence at high and low beta
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| Zeitschriftentitel: | Geophysical Research Letters |
|---|---|
| Personen und Körperschaften: | , , , , |
| In: | Geophysical Research Letters, 41, 2014, 22, S. 8081-8088 |
| Format: | E-Article |
| Sprache: | Englisch |
| veröffentlicht: |
American Geophysical Union (AGU)
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| Schlagwörter: |
| author_facet |
Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. |
|---|---|
| author |
Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. |
| spellingShingle |
Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. Geophysical Research Letters Ion‐scale spectral break of solar wind turbulence at high and low beta General Earth and Planetary Sciences Geophysics |
| author_sort |
chen, c. h. k. |
| spelling |
Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. 0094-8276 1944-8007 American Geophysical Union (AGU) General Earth and Planetary Sciences Geophysics http://dx.doi.org/10.1002/2014gl062009 <jats:title>Abstract</jats:title><jats:p>The power spectrum of magnetic fluctuations in the solar wind at 1 AU displays a break between two power laws in the range of spacecraft‐frame frequencies 0.1 to 1 Hz. These frequencies correspond to spatial scales in the plasma frame near the proton gyroradius <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub> and proton inertial length <jats:italic>d</jats:italic><jats:sub>i</jats:sub>. At 1 AU it is difficult to determine which of these is associated with the break, since <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/grl52226-math-0001.png" xlink:title="urn:x-wiley:grl:media:grl52226:grl52226-math-0001" /> and the perpendicular ion plasma beta is typically <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>∼1. To address this, several exceptional intervals with <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 and <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 were investigated, during which these scales were well separated. It was found that for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 the break occurs at <jats:italic>d</jats:italic><jats:sub>i</jats:sub> and for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 at <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub>, i.e., the larger of the two scales. Possible explanations for these results are discussed, including Alfvén wave dispersion, damping, and current sheets.</jats:p> Ion‐scale spectral break of solar wind turbulence at high and low beta Geophysical Research Letters |
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10.1002/2014gl062009 |
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Online Free |
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Geologie und Paläontologie Geographie Physik |
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American Geophysical Union (AGU), 2014 |
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American Geophysical Union (AGU), 2014 |
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0094-8276 1944-8007 |
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2014 |
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Geophysical Research Letters |
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| title |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_unstemmed |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_full |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_fullStr |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_full_unstemmed |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_short |
Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_sort |
ion‐scale spectral break of solar wind turbulence at high and low beta |
| topic |
General Earth and Planetary Sciences Geophysics |
| url |
http://dx.doi.org/10.1002/2014gl062009 |
| publishDate |
2014 |
| physical |
8081-8088 |
| description |
<jats:title>Abstract</jats:title><jats:p>The power spectrum of magnetic fluctuations in the solar wind at 1 AU displays a break between two power laws in the range of spacecraft‐frame frequencies 0.1 to 1 Hz. These frequencies correspond to spatial scales in the plasma frame near the proton gyroradius <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub> and proton inertial length <jats:italic>d</jats:italic><jats:sub>i</jats:sub>. At 1 AU it is difficult to determine which of these is associated with the break, since <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/grl52226-math-0001.png" xlink:title="urn:x-wiley:grl:media:grl52226:grl52226-math-0001" /> and the perpendicular ion plasma beta is typically <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>∼1. To address this, several exceptional intervals with <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 and <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 were investigated, during which these scales were well separated. It was found that for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 the break occurs at <jats:italic>d</jats:italic><jats:sub>i</jats:sub> and for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 at <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub>, i.e., the larger of the two scales. Possible explanations for these results are discussed, including Alfvén wave dispersion, damping, and current sheets.</jats:p> |
