Substorm associated traveling compression regions in the distant tail: Isee‐3 Geotail observations

Slavin, J. A.; Smith, E. J.; Tsurutani, B. T.; Sibeck, D. G.; Singer, H. J.; Baker, D. N.; Gosling, J. T.; Hones, E. W.; Scarf, F. L.

doi:10.1029/gl011i007p00657

Cited by 195 publications

(132 citation statements)

References 5 publications

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“…Unfortunately, P2 data experienced a loss in the transmission from a ground station to the operations center, but we can use P1 observations for distant tail signatures and P3, P4, P5 data for investigations of corresponding near-Earth structures. During the first event at about 0200 UT, the operating THEMIS spacecraft were located as shown in Figure 11 and Table 1. [21] At 0200:05 UT P1 observes a TCR-like signature, [e.g., Slavin et al, 1984Slavin et al, , 2005 and P3 and P4 observe dipolarization at 0158:11 UT and 0159:26 UT, respectively (see Figures 12, 13, and 14). Dipolarization observed by P3 Figure 9.…”

Section: Event On 2 February 2008 $0200 Utmentioning

confidence: 99%

First application of a Petschek‐type reconnection model with time‐varying reconnection rate to THEMIS observations

et al. 2009

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[1] We present a method to determine the location of the reconnection site and the amount of reconnected magnetic flux out of an analytical time-dependent reconnection model and apply this method to disturbances observed on 2 February 2008 at about 0200 and 0815 UT by THEMIS B (P1). During these events, P1 detected two tailward propagating traveling compression regions, associated with typical variations in B z and B x . We find the reconnection site to be located at about À16 R E for the event at 0200 UT and À17.5 R E for the event at 0815 UT. These locations are consistent with simple timing considerations with respect to disturbances detected by the inner THEMIS spacecraft. The amount of reconnected flux in our 2-D model can be found to be in the order of 10 8 nT m for both events. The calculations for the reconnection site's location are done by using two approaches, i.e., by using the B z and the B x signals, yielding consistent results. The reconnected flux can be determined using B z and v z . Also, these results are in good agreement. A comparison between the disturbances detected by P1 and the modeled variations shows that our model describes disturbances in the magnetic field and the background plasma very well.

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Section: Event On 2 February 2008 $0200 Utmentioning

confidence: 99%

First application of a Petschek‐type reconnection model with time‐varying reconnection rate to THEMIS observations

et al. 2009

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“…Usually they are interpreted (see, e.g., Lin et al 2007) in terms of magnetic islands produced as the result of the tearingmode instability (Furth et al 1963), or invoking time-dependent Petschek-type reconnection (see, e.g., Priest & Forbes 2000). These interpretations establish a link between solar and magnetospheric reconnection: blobs should be identified with plasmoids, which are known to form in the terrestrial magnetosphere (Hones 1985) and which have been first discovered in the ISEE data by Hones et al (1984) and Slavin et al (1984), and have been described in terms of magnetic islands in the CS. Recently, observations from the CLUSTER spacecraft confirmed this magnetic island structure and led to an interpretation in terms of multiple X-line reconnection (e.g., Slavin et al 2003Slavin et al , 2005Eastwood et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Uv Transient Brightenings Associated With a Coronal Mass Ejection

Schettino¹,

Poletto²,

Romoli³

2009

ApJ

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In this paper, we analyze transient UV brightenings in spectra acquired by SOHO/UltraViolet Coronagraph Spectrometer (UVCS) on 2003 June 2 in association with a coronal mass ejection (CME) that occurred at the West limb of the Sun at 08:54 UT. Brightenings have been observed in lines from cool (C iii, O vi), intermediate (Si viii, Si xii), and high ([Fe xviii]) temperature ions over about 7 hr from the CME. Brightenings in cool lines are interpreted in terms of mini-ejections that appear at the time of, and after, the passage of the CME front through the UVCS slit. We give here their temperature and density and we point out that, assuming a spherical shape, a few of these mini-CMEs can provide a mass comparable to that quoted for typical CMEs. Hot lines, like the [Fe xviii] line at 974.9 Å which shows up in the CME associated current sheet (CS), undergo transient brightness as well, but hot lines brightenings are more difficult to interpret. We propose here a scenario where they are signatures of the passage through the UVCS slit of plasmoids similar to those observed in the filamentary CS of the magnetotail that form as a consequence of the tearing-mode instability or of a time-dependent Petschek-type reconnection.

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“…Traveling compression regions (TCRs) are the lobe signature of a passing plasmoid [e.g., Slavin et al, 1984Slavin et al, , 1994Moldwin and Hughes, 1994]. They are formed due to the compression of the magnetotail lobe against the magnetosheath pressure by the vertical (north-south) extent of a plasmoid [Slavin et al, 1994].…”

Section: Introductionmentioning

confidence: 99%

On the origin of reverse polarity TCRs

Moldwin¹,

Collier²,

Slavin³

et al. 2001

Geophysical Research Letters

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Abstract.Reverse polarity, or South-then-North (SN) bipolar, traveling compression regions (SN TCRs) are often observed in the Earth's magnetotail lobes. These events have been interpreted as either slowly earthward propagating "proto-plasmoids" during extremely quiet geomagnetic conditions, or due to pressure pulses in the solar wind or magnetosheath compressing the magnetotail. This study presents a survey of 21 IMP 8 observations of SN TCRs and the corresponding solar wind pressure conditions as measured by WIND. We found that solar wind or magnetosheath pressure pulses nicely explain most (17), though not all, of the SN TCR observations. Therefore, it appears that both explanations previously given are needed to explain SN TCRs. We also found that most of these events occurred during northward Interplanetary Magnetic Field (IMF) conditions. This suggests that the magnetotail may respond differently to solar wind dynamic pressure pulses for different orientations of the IMF.

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Substorm associated traveling compression regions in the distant tail: Isee‐3 Geotail observations

Cited by 195 publications

References 5 publications

First application of a Petschek‐type reconnection model with time‐varying reconnection rate to THEMIS observations

First application of a Petschek‐type reconnection model with time‐varying reconnection rate to THEMIS observations

Uv Transient Brightenings Associated With a Coronal Mass Ejection

On the origin of reverse polarity TCRs

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