This paper, using the dataset of BBFs （bursty bulk flows） observed by two Cluster satellites C1 and C4, studies the difference between onset times of BBFs observed by C1 and C4. It is found that the onset time diffe...This paper, using the dataset of BBFs （bursty bulk flows） observed by two Cluster satellites C1 and C4, studies the difference between onset times of BBFs observed by C1 and C4. It is found that the onset time differences of most of BBFs observed by Cl and C4 are smaller than 60 s. The average onset time difference of BBFs of CI and C4 is 68.5 s. The probabilities of onset time difference of BBFs of C1 and C4 larger than 30, 60, 90 and 120 s are respectively 55%, 35%, 27% and 23%. The largest onset time difference of BBFs of C1 and C4 decreases with the increase of earthward component of maximum velocities of BBFs. The onset time difference of BBFs of C1 and C4 results from the velocity inhomogeneity inside the flow channel of BBF, which may be produced in propagation path and/or in source region of BBFs. Such a wide range of onset time difference of BBFs suggests that the velocity inhomogeneity inside the flow channel of BBF is various. These results are very important to the current study of substorm research based on THEMIS data because they indicate that it is impossible to determine the onset time of BBF with a single satellite.展开更多
In August 2001,Cluster satellites observed that the mid-tail current sheet(CS) moved southward continuously for almost seven hours.Meanwhile,Cluster crossed back and forth the CS repeatedly.This means that the large-s...In August 2001,Cluster satellites observed that the mid-tail current sheet(CS) moved southward continuously for almost seven hours.Meanwhile,Cluster crossed back and forth the CS repeatedly.This means that the large-scale southward movement of the CS was accompanied by a small-scale CS flapping during this period.Using the minimum-variation-analysis(MVA) method and the multi-spacecraft data,we calculated the normal vector,current density and the magnetic curvature of the CS,the results showed that the CS alternated between flattened CS and tilted CS for several times.Strong dawn-dusk oscillations were found for the tilted CS,which caused the repeated crossings of the center of CS by the satellites.This feature is obviously different from the previous observations of the vertical flapping of the CS induced by the kink instability.Two types of flapping were observed:One of them is accompanied with bursty bulk flows(BBFs) and the other is not.This suggests that in this event there was no direct relationship between the CS flapping and BBFs.展开更多
Bursty Bulk Flows(BBF) events are an important phenomenon of plasma transport in the Earth’s magneto tail during substorms, and can be explained by the bubbles model. Although the theories and observations have provi...Bursty Bulk Flows(BBF) events are an important phenomenon of plasma transport in the Earth’s magneto tail during substorms, and can be explained by the bubbles model. Although the theories and observations have provided some estimates of the important parameters of BBFs, such as the cross tail size, these parameters are still an extent instead of accurate value. Based on the latest Tsyganenko magnetospheric model, we provide the cross tail size of BBFs in the magnetic equatorial plane through the north south aligned auroral structures and tracer program. The results show that the predications of the bubbles model agree with the observed facts.展开更多
基金supported by the National Natural Science Foundation of China (Grant Nos. 40931054 and 41174141)National Basic Research Program of China ("973" Program) (Grant No. 2011CB811404)
文摘This paper, using the dataset of BBFs （bursty bulk flows） observed by two Cluster satellites C1 and C4, studies the difference between onset times of BBFs observed by C1 and C4. It is found that the onset time differences of most of BBFs observed by Cl and C4 are smaller than 60 s. The average onset time difference of BBFs of CI and C4 is 68.5 s. The probabilities of onset time difference of BBFs of C1 and C4 larger than 30, 60, 90 and 120 s are respectively 55%, 35%, 27% and 23%. The largest onset time difference of BBFs of C1 and C4 decreases with the increase of earthward component of maximum velocities of BBFs. The onset time difference of BBFs of C1 and C4 results from the velocity inhomogeneity inside the flow channel of BBF, which may be produced in propagation path and/or in source region of BBFs. Such a wide range of onset time difference of BBFs suggests that the velocity inhomogeneity inside the flow channel of BBF is various. These results are very important to the current study of substorm research based on THEMIS data because they indicate that it is impossible to determine the onset time of BBF with a single satellite.
基金supported by the National Natural Science Foundation of China (Grant Nos. NSFC40931054,41174141 and 41174144)the National Basic Research Program of China ("973" Project) (Grant No.2011CB811404)
文摘In August 2001,Cluster satellites observed that the mid-tail current sheet(CS) moved southward continuously for almost seven hours.Meanwhile,Cluster crossed back and forth the CS repeatedly.This means that the large-scale southward movement of the CS was accompanied by a small-scale CS flapping during this period.Using the minimum-variation-analysis(MVA) method and the multi-spacecraft data,we calculated the normal vector,current density and the magnetic curvature of the CS,the results showed that the CS alternated between flattened CS and tilted CS for several times.Strong dawn-dusk oscillations were found for the tilted CS,which caused the repeated crossings of the center of CS by the satellites.This feature is obviously different from the previous observations of the vertical flapping of the CS induced by the kink instability.Two types of flapping were observed:One of them is accompanied with bursty bulk flows(BBFs) and the other is not.This suggests that in this event there was no direct relationship between the CS flapping and BBFs.
文摘Bursty Bulk Flows(BBF) events are an important phenomenon of plasma transport in the Earth’s magneto tail during substorms, and can be explained by the bubbles model. Although the theories and observations have provided some estimates of the important parameters of BBFs, such as the cross tail size, these parameters are still an extent instead of accurate value. Based on the latest Tsyganenko magnetospheric model, we provide the cross tail size of BBFs in the magnetic equatorial plane through the north south aligned auroral structures and tracer program. The results show that the predications of the bubbles model agree with the observed facts.