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| author | Chen, C. H. K., Leung, L., Boldyrev, S., Maruca, B. A., Bale, S. D. |
| author_facet | Chen, C. H. K., Leung, L., Boldyrev, S., Maruca, B. A., Bale, S. D., Chen, C. H. K., Leung, L., Boldyrev, S., Maruca, B. A., Bale, S. D. |
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| description | <jats:title>Abstract</jats:title><jats:p>The power spectrum of magnetic fluctuations in the solar wind at 1 AU displays a break between two power laws in the range of spacecraft‐frame frequencies 0.1 to 1 Hz. These frequencies correspond to spatial scales in the plasma frame near the proton gyroradius <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub> and proton inertial length <jats:italic>d</jats:italic><jats:sub>i</jats:sub>. At 1 AU it is difficult to determine which of these is associated with the break, since <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/grl52226-math-0001.png" xlink:title="urn:x-wiley:grl:media:grl52226:grl52226-math-0001" /> and the perpendicular ion plasma beta is typically <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>∼1. To address this, several exceptional intervals with <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 and <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 were investigated, during which these scales were well separated. It was found that for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 the break occurs at <jats:italic>d</jats:italic><jats:sub>i</jats:sub> and for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 at <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub>, i.e., the larger of the two scales. Possible explanations for these results are discussed, including Alfvén wave dispersion, damping, and current sheets.</jats:p> |
| doi_str_mv | 10.1002/2014gl062009 |
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| imprint | American Geophysical Union (AGU), 2014 |
| imprint_str_mv | American Geophysical Union (AGU), 2014 |
| institution | DE-15, DE-Pl11, DE-Rs1, DE-105, DE-14, DE-Ch1, DE-L229, DE-D275, DE-Bn3, DE-Brt1, DE-Zwi2, DE-D161, DE-Gla1, DE-Zi4 |
| issn | 0094-8276, 1944-8007 |
| issn_str_mv | 0094-8276, 1944-8007 |
| language | English |
| last_indexed | 2024-03-01T17:07:34.441Z |
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| mega_collection | American Geophysical Union (AGU) (CrossRef) |
| physical | 8081-8088 |
| publishDate | 2014 |
| publishDateSort | 2014 |
| publisher | American Geophysical Union (AGU) |
| record_format | ai |
| recordtype | ai |
| series | Geophysical Research Letters |
| source_id | 49 |
| spelling | Chen, C. H. K. Leung, L. Boldyrev, S. Maruca, B. A. Bale, S. D. 0094-8276 1944-8007 American Geophysical Union (AGU) General Earth and Planetary Sciences Geophysics http://dx.doi.org/10.1002/2014gl062009 <jats:title>Abstract</jats:title><jats:p>The power spectrum of magnetic fluctuations in the solar wind at 1 AU displays a break between two power laws in the range of spacecraft‐frame frequencies 0.1 to 1 Hz. These frequencies correspond to spatial scales in the plasma frame near the proton gyroradius <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub> and proton inertial length <jats:italic>d</jats:italic><jats:sub>i</jats:sub>. At 1 AU it is difficult to determine which of these is associated with the break, since <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/grl52226-math-0001.png" xlink:title="urn:x-wiley:grl:media:grl52226:grl52226-math-0001" /> and the perpendicular ion plasma beta is typically <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>∼1. To address this, several exceptional intervals with <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 and <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 were investigated, during which these scales were well separated. It was found that for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≪1 the break occurs at <jats:italic>d</jats:italic><jats:sub>i</jats:sub> and for <jats:italic>β</jats:italic><jats:sub>⊥i</jats:sub>≫1 at <jats:italic>ρ</jats:italic><jats:sub>i</jats:sub>, i.e., the larger of the two scales. Possible explanations for these results are discussed, including Alfvén wave dispersion, damping, and current sheets.</jats:p> Ion‐scale spectral break of solar wind turbulence at high and low beta Geophysical Research Letters |
| spellingShingle | Chen, C. H. K., Leung, L., Boldyrev, S., Maruca, B. A., Bale, S. D., Geophysical Research Letters, Ion‐scale spectral break of solar wind turbulence at high and low beta, General Earth and Planetary Sciences, Geophysics |
| title | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_full | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_fullStr | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_full_unstemmed | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_short | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_sort | ion‐scale spectral break of solar wind turbulence at high and low beta |
| title_unstemmed | Ion‐scale spectral break of solar wind turbulence at high and low beta |
| topic | General Earth and Planetary Sciences, Geophysics |
| url | http://dx.doi.org/10.1002/2014gl062009 |