Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence
| Publication Date: |
2018-01-04
|
|---|---|
| Publisher: |
Wiley-Blackwell
|
| Print ISSN: |
0148-0227
|
| Topics: |
Geosciences
Physics
|
| Published by: |
| _version_ | 1836398730216996864 |
|---|---|
| autor | X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang |
| beschreibung | The spectral break ( f b ) of magnetic fluctuations at the ion scale in the solar wind is considered to give important clue on the turbulence dissipation mechanism. Among several possible mechanisms, the most notable two are related respectively to proton thermal gyro-radius ρ i and proton inertial length d i . The corresponding frequencies of them are f ρ i = V S W /(2 π ρ i ) and f d i = V S W /(2 π d i ), respectively, where V S W is the solar wind speed. However, no definite conclusion has been given for which one is more reasonable because the two parameters have similar value when plasma beta β ∼ 1. Here, we do a statistical study to see if the two ratios f b / f ρ i and f b / f d i have different dependence on β in the solar wind turbulence with 0.1 〈 β 〈 1.3. From magnetic measurements by the WIND spacecraft, we select 141 data sets with each one longer than 13 hours. We find that the ratio f b / f d i is statistically not dependent on β , and the average value of it is 0.48 ± 0.06. However, f b / f ρ i increases with increasing β clearly, and is significantly smaller than f b / f d i when β 〈 0.8. These new results show that f b is statistically 0.48 f d i , and the influence of β could be negligible in the studied β range. It indicates a preference of the dissipation mechanism associated with d i in the solar wind with 0.1 〈 β 〈 0.8. Further theoretical studies are needed to give detailed explanation. |
| citation_standardnr | 6128921 |
| datenlieferant | ipn_articles |
| feed_copyright | American Geophysical Union (AGU) |
| feed_copyright_url | http://www.agu.org/ |
| feed_id | 7531 |
| feed_publisher | Wiley-Blackwell |
| feed_publisher_url | http://www.wiley.com/wiley-blackwell |
| insertion_date | 2018-01-04 |
| journalissn | 0148-0227 |
| publikationsjahr_anzeige | 2018 |
| publikationsjahr_facette | 2018 |
| publikationsjahr_intervall | 7984:2015-2019 |
| publikationsjahr_sort | 2018 |
| publisher | Wiley-Blackwell |
| quelle | Journal of Geophysical Research JGR - Space Physics |
| relation | http://onlinelibrary.wiley.com/resolve/doi?DOI=10.1002%2F2017JA024813 |
| search_space | articles |
| shingle_author_1 | X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang |
| shingle_author_2 | X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang |
| shingle_author_3 | X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang |
| shingle_author_4 | X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang |
| shingle_catch_all_1 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence The spectral break ( f b ) of magnetic fluctuations at the ion scale in the solar wind is considered to give important clue on the turbulence dissipation mechanism. Among several possible mechanisms, the most notable two are related respectively to proton thermal gyro-radius ρ i and proton inertial length d i . The corresponding frequencies of them are f ρ i = V S W /(2 π ρ i ) and f d i = V S W /(2 π d i ), respectively, where V S W is the solar wind speed. However, no definite conclusion has been given for which one is more reasonable because the two parameters have similar value when plasma beta β ∼ 1. Here, we do a statistical study to see if the two ratios f b / f ρ i and f b / f d i have different dependence on β in the solar wind turbulence with 0.1 < β < 1.3. From magnetic measurements by the WIND spacecraft, we select 141 data sets with each one longer than 13 hours. We find that the ratio f b / f d i is statistically not dependent on β , and the average value of it is 0.48 ± 0.06. However, f b / f ρ i increases with increasing β clearly, and is significantly smaller than f b / f d i when β < 0.8. These new results show that f b is statistically 0.48 f d i , and the influence of β could be negligible in the studied β range. It indicates a preference of the dissipation mechanism associated with d i in the solar wind with 0.1 < β < 0.8. Further theoretical studies are needed to give detailed explanation. X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang Wiley-Blackwell 0148-0227 01480227 |
