Dependence of magnetic field parameters at the subsolar point of the magnetosphere on the interplanetary magnetic field according to the data of the THEMIS experiment

Pulinets, M. S.; Ryazantsev, M. O.; Антонова, Е. Е.; Kirpichev, I. P.

doi:10.1134/s0016793212060084

Cited by 13 publications

(3 citation statements)

References 20 publications

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“…Pulinets et al . [] showed that B y in front of the magnetopause can be enhanced around 6 to 7 times in comparison with the corresponding IMF B y . Considering all the processes that enhance the magnetic field in the magnetosheath, ratio of 5–16 of the IMF B y component and the magnetosheath B y component is reasonable; however, the B z enhancement in the magnetosheath can be even larger than B y enhancement in our study.…”

Section: Discussionmentioning

confidence: 99%

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Shue

Grygorov

et al. 2017

JGR Space Physics

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We use the Time History of Events and Macroscale Interactions during Substorms data to investigate the magnetic field structure just outside the magnetopause and its time evolution for radial interplanetary magnetic field (IMF) events. When the magnetic field drapes around the magnetopause in the magnetosheath region, an asymmetric magnetic field orientation in different hemispheres is expected. Our two‐case study reveals some conflicts with the predicted draped field configuration in the Southern Hemisphere. The magnetosheath Bz component had a different sign depending on the upstream IMF Bx component's polarity at the beginning of the radial IMF intervals. With time, the observed Bz became northward in both cases with increasing positive values through the events. The increasing value of the Bz component may be explained by two possible mechanisms: by a change of the upstream IMF and by a reconnection between magnetosheath and magnetospheric field lines. Our study shows that both mechanisms contributed to the observed changes. Thus, there was a correlation between the change of the upstream IMF conditions and an increase in the magnetosheath northward magnetic field component. The observed formation of the boundary layer near the magnetopause proves that the reconnection process was ongoing at least for a part of the time. We suggest two possible reconnection scenarios: one near subsolar point and another tailward of the one cusp due to lobe reconnection. The asymmetry of reconnection locations causes rearrangement of the magnetic field structure near the magnetopause and turns the observed magnetosheath Bz component even further into positive values.

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Section: Discussionmentioning

confidence: 99%

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Shue

Grygorov

et al. 2017

JGR Space Physics

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“…The interplanetary magnetic field (IMF) direction changes its direction also in this region. Pulinets et al (2012) compared the IMF direction in the SW near the BS and in the MSH close to the magnetopause and showed that the B Z component changes its sign in ≈ 30% of the cases. Šafránková et al (2009) studied a reliability of prediction of the magnetosheath B Z component from IMF observations and found that this probability is close to 0.5 (a random coincidence) for IMF |B Z | < 1 nT regardless of the solar cycle phase.…”

Section: Introductionmentioning

confidence: 98%

Modification of small- and middle-scale solar wind structures by the bow shock and magnetosheath: Correlation analysis

Rakhmanova

Рязанцева

Zastenker

et al. 2015

Planetary and Space Science

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“…Variations in the plasma and magnetic field parameters in the magneto sheath can reach considerable values and are observed in a wide range of time scales (Sibeck et al, 2000;Zas tenker, 2008). It was shown (Šafránkova et al, 2009;Pulinets et al, 2012Pulinets et al, , 2014) that the magnetic field direction near the magnetopause poorly correlates with this direction in the solar wind, including a sign reversal. Zastenker et al (2002) showed that an increase in the variation level in the solar wind is accompanied by an increase in the magnetosheath variation level.…”

Section: Introductionmentioning

confidence: 99%

Thickness of the low-latitude boundary layer at different levels of magnetic field fluctuations in the magnetosheath

et al. 2015

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Dependence of magnetic field parameters at the subsolar point of the magnetosphere on the interplanetary magnetic field according to the data of the THEMIS experiment

Cited by 13 publications

References 20 publications

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Modification of small- and middle-scale solar wind structures by the bow shock and magnetosheath: Correlation analysis

Thickness of the low-latitude boundary layer at different levels of magnetic field fluctuations in the magnetosheath

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