Magnetopause ripples going against the flow form azimuthally stationary surface waves

Archer, Martin; Hartinger, M.; Plaschke, Ferdinand; Southwood, D. J.; Rastäetter, L.

doi:10.1038/s41467-021-25923-7

Cited by 21 publications

(27 citation statements)

References 79 publications

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“…The phase of the compressional magnetic field reverses either side of the boundary, that is, when the magnetosphere is compressed the magnetosheath becomes rarefied. Archer et al (2021), A21 herein, found similar motion of the subsolar bow shock, lagging behind the magnetopause. While the magnetopause waves travel tailward at the equatorial flanks, between 09 and 15 hr Magnetic Local Time (MLT) they are stationary despite significant magnetosheath flows being present.…”

Section: Surface Modessupporting

confidence: 61%

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How a Realistic Magnetosphere Alters the Polarizations of Surface, Fast Magnetosonic, and Alfvén Waves

et al. 2022

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System-scale magnetohydrodynamic (MHD) waves in Earth's magnetosphere are routinely observed by spacecraft and ground-based instrumentation as ultra-low frequency (ULF) waves, with frequencies of fractions of mil-liHertz to a few Hertz (Jacobs et al., 1964). These waves provide a means for solar wind energy and momentum to be transferred throughout geospace, for example, to the radiation belts (Elkington, 2006). They can also, through understanding the various normal modes they may establish, be used as a tool for probing the ever-changing nature of the terrestrial system (Menk & Waters, 2013). The foundations of MHD wave theory have largely been built in so-called box models, where the curved geomagnetic field lines are straightened into a uniform field anchored at the northern and southern ionospheres due to their high conductivity as shown in Figure 1a (e.g., Radoski, 1971;Southwood, 1974). While such analytic models have proven extremely useful, they are of course highly simplified compared to reality, thus it is important to understand their limitations. Numerical modeling of MHD waves can help in this regard and there are a number of different approaches which may be taken, from dedicated wave codes (e.g.,

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Section: Surface Modessupporting

confidence: 61%

“…Archer et al. ( 2021 ), A21 herein, found similar motion of the subsolar bow shock, lagging behind the magnetopause. While the magnetopause waves travel tailward at the equatorial flanks, between 09 and 15 hr Magnetic Local Time (MLT) they are stationary despite significant magnetosheath flows being present.…”

Section: Introductionmentioning

confidence: 54%

How a Realistic Magnetosphere Alters the Polarizations of Surface, Fast Magnetosonic, and Alfvén Waves

et al. 2022

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“…It has been shown that jets appear more frequently behind the Qpar shock rather than the Qperp one (Raptis, Aminalragia‐Giamini, et al., 2020; Raptis, Karlsson, et al., 2020; Vuorinen et al., 2019), and typically have significant effects on the geomagnetic environment of Earth (Plaschke et al., 2018). For example, they can enhance or initiate magnetopause reconnection (Escoubet et al., 2020; Hietala et al., 2018; Ng et al., 2021; Vuorinen et al., 2021), accelerate particles (Liu et al., 2019, 2020), generate a variety of different waves in the MSH and outer magnetosphere environment (Archer et al., 2019, 2021; Katsavrias et al., 2021) and even have effects on the inner magnetosphere and ionosphere (Hietala et al., 2012; Norenius et al., 2021; Wang et al., 2018).…”

Section: Introductionmentioning

confidence: 99%

“…outer magnetosphere environment (Archer et al, 2019(Archer et al, , 2021Katsavrias et al, 2021) and even have effects on the inner magnetosphere and ionosphere (Hietala et al, 2012;Norenius et al, 2021;Wang et al, 2018).…”

