Evidence of MLT propagation of the plasmapause inferred from THEMIS data

Bandić, Mario; Verbanac, Giuliana; Pierrard, Viviane; Cho, Junghee

doi:10.1016/j.jastp.2017.05.005

Cited by 14 publications

(32 citation statements)

References 36 publications

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“…This exactly reflects the T lag belt around the maximal T lag of 9 h. If we suppose that the plasmapause is transmitted with ω IM = 1, then we expect T lag s around 13 h or around 3 h depending if the formation was triggered at 21 MLT or at 07 MLT. Taking further into account that the deformation likely comprises a few MLTs simultaneously (Bandić et al, ; Goldstein, Burch, et al, ; Pierrard & Lemaire, ), for instance, 3 MLTs, the observed T lag can be even less than 3 h. A wider belt of T lag s with values between 0 and 16 h is therefore expected. In each MLT sector, the widths of the T lag belts are calculated as explained above and are indicated by red circles and black crosses in Figures and .…”

Section: Mlt Dependence Of the Simulated Plasmapausementioning

confidence: 93%

“…To examine the meaning of the T lag belts, let us consider the 10–11 MLT sector. The determined T lag is 9 h. As pointed out above it is possible that the plasmapause is also formed after 05 MLT, for example, at 06 MLT as obtained when Weimer E field model is used (Pierrard et al, ) or at 07 MLT obtained from past THEMIS e L PP analyses (Bandić et al, ). Let us suppose now that plasmapause is formed somewhere between 21 MLT and 07 MLT.…”

Section: Mlt Dependence Of the Simulated Plasmapausementioning

confidence: 93%

“…We used the same 6,840 e L PP s as in Bandić et al (), which are obtained from measurements of the electric field instrument (EFI) and the electrostatic analyzer (ESA) on board THEMIS A, D, and E satellites. They define the plasmapause as the innermost sharp density gradient (d n /d r where n is density and r is radial distance) of at least a factor of 15 within a radial distance of 0.5 R E .…”

Section: Methodsmentioning

confidence: 99%

“…As in Bandić et al (), to investigate the propagation of the plasmapause we use here the mean angular velocity defined as

ω_{IM} = \frac{Δ T_{resolution}}{Δ T_{lag}} \frac{[h]}{[h]}

where Δ T resolution is the interval length of the MLT bin and Δ T lag is the difference between the T lag of the analyzed MLT bin and of the previous MLT bin. Since data are binned in 1 h MLT bins (00–01 MLT, 02–03 MLT, …, 23–24 MLT) the Δ T resolution is 1 h. The ω IM is expressed as a fraction of the Earth's angular rotation speed.…”

Section: Methodsmentioning

confidence: 99%

“…The MLT propagation effects and other plasmapause characteristics inferred from THEMIS‐based e L PP s are presented in Bandić et al (). Here we show and discuss the behavior of the CC curves (presented in Figures and , last column) and compare them with those obtained from the simulations (first column or first two columns for sectors 02–05 MLTs in Figures and ).…”

Section: Mlt Dependence Of Themis‐based Plasmapause and Comparison Wimentioning

confidence: 99%

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MLT Plasmapause Characteristics: Comparison Between THEMIS Observations and Numerical Simulations

Verbanac

Bandić²,

Pierrard

et al. 2018

JGR Space Physics

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We perform a statistical comparison of the global behavior of the THEMIS observed and simulated plasmapause in the geomagnetic equatorial plane. Simulation is based on the interchange instability mechanism. Analyzing plasmapause positions (LPPs) from the period July 2008 to December 2012, we derived formation and propagation characteristics of the main plasmapause, which reflect the most probable global plasmapause behavior. The results suggest a global eastward azimuthal plasmapause propagation and a radial plasmapause motion limited to the 21–07 MLT sector. The formation of the plasmapause takes place with the highest probability at postmidnight. It is likely that the erosion occurs in a range of MLTs simultaneously. On the dayside, the plasmapause moves almost entirely azimuthally. We suggest that the plasmapause propagates azimuthally with a mean angular velocity close to the corotation speed at all MLTs, at least during periods of lower geomagnetic activity. The results also show that the experimental plasmapause characteristics are in accordance with the interchange instability mechanism. Along with the proposed suggestions for future works, this study contributes to making a further step toward resolving some of the long‐lasting, unresolved issues related to plasmapause dynamics.

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Section: Mlt Dependence Of the Simulated Plasmapausementioning

confidence: 93%

Section: Mlt Dependence Of the Simulated Plasmapausementioning

confidence: 93%

Section: Methodsmentioning

confidence: 99%

“…As in Bandić et al (), to investigate the propagation of the plasmapause we use here the mean angular velocity defined as

ω_{IM} = \frac{Δ T_{resolution}}{Δ T_{lag}} \frac{[h]}{[h]}

Section: Methodsmentioning

confidence: 99%

Section: Mlt Dependence Of Themis‐based Plasmapause and Comparison Wimentioning

confidence: 99%

See 3 more Smart Citations

MLT Plasmapause Characteristics: Comparison Between THEMIS Observations and Numerical Simulations

Verbanac

Bandić²,

Pierrard

et al. 2018

JGR Space Physics

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Experimental Study of the Plasmasphere Boundary Layer Using MAGION 5 Data

et al. 2018

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The in situ cold plasma measurements onboard MAGION 5 were carried out with very good time resolution, and this permitted to analyze thin plasmasphere boundary layer (PBL) near the plasmapause. In this layer the plasma density N is decreasing exponentially with L: N~exp((LPP − L)/WB), where WB corresponds to the characteristic width of the PBL, the distance in L within which the density varies by a factor of e, and LPP is the position of the plasmapause. The density in the boundary layer is inversely proportional to the volume of the unit magnetic flux tube, whereas its width is proportional to the volume of magnetic flux tube. The characteristic width of the PBL linearly depends on the time elapsed since the most recent maximum value of KP. Empirical relation for the dependence of the PBL width on most recent maximum value of KP and on the lapse time between this maximum and the plasmapause observations is proposed.

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