Causes of Jets in the Quasi‐Perpendicular Magnetosheath

Kajdič, Primož; Raptis, Savvas; Blanco‐Cano, X.; Karlsson, Tomas

doi:10.1029/2021gl093173

Cited by 19 publications

(24 citation statements)

References 60 publications

(106 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, the traces of HSJs moving in the magnetosheath are the filamentary structures. Recently, HSJs are also found in the magnetosheath downstream of the quasi‐perpendicular shock and they are thought to be derived from magnetic flux tubes connected to the quasi‐parallel bow shock (Kajdič et al., 2021). In this study, the elongated HSJs as flux tubes transfer particles and energy from the solar wind toward the quasi‐perpendicular magnetosheath, which can help understand the formation of quasi‐perpendicular magnetosheath HSJs.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Large‐Scale High‐Speed Jets in Earth's Magnetosheath: Global Hybrid Simulations

Guo

et al. 2022

JGR Space Physics

View full text Add to dashboard Cite

High‐speed jets (HSJs) occur frequently in Earth's magnetosheath downstream of the quasiparallel bow shock. They have great impacts on the magnetosheath and the magnetosphere. Using two‐dimensional global hybrid simulations, we investigate the formation and evolution of HSJs with different solar wind conditions. When the quasi‐parallel shock is formed, HSJs begin to appear in the quasi‐parallel magnetosheath. Some elongated HSJs formed at the quasi‐parallel bow shock extend toward the quasi‐perpendicular magnetosheath along with the background magnetosheath flow. As the elongated HSJs moves in the magnetosheath, filamentary structures of the velocity, ion density, and temperature occur in the magnetosheath. The filamentary structures are the traces of HSJs moving in the magnetosheath. Moreover, the Kelvin‐Helmholtz instability can be excited at HSJs, which causes meandering of HSJs. When the interplanetary magnetic field is aligned to the solar wind velocity, the large‐scale HSJs with a parallel (perpendicular) scale size of about 2.5 RE (0.3 RE) are formed at the magnetosheath where the θBn is approaching zero. Then, some HSJs converge, leading to the formation of even larger HSJs with a parallel (perpendicular) scale size of 5 RE (0.6 RE).

show abstract

Section: Conclusion and Discussionmentioning

confidence: 99%

Large‐Scale High‐Speed Jets in Earth's Magnetosheath: Global Hybrid Simulations

Guo

et al. 2022

JGR Space Physics

View full text Add to dashboard Cite

show abstract

“…The boundaries of cavities in the magnetosheath exhibit flow velocity enhancements or jets relative to the surrounding plasma, where as the boundaries of cavities upstream in the foreshock do not (Kajdič et al. 2021 ; Sibeck et al. 2021 ).…”

Section: Transient Processes In the Foreshock Bow Shock And Magnetosh...mentioning

confidence: 99%

“…However, there is one big difference between the boundaries of cavities in the magnetosheath and upstream from the bow shock. The boundaries of cavities in the magnetosheath exhibit flow velocity enhancements or jets relative to the surrounding plasma, where as the boundaries of cavities upstream in the foreshock do not (Kajdič et al 2021;. Foreshock cavities can drive strong pressure variations in the sheath and along the magnetopause, resulting in strong magnetopause motion (Turner et al 2011).…”

Section: Foreshock Cavitiesmentioning

confidence: 99%

Dayside Transient Phenomena and Their Impact on the Magnetosphere and Ionosphere

et al. 2022

View full text Add to dashboard Cite

Dayside transients, such as hot flow anomalies, foreshock bubbles, magnetosheath jets, flux transfer events, and surface waves, are frequently observed upstream from the bow shock, in the magnetosheath, and at the magnetopause. They play a significant role in the solar wind-magnetosphere-ionosphere coupling. Foreshock transient phenomena, associated with variations in the solar wind dynamic pressure, deform the magnetopause, and in turn generates field-aligned currents (FACs) connected to the auroral ionosphere. Solar wind dynamic pressure variations and transient phenomena at the dayside magnetopause drive magnetospheric ultra low frequency (ULF) waves, which can play an important role in the dynamics of Earth’s radiation belts. These transient phenomena and their geoeffects have been investigated using coordinated in-situ spacecraft observations, spacecraft-borne imagers, ground-based observations, and numerical simulations. Cluster, THEMIS, Geotail, and MMS multi-mission observations allow us to track the motion and time evolution of transient phenomena at different spatial and temporal scales in detail, whereas ground-based experiments can observe the ionospheric projections of transient magnetopause phenomena such as waves on the magnetopause driven by hot flow anomalies or flux transfer events produced by bursty reconnection across their full longitudinal and latitudinal extent. Magnetohydrodynamics (MHD), hybrid, and particle-in-cell (PIC) simulations are powerful tools to simulate the dayside transient phenomena. This paper provides a comprehensive review of the present understanding of dayside transient phenomena at Earth and other planets, their geoeffects, and outstanding questions.

show abstract

“…The origin of MSH jets is still under debate. Regarding jets found downstream of a Qperp shock, they have been associated with a variety of different phenomena such as reconnection exhausts, mirror mode waves and magnetic flux tubes (Blanco‐Cano et al., 2020; Kajdič et al., 2021). Downstream of the Qpar shock, jets have been associated with several other generation mechanisms, from shock ripples (Hietala et al., 2009; Hietala & Plaschke, 2013) to upstream rotational discontinuities (Archer et al., 2012; Dmitriev & Suvorova, 2012) and reconnection (Preisser et al., 2020).…”

Section: Introductionmentioning

confidence: 99%

On Magnetosheath Jet Kinetic Structure and Plasma Properties

Raptis

Karlsson

Vaivads

et al. 2022

Geophysical Research Letters

Self Cite

View full text Add to dashboard Cite

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 (

show abstract

Causes of Jets in the Quasi‐Perpendicular Magnetosheath

Cited by 19 publications

References 60 publications

Large‐Scale High‐Speed Jets in Earth's Magnetosheath: Global Hybrid Simulations

Large‐Scale High‐Speed Jets in Earth's Magnetosheath: Global Hybrid Simulations

Dayside Transient Phenomena and Their Impact on the Magnetosphere and Ionosphere

On Magnetosheath Jet Kinetic Structure and Plasma Properties

Contact Info

Product

Resources

About