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confidence: 99%

On Magnetosheath Jet Kinetic Structure and Plasma Properties

Raptis

Karlsson

Vaivads

et al. 2022

Geophysical Research Letters

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As the supersonic solar wind (SW) approaches Earth, it interacts with the planet's magnetic field, forming a bow shock. Downstream of the shock, the magnetosheath (MSH) region forms, which is a highly turbulent plasma environment where several phenomena co-exist. One of these phenomena is the so called MSH jets and during the last two decades, they have drawn considerable attention (Plaschke et al., 2018). These jets are transient dynamic pressure enhancement with respect to the downstream ambient background plasma. The dynamic pressure enhancements can be due to either a velocity and/or density increase (Archer et al., 2012).One of the most important features that determines the properties of jets is whether they are found in the so called Quasi-parallel (Qpar) or Quasi-perpendicular (Qperp) MSH. These regions are, respectively, the plasma downstream of a Qpar or a Qperp shock crossing. Typically, the distinction between Qpar and Qperp shock crossings is based on the angle between the upstream Interplanetary Magnetic Field vector and the bow shock normal vector. If the angle is less than 45°, we call the crossing Qpar, while if it is greater, we call it Qperp. The downstream MSH of the Qpar shocks is more turbulent, exhibits lower temperature anisotropy, and contains more high-energy particles (Fuselier, 1994;Karlsson et al., 2021;. The complexity of Qpar shocks also extends upstream of the shock to the foreshock region where non-linear ULF waves, field-aligned beams and wave-particle interaction regions are observed (

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“…ULF waves in the magnetosphere are studied using coupled global magnetospheric models (e.g., Claudepierre et al, 2008;Hartinger et al, 2014;Claudepierre et al, 2016;Komar et al, 2017) and in simplified field geometries to isolate and better understand underlying physics (Xia et al, 2017;Denton, 2018;Elsden and Wright, 2020;Lysak et al, 2020). Examples of simulations of ULF waves in the magnetosphere presented at GEM UMEA sessions include studies of: global magnetospheric ULF wave modes (Claudepierre et al, 2010;Elsden et al, 2016;Wright, 2017, 2020;Xia et al, 2017;Lysak et al, 2020), magnetospheric ULF wave propagation (Degeling et al, 2018), growth and propagation of EMIC waves (Denton et al, 2014), magnetopause surface waves (Lin et al, 2017;Archer et al, 2021), and interaction of ULF waves with ring current and radiation belt particle populations (Komar et al, 2017;Denton et al, 2019;Patel et al, 2019).…”

Section: Ulf Wave Modeling and The Gem Ulf Wave Modeling Challengementioning

confidence: 99%

ULF Wave Modeling, Effects, and Applications: Accomplishments, Recent Advances, and Future

Hartinger

Takahashi

Drozdov

et al. 2022

Front. Astron. Space Sci.

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Ultra Low Frequency (ULF) waves play important roles in magnetosphere-ionosphere coupling, ring current and radiation belt dynamics, and modulation of higher frequency wave modes and energetic particle precipitation. The “ULF wave modeling, effects, and applications” (UMEA) focus group - part of the Geospace Environment Modeling effort from 2016 to 2021 - sought to improve understanding of the physics of ULF waves and their specification in geospace models. Through a series of in person and virtual meetings the UMEA focus group brought modelers and experimentalists together to compare ULF wave outputs in different models, plan observation campaigns focused on ULF waves, discuss recent advances in ULF wave research, and identify unresolved ULF wave science questions. This article summarizes major discussion points and accomplishments in the UMEA focus group over the last 6 years, recent advances and their connection to Richard Thorne and Peter Gary’s significant contributions to ULF wave research, and the future of ULF wave research.

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Magnetopause ripples going against the flow form azimuthally stationary surface waves

Cited by 21 publications

References 79 publications

How a Realistic Magnetosphere Alters the Polarizations of Surface, Fast Magnetosonic, and Alfvén Waves

How a Realistic Magnetosphere Alters the Polarizations of Surface, Fast Magnetosonic, and Alfvén Waves

On Magnetosheath Jet Kinetic Structure and Plasma Properties

ULF Wave Modeling, Effects, and Applications: Accomplishments, Recent Advances, and Future

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