| shingle_catch_all_2 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence The spectral break ( f b ) of magnetic fluctuations at the ion scale in the solar wind is considered to give important clue on the turbulence dissipation mechanism. Among several possible mechanisms, the most notable two are related respectively to proton thermal gyro-radius ρ i and proton inertial length d i . The corresponding frequencies of them are f ρ i = V S W /(2 π ρ i ) and f d i = V S W /(2 π d i ), respectively, where V S W is the solar wind speed. However, no definite conclusion has been given for which one is more reasonable because the two parameters have similar value when plasma beta β ∼ 1. Here, we do a statistical study to see if the two ratios f b / f ρ i and f b / f d i have different dependence on β in the solar wind turbulence with 0.1 < β < 1.3. From magnetic measurements by the WIND spacecraft, we select 141 data sets with each one longer than 13 hours. We find that the ratio f b / f d i is statistically not dependent on β , and the average value of it is 0.48 ± 0.06. However, f b / f ρ i increases with increasing β clearly, and is significantly smaller than f b / f d i when β < 0.8. These new results show that f b is statistically 0.48 f d i , and the influence of β could be negligible in the studied β range. It indicates a preference of the dissipation mechanism associated with d i in the solar wind with 0.1 < β < 0.8. Further theoretical studies are needed to give detailed explanation. X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang Wiley-Blackwell 0148-0227 01480227 |
| shingle_catch_all_3 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence The spectral break ( f b ) of magnetic fluctuations at the ion scale in the solar wind is considered to give important clue on the turbulence dissipation mechanism. Among several possible mechanisms, the most notable two are related respectively to proton thermal gyro-radius ρ i and proton inertial length d i . The corresponding frequencies of them are f ρ i = V S W /(2 π ρ i ) and f d i = V S W /(2 π d i ), respectively, where V S W is the solar wind speed. However, no definite conclusion has been given for which one is more reasonable because the two parameters have similar value when plasma beta β ∼ 1. Here, we do a statistical study to see if the two ratios f b / f ρ i and f b / f d i have different dependence on β in the solar wind turbulence with 0.1 < β < 1.3. From magnetic measurements by the WIND spacecraft, we select 141 data sets with each one longer than 13 hours. We find that the ratio f b / f d i is statistically not dependent on β , and the average value of it is 0.48 ± 0.06. However, f b / f ρ i increases with increasing β clearly, and is significantly smaller than f b / f d i when β < 0.8. These new results show that f b is statistically 0.48 f d i , and the influence of β could be negligible in the studied β range. It indicates a preference of the dissipation mechanism associated with d i in the solar wind with 0.1 < β < 0.8. Further theoretical studies are needed to give detailed explanation. X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang Wiley-Blackwell 0148-0227 01480227 |
| shingle_catch_all_4 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence The spectral break ( f b ) of magnetic fluctuations at the ion scale in the solar wind is considered to give important clue on the turbulence dissipation mechanism. Among several possible mechanisms, the most notable two are related respectively to proton thermal gyro-radius ρ i and proton inertial length d i . The corresponding frequencies of them are f ρ i = V S W /(2 π ρ i ) and f d i = V S W /(2 π d i ), respectively, where V S W is the solar wind speed. However, no definite conclusion has been given for which one is more reasonable because the two parameters have similar value when plasma beta β ∼ 1. Here, we do a statistical study to see if the two ratios f b / f ρ i and f b / f d i have different dependence on β in the solar wind turbulence with 0.1 < β < 1.3. From magnetic measurements by the WIND spacecraft, we select 141 data sets with each one longer than 13 hours. We find that the ratio f b / f d i is statistically not dependent on β , and the average value of it is 0.48 ± 0.06. However, f b / f ρ i increases with increasing β clearly, and is significantly smaller than f b / f d i when β < 0.8. These new results show that f b is statistically 0.48 f d i , and the influence of β could be negligible in the studied β range. It indicates a preference of the dissipation mechanism associated with d i in the solar wind with 0.1 < β < 0.8. Further theoretical studies are needed to give detailed explanation. X. Wang, C.-Y. Tu, J.-S. He, L.-H. Wang Wiley-Blackwell 0148-0227 01480227 |
| shingle_title_1 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| shingle_title_2 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| shingle_title_3 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| shingle_title_4 | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| timestamp | 2025-06-30T23:31:43.536Z |
| titel | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| titel_suche | Ion-scale spectral break in the normal plasma beta range in the solar wind turbulence |
| topic | TE-TZ U |
| uid | ipn_articles_6128921 |