Identification of the dominant ULF wave mode and generation mechanism for obliquely propagating waves in the Earth's foreshock

Strumik, M.; Roytershteyn, V.; Karimabadi, H.; Stasiewicz, K.; Grzesiak, Marcin; Przepiórka, Dorota

doi:10.1002/2015gl064915

Cited by 9 publications

(23 citation statements)

References 41 publications

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“…The majority of the ULF waves are either Alfvénic (mostly transverse) or magnetosonic-whistler (mostly compressive). We should also note that observed wave properties have also been reproduced in FS numerical simulations (Blanco-Cano et al, 2006Omidi et al, 2002Omidi et al, , 2005Strumik et al, 2015) or in a global hybrid Vlasov code (Palmroth et al, 2015). We should also note that observed wave properties have also been reproduced in FS numerical simulations (Blanco-Cano et al, 2006Omidi et al, 2002Omidi et al, , 2005Strumik et al, 2015) or in a global hybrid Vlasov code (Palmroth et al, 2015).…”

Section: Introductionmentioning

confidence: 65%

“…Hoppe et al (1981) and Hoppe and Russell (1983) identified them as right-hand polarized in the plasma rest frame. The waves are referred either as almost sinusoidal structures or as more compressional and obliquely propagating waves (Hoppe & Russell, 1983) with an alternative interpretation that the oblique waves can represent a kinetic fast magnetosonic wave resulting from an ion/ion cyclotron right-hand resonant instability (Blanco-Cano & Schwartz, 1997;Gary et al, 1981;Gary, 1991Gary, , 1993Strumik et al, 2015). The waves are referred either as almost sinusoidal structures or as more compressional and obliquely propagating waves (Hoppe & Russell, 1983) with an alternative interpretation that the oblique waves can represent a kinetic fast magnetosonic wave resulting from an ion/ion cyclotron right-hand resonant instability (Blanco-Cano & Schwartz, 1997;Gary et al, 1981;Gary, 1991Gary, , 1993Strumik et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

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Solar Wind Proton Deceleration in Front of the Terrestrial Bow Shock

et al. 2019

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The terrestrial foreshock as a region permeated by different types of plasma waves, various particle populations, and strong wave activity is a subject of intensive investigations. Our statistical study of the solar wind proton velocity deceleration in the foreshock uses multipoint observations of the THEMIS mission and compare them with the Wind solar wind monitor with a motivation to estimate the factors influencing evolution/modification of the solar wind speed. In order to follow changes of the solar wind proton speed, our moment calculations do not include the reflected particles as well as heavier ions. We have found a systematic deceleration of the solar wind protons with a decreasing distance to the bow shock that is correlated with the flux of reflected and accelerated particles, with the level of magnetic field fluctuations in the ultralow frequency range, and with their compressibility. We can conclude that the reflected particles excite waves of large amplitudes and, as a consequence, modify median values of the velocity measured in an unperturbed solar wind. The deceleration is as high as 3% in front of the quasi‐parallel bow shock and decreases with the distance being observable up to 50 RE. We found similar effects in front of the Moon and attributed them to an influence of the solar wind ions reflected from the lunar surface.

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Section: Introductionmentioning

confidence: 65%

Section: Introductionmentioning

confidence: 99%

Solar Wind Proton Deceleration in Front of the Terrestrial Bow Shock

et al. 2019

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“…These instabilities can generate waves in the upstream region (e.g. Blanco-Cano et al 2011;Wang et al 2015;Strumik et al 2015), so that an increased level A&A 592, A118 (2016) of fluctuations is expected before and after the shocks associated with ICMEs.…”

Section: Introductionmentioning

confidence: 99%

Superposed epoch study of ICME sub-structures near Earth and their effects on Galactic cosmic rays

