Magnetosheath jet occurrence rate in relation to CMEs and SIRs

Koller, Florian; Temmer, Manuela; Preisser, Luis; Plaschke, Ferdinand; Geyer, Paul; Jian, L. K.; Roberts, Owen; Hietala, Heli; LaMoury, Adrian T.

doi:10.1002/essoar.10508761.1

Cited by 2 publications

(3 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The second jet list, named the local jet list, is based on local magnetosheath data to reduce the previously mentioned biases. We provide both new jet lists (upstream and local criteria) and the magnetosheath times at https://osf.io/6ywjz/ (Koller et al., 2021 ).…”

Section: Methodsmentioning

confidence: 99%

“…Both original jet lists covering the time ranges of 2008–2012 and 2012–2018 are available online https://osf.io/gf732/ (Plaschke, Hietala, & Angelopoulos, 2020 ), https://osf.io/7rjs4/ (Plaschke, Hietala, & LaMoury, 2020 ). We provide the new jet lists (upstream and local criteria) as well as the magnetosheath times at https://osf.io/6ywjz/ (Koller et al., 2021 ).…”

Section: Data Availability Statementmentioning

confidence: 99%

See 1 more Smart Citation

Magnetosheath Jet Occurrence Rate in Relation to CMEs and SIRs

et al. 2022

Self Cite

View full text Add to dashboard Cite

Magnetosheath jets constitute a significant coupling effect between the solar wind (SW) and the magnetosphere of the Earth. In order to investigate the effects and forecasting of these jets, we present the first‐ever statistical study of the jet production during large‐scale SW structures like coronal mass ejections (CMEs), stream interaction regions (SIRs) and high speed streams (HSSs). Magnetosheath data from Time History of Events and Macroscale Interactions during Substorms (THEMIS) spacecraft between January 2008 and December 2020 serve as measurement source for jet detection. Two different jet definitions were used to rule out statistical biases induced by our jet detection method. For the CME and SIR + HSS lists, we used lists provided by literature and expanded on incomplete lists using OMNI data to cover the time range of May 1996 to December 2020. We find that the number and total time of observed jets decrease when CME‐sheaths hit the Earth. The number of jets is lower throughout the passing of the CME‐magnetic ejecta (ME) and recovers quickly afterward. On the other hand, the number of jets increases during SIR and HSS phases. We discuss a few possibilities to explain these statistical results.

show abstract

Section: Methodsmentioning

confidence: 99%

Section: Data Availability Statementmentioning

confidence: 99%

Magnetosheath Jet Occurrence Rate in Relation to CMEs and SIRs

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…More recently, investigations have focused on the connection of jets to upstream foreshock structures (Karlsson et al., 2015; Omelchenko et al., 2021; Sibeck et al., 2021; Suni et al., 2021) and to the reformation of the Qpar shock (Raptis et al., 2022). While the exact generation mechanism of these structures is still under investigation, the connection to SW properties such as the cone angle and transient events has been demonstrated in various recent studies, indicating that there is a direct link between SW conditions and MSH jets (Koller et al., 2022; LaMoury et al., 2021; Plaschke et al., 2013; Tinoco‐Arenas et al., 2022).…”

Section: Introductionmentioning

confidence: 99%

On Magnetosheath Jet Kinetic Structure and Plasma Properties

Raptis

Karlsson

Vaivads

et al. 2022

Geophysical Research Letters

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

Magnetosheath jet occurrence rate in relation to CMEs and SIRs

Cited by 2 publications

References 0 publications

Magnetosheath Jet Occurrence Rate in Relation to CMEs and SIRs

Magnetosheath Jet Occurrence Rate in Relation to CMEs and SIRs

On Magnetosheath Jet Kinetic Structure and Plasma Properties

Contact Info

Product

Resources

About