Hot flow anomaly remnant in the far geotail?

Facskó, G.; Opitz, A.; Lavraud, B.; Luhmann, J. G.; Russell, C. T.; Sauvaud, J. A.; Fedorov, A.; Kis, Árpád; Wesztergom, Viktor

doi:10.1016/j.jastp.2015.01.011

Cited by 9 publications

(7 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using multiple spacecraft, C.-P. Wang, Liu, et al (2018) found that foreshock transient-driven perturbations in the magnetosheath can propagate with the driver solar wind discontinuity from dayside to midtail, causing the midtail magnetopause to locally move outward. Using STEREO observations, Facskó, Opitz, et al (2015) also found HFA-like perturbations in the far tail magnetosheath (X ∼ −310 R E ). Using Acceleration Reconnection Turbulence & Electrodynamics of Moon's Interaction with the Sun (ARTEMIS) observations, T. Z.…”

mentioning

confidence: 82%

See 1 more Smart Citation

Statistical Study of Foreshock Transients in the Midtail Foreshock

et al. 2021

View full text Add to dashboard Cite

show abstract

mentioning

confidence: 82%

“…Using STEREO observations, Facskó, Opitz, et al. (2015) also found HFA‐like perturbations in the far tail magnetosheath ( X ∼ −310 R E ). Using Acceleration Reconnection Turbulence & Electrodynamics of Moon’s Interaction with the Sun (ARTEMIS) observations, T. Z. Liu et al.…”

Section: Introductionmentioning

confidence: 91%

Statistical Study of Foreshock Transients in the Midtail Foreshock

et al. 2021

View full text Add to dashboard Cite

show abstract

“…Recent multipoint observations by Wang et al (2018) found that as the driver discontinuity of a foreshock transient convected tailward with the solar wind, the foreshock transient‐driven perturbations propagated with the discontinuity from the dayside magnetosheath to the midtail magnetosheath (X ~ −30 to −50 R E ), which caused local outward motion of the midtail magnetopause. Additionally, STEREO at X ~ −310 R E also observed HFA‐like perturbations in the far tail magnetosheath (Facskó et al, 2015). These results suggest that foreshock transient‐driven perturbations could continuously disturb the magnetosphere‐ionosphere system from dayside to nightside over timescales of tens of minutes.…”

Section: Introductionmentioning

confidence: 95%

ARTEMIS Observations of Foreshock Transients in the Midtail Foreshock

Liu

Wang

et al. 2020

Geophysical Research Letters

View full text Add to dashboard Cite

Foreshock transients such as hot flow anomalies (HFAs) are frequently observed in the dayside foreshock. They can disturb the local bow shock, magnetopause, and consequently the magnetosphereionosphere system through dynamic pressure perturbations. Recent multipoint observations found that such perturbations can even propagate from the dayside to the midtail. However, whether the drivers of such perturbations, foreshock transients, persist in the midtail foreshock has not been observed. Thus, it is unclear whether the observed nightside magnetosheath/magnetopause perturbations are traveling waves or continuously driven by a propagating foreshock transient. Using two Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) spacecraft, we report direct observational evidence of foreshock transients in the midtail foreshock. We present a case study showing an elongated mature HFA propagating with its driver discontinuity from TH-C (X~−43 R E) to TH-B (X~−48 R E). Our results confirm that foreshock transients disturb not only the dayside bow shock but also the nightside bow shock while propagating tailward.

show abstract

“…Collinson et al [] suggested that the smaller physical size of Cytherian HFAs may simply be a result of them not having as long to form before the current sheet entirely transits the shock, and the HFA is swept off down the magnetotail [e.g., see Facskó et al , ]. The time taken ( τ ) for a current sheet to transit the bow shock from one side to the other (flank to flank) is given by equation .…”

Section: Size and Durationmentioning

confidence: 99%

A hot flow anomaly at Mars

Collinson

Halekas

Grebowsky

et al. 2015

Geophysical Research Letters

View full text Add to dashboard Cite

One of the most important modes of planet/solar wind interaction are “foreshock transients” such as hot flow anomalies (HFAs). Here we present early observations by the NASA Mars Atmosphere and Volatile EvolutioN spacecraft, confirming their presence at Mars and for the first time at an unmagnetized planet revealing the underlying ion perturbations that drive the phenomenon, finding them to be weaker than at magnetized planets. Analysis revealed the HFA to be virtually microscopic: the smallest on record at ∼2200 km across and commensurate with the local proton gyroradius, resulting in a much stronger perturbation in solar wind protons than alpha particles. As at Venus, despite being physically diminutive, the HFA is still large (0.66 RM) when compared to the relative size of the induced magnetosphere. Given the associated order of magnitude decrease in solar wind dynamic pressure (411 pPa ⇒ 70 pPa), we find that HFAs at Mars have the potential to directly impact the topside ionosphere. We thus hypothesize that the loss of a planetary magnetic dynamo left Mars far more vulnerable to the pressure pulses resulting from HFAs and related foreshock transients.

show abstract

Hot flow anomaly remnant in the far geotail?

Cited by 9 publications

References 47 publications

Statistical Study of Foreshock Transients in the Midtail Foreshock

Statistical Study of Foreshock Transients in the Midtail Foreshock

ARTEMIS Observations of Foreshock Transients in the Midtail Foreshock

A hot flow anomaly at Mars

Contact Info

Product

Resources

About