Modification of interplanetary shocks near the bow shock and through the magnetosheath

Šafránková, Jana; Němeček, Zdenek; Přech, Lubomír; Samsonov, A. A.; Koval, A.; Andréeová, K.

doi:10.1029/2007ja012503

Cited by 33 publications

(42 citation statements)

References 24 publications

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“…This rarefaction wave could result in outward bow shock motion. In MHD simulations, the bow shock begins moving earthward immediately after an encounter with an IP shock at velocities of ∼100 km s −1 (Samsonov et al, 2006). Results from a three-dimensional magnetosheath numerical model show that both a fast reverse shock and a fast expansion wave (rarefaction wave) may result from the interaction of the IP shock with the magnetopause depending on boundary conditions of the model (Samsonov et al, 2006).…”

Section: Introductionmentioning

confidence: 99%

“…The interaction of IP shocks with the bow shock has been extensively studied (e.g., Shen and Dryer, 1972;Grib et al, 1979;Zhuang et al, 1981;Samsonov et al, 2006Samsonov et al, , 2007Zhang et al, 2009). In MHD simulations, the interaction of an IP shock with the bow shock launches a fast shock into the magnetosheath and creates a new discontinuity (Zhuang et al, 1981) where the magnetic field strength and density increase, the temperature decreases and the velocity remains unchanged (Samsonov et al, 2006).…”

Section: Introductionmentioning

confidence: 99%

“…In MHD simulations, the bow shock begins moving earthward immediately after an encounter with an IP shock at velocities of ∼100 km s −1 (Samsonov et al, 2006). Results from a three-dimensional magnetosheath numerical model show that both a fast reverse shock and a fast expansion wave (rarefaction wave) may result from the interaction of the IP shock with the magnetopause depending on boundary conditions of the model (Samsonov et al, 2006). The existence of the rarefaction wave reflected from the magnetopause due to the shock-magnetopause interaction was confirmed by a case study employing observations made by Cluster spacecraft in the magnetosheath (Maynard et al, 2008).…”

Section: Introductionmentioning

confidence: 99%

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Global magnetospheric response to an interplanetary shock: THEMIS observations

et al. 2012

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Abstract. We investigate the global response of the geospace plasma environment to an interplanetary (IP) shock at ∼02:24 UT on 28 May 2008 from multiple THEMIS spacecraft observations in the magnetosheath (THEMIS B and C), the mid-afternoon magnetosphere (THEMIS A), and the dusk magnetosphere (THEMIS D and E). The interaction of the transmitted IP shock with the magnetosphere has global effects. Consequently, it can affect geospace plasma significantly. After interacting with the bow shock, the IP shock transmitted a fast shock and a discontinuity which propagated through the magnetosheath toward the Earth at speeds of 301 km s −1 and 137 km s −1 , respectively. THEMIS A observations indicate that the IP shock changed the properties of a plasmaspheric plume significantly. The plasmaspheric plume density increased rapidly from 10 to 100 cm −3 in 4 min and the ion distribution changed from an isotropic to a strongly anisotropic distribution. Electromagnetic ion cyclotron (EMIC) waves observed by THEMIS A are most likely excited by the anisotropic ion distributions caused by the IP shock impact. THEMIS A, but not D or E, observed a plasmaspheric plume in the dayside magnetosphere. Multiple spacecraft observations indicate that the dawn-side edge of the plasmaspheric plume was located between THEMIS A and D (or E).

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Global magnetospheric response to an interplanetary shock: THEMIS observations

et al. 2012

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“…The motion of the indentation can be recorded as two bow shock crossings separated by 1-5 min. Safrankova et al (2007) interpreted out-and inbound bow shock crossing pairs observed by Interball 1 and Geotail as the result of the passage of an interplanetary shock through the magnetosheath. Jelinek et al (2010) found several cases in THEMIS observations when the whole magnetosheath was swept along the probes in a few minutes due to the large displacement of the bow shock and the magnetopause as a result of their interaction with solar wind discontinuities.…”

Section: Discussionmentioning

confidence: 99%

“…The passage of the inbound transmitted shock causes the bow shock and the magnetopause to move inward, while the passage of the sunward-propagating reflected shock causes the boundaries to move out, as confirmed by Pallocchia et al (2010) based on observations aboard Double Star TC1 and Cluster 3. Safrankova et al (2007) suggested that the combination of the inward and outward motions of the bow shock, caused by the transition of an interplanetary shock, results in an indentation of the bow shock surface which flows along the bow shock together with the interplanetary shock. The motion of the indentation can be recorded as two bow shock crossings separated by 1-5 min.…”

Section: Discussionmentioning

confidence: 99%

Multispacecraft observations of the terrestrial bow shock and magnetopause during extreme solar wind disturbances

et al. 2012

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Abstract. Three events are discussed from the declining phase of the last solar cycle when the magnetopause and/or the bow shock were observed unusually close to the Earth due to major interplanetary disturbances. The observed extreme locations of the discontinuities are compared with the predictions of three magnetopause and four bow shock models which describe them in considerably different ways using statistical methods based on observations. A new 2-D magnetopause model is introduced (based on Verigin et al., 2009) which takes into account the pressure of the compressed magnetosheath field raised by the interplanetary magnetic field (IMF) component transverse to the solar wind flow. The observed magnetopause crossings could be predicted with a reasonable accuracy (0.1-0.2 R E ) by one of the presented models at least. For geosynchronous magnetopause crossings observed by the GOES satellites, (1) the new model provided the best predictions when the IMF was extremely large having a large negative B z component, and (2)

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Sudden impulse observations in the dayside magnetosphere by THEMIS

et al. 2014

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We present a study of the magnetospheric response to interplanetary shocks. We show eight events with simultaneous observations of sudden impulses in the dayside magnetosphere and interplanetary shocks in the solar wind. The spacecraft measurements in the equatorial plane, even those very close to the Earth, can be interpreted in terms of the vortices predicted by previous studies employing global MHD models. In fact, these vortices are velocity oscillations with the properties of Alfvén waves. The amplitude and frequency of the oscillations depend on radial distance from the Earth. The amplitude of the velocity perturbations decreases with increase of the density and magnetic field magnitude, but the velocity amplitude shows no dependence on magnitude of the solar wind dynamic pressure change attending the interplanetary shocks. The oscillations are observed both in the outer magnetosphere and the plasmasphere, but they become less sinusoidal near the plasmapause, i.e., in the region with a large-density gradient. The amplitude of the magnetic field enhancement in the sudden impulses also depends on the radial distance. The MHD simulations successfully predict the amplitudes of magnetic field increase and the first cycles of the velocity oscillations in these events.

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Modification of interplanetary shocks near the bow shock and through the magnetosheath

Cited by 33 publications

References 24 publications

Global magnetospheric response to an interplanetary shock: THEMIS observations

Global magnetospheric response to an interplanetary shock: THEMIS observations

Multispacecraft observations of the terrestrial bow shock and magnetopause during extreme solar wind disturbances

Sudden impulse observations in the dayside magnetosphere by THEMIS

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