Masías-Meza

Dasso

Démoulin

et al. 2016

A&A

113

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Context. Interplanetary coronal mass ejections (ICMEs) are the interplanetary manifestations of solar eruptions. The overtaken solar wind forms a sheath of compressed plasma at the front of ICMEs. Magnetic clouds (MCs) are a subset of ICMEs with specific properties (e.g. the presence of a flux rope). When ICMEs pass near Earth, ground observations indicate that the flux of Galactic cosmic rays (GCRs) decreases. Aims. The main aims of this paper are to find common plasma and magnetic properties of different ICME sub-structures and which ICME properties affect the flux of GCRs near Earth. Methods. We used a superposed epoch method applied to a large set of ICMEs observed in situ by the spacecraft ACE, between 1998 and 2006. We also applied a superposed epoch analysis on GCRs time series observed with the McMurdo neutron monitors. Results. We find that slow MCs at 1 AU have on average more massive sheaths. We conclude that this is because they are more effectively slowed down by drag during their travel from the Sun. Slow MCs also have a more symmetric magnetic field and sheaths expanding similarly as their following MC, while in contrast, fast MCs have an asymmetric magnetic profile and a sheath in compression. In all types of MCs, we find that the proton density and the temperature and the magnetic fluctuations can diffuse within the front of the MC due to 3D reconnection. Finally, we derive a quantitative model that describes the decrease in cosmic rays as a function of the amount of magnetic fluctuations and field strength. Conclusions. The obtained typical profiles of sheath, MC and GCR properties corresponding to slow, middle, and fast ICMEs, can be used for forecasting or modelling these events, and to better understand the transport of energetic particles in ICMEs. They are also useful for improving future operative space weather activities.

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“…A determination of their polarization in the plasma frame is difficult because only single-point measurements are available. Taken into account the compressive nature of the observed waves (Figure 4i) and the propagation angle, we can probably attribute them to the kinetic fast magnetosonic waves (Strumik et al, 2015;Wilson, 2016).…”

Section: Wave Propertiesmentioning

confidence: 81%

“…As a result, ULF wave activity is not detected at the ion foreshock boundary but at another boundary located further downstream, identified as the ULF foreshock boundary (Greenstadt et al, 1980). The wave activity observed in these regions includes quasi-monochromatic waves and occasionally contains a broad spectrum of turbulent electromagnetic fluctuations (for details of wave properties see, e.g., the following papers: Thomsen (1985), Eastwood et al (2005), Narita et al (2006), Burgess et al (2012), Stasiewicz et al (2013), Selzer et al (2014), Strumik et al (2015), Wilson (2016)). Omidi et al (2005) and Blanco-Cano et al (2006) studied the morphology of the foreshock and characterized the nature of ULF waves using global 2-D hybrid simulations.…”

Section: Introductionmentioning

confidence: 99%

Solar Wind Deflection in the Foreshock: Model‐Data Comparison

et al. 2020

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We present the results of a 2.5‐D (2‐D in space and 3‐D in currents and electromagnetic fields) electromagnetic hybrid simulation run for foreshock wave activity during an interval of a radial interplanetary magnetic field (IMF). The simulation predicts nonlinear waves and foreshock expansion in connection with the development of cavitons and the formation of the foreshock compressional boundary. Fluctuations of the ion velocity VY component are associated with wave fronts corresponding to small wave normal angles and oscillate around 0 in the far upstream region. At distances closer to the bow shock, these fluctuations become asymmetric with duskward flow perturbations dominating at dusk and dawnward flow perturbations at dawn. We compare this simulation with THEMIS observations of large‐amplitude quasi‐monochromatic variations of ion velocity in the foreshock under radial IMF. A case study of simultaneous dual observations of unipolar VY fluctuations is followed by a statistical study of similar solar wind deflections in the foreshock. The observations that confirm the simulation predictions indicate that, in addition to ion heating, ultralow‐frequency waves participate in the magnetosheath‐like plasma flow deflection in the foreshock during periods of small IMF cone angles.

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Identification of the dominant ULF wave mode and generation mechanism for obliquely propagating waves in the Earth's foreshock

Cited by 9 publications

References 41 publications

Solar Wind Proton Deceleration in Front of the Terrestrial Bow Shock

Solar Wind Proton Deceleration in Front of the Terrestrial Bow Shock

Superposed epoch study of ICME sub-structures near Earth and their effects on Galactic cosmic rays

Solar Wind Deflection in the Foreshock: Model‐Data Comparison

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