Short large‐amplitude magnetic structures (SLAMS) at Venus

Collinson, G.; Wilson, L. B.; Sibeck, D. G.; Shane, N.; Zhang, T.L.; Moore, T. E.; Coates, A. J.; Barabash, S.

doi:10.1029/2012ja017838

Cited by 23 publications

(33 citation statements)

References 51 publications

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“…So far only three potential SLAMS has been observed in the Venusian foreshock (Collinson et al 2012b). Their characteristics are similar to SLAMS observed at Earth.…”

Section: Foreshock Observationssupporting

confidence: 53%

“…The first observations of SLAMS (Short Large-Amplitude Magnetic Structures) in the Venusian foreshock may have been made with VEX (Collinson et al 2012b). SLAMS are previously observed in the Earth's foreshock (Schwartz et al 1992;Mann et al 1994), but have also been detected at comet Giacobini-Zinner (Tsurutani et al 1990) and at Jupiter (Tsurutani et al 1993).…”

Section: Foreshock Observationsmentioning

confidence: 99%

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Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

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Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of "Earth's Twin". Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions. They identified the basic structure of the near-Venus space environment, for example, existence of the bow shock, magnetotail, ionosphere, as well as the lack of the intrinsic magnetic field. A huge leap in knowledge about the solar wind interaction with Venus was made possible by the 14-year long mission, Pioneer Venus Orbiter (PVO), launched in 1978. More recently, ESA's probe, Venus Express (VEX), was inserted into orbit in 2006, operated for 8 years.Owing to its different orbit from that of PVO, VEX made unique measurements in the polar and terminator regions, and probed the near-Venus tail for the first time. The near-tail hosts dynamic processes that lead to plasma energization. These processes in turn lead to the loss of ionospheric ions to space, slowly eroding the Venusian atmosphere. VEX carried an ion spectrometer with a moderate mass-separation capability and the observed ratio of the escaping hydrogen and oxygen ions in the wake indicates the stoichiometric loss of water from Venus. The structure and dynamics of the induced magnetosphere depends on the prevailing solar wind conditions. VEX studied the response of the magnetospheric system on different time scales. A plethora of waves was identified by the magnetometer on VEX; some of them were not previously observed by PVO. Proton cyclotron waves were seen far upstream of the bow shock, mirror mode waves were observed in magnetosheath and whistler mode waves, possibly generated by lightning discharges were frequently seen. VEX also encouraged renewed numerical modeling efforts, including fluid-type of models and particle-fluid hybrid type of models, describing the plasma interaction on scales ranging from ion gyro radius to the entire induced magnetosphere. In this review article, we review what has been found from space physics measurements around Venus (from the solar wind down to the ionopause), with a particular emphasis on updated results since the Venus Express mission. We conclude the article by a short discussion on the remaining open scientific questions and the future of this field.

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“…So far only three potential SLAMS has been observed in the Venusian foreshock (Collinson et al 2012b). Their characteristics are similar to SLAMS observed at Earth.…”

Section: Foreshock Observationssupporting

confidence: 53%

Section: Foreshock Observationsmentioning

confidence: 99%

Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

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“…Recently Halekas et al (2017) have shown using MAVEN data that SLAMS can occur upstream of the Martian bow shock for near-radial interplanetary magnetic fields, reconfiguring the Martian bow shock. Similarly, Collinson et al (2012) have observed SLAMS upstream of the bow shock of Venus. More work is needed to determine how often these waves can steepen, the possibility of shock rippling, and the existence of magnetosheath jets.…”

Section: Discussion and Conclusion On Planetary Bow Shocksmentioning

confidence: 99%

Jets Downstream of Collisionless Shocks

et al. 2018

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The magnetosheath flow may take the form of large amplitude, yet spatially localized, transient increases in dynamic pressure, known as "magnetosheath jets" or "plasmoids" among other denominations. Here, we describe the present state of knowledge with respect to such jets, which are a very common phenomenon downstream of the quasi-parallel bow shock. We discuss their properties as determined by satellite observations (based on both case and statistical studies), their occurrence, their relation to solar wind and foreshock conditions, and their interaction with and impact on the magnetosphere. As carriers of plasma and corresponding momentum, energy, and magnetic flux, jets bear some similarities to bursty bulk flows, which they are compared to. Based on our knowledge of jets in the near Earth environment, we discuss the expectations for jets occurring in other planetary and

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“…Recent simulations by Omidi et al () show that, despite their diminutive size with respect to the ion gyroradius, the foreshocks of unmagnetized planets are nevertheless essentially identical to that at Earth, albeit in miniature. The foreshocks of Venus and Mars exhibit the same plethora of transient phenomena as at Earth, such as whistler waves (Brain et al, ; Orlowski & Russell, ), hot flow anomalies (Collinson, Sibeck, et al, , Collinson et al, , ; Slavin et al, ), short large amplitude magnetic structures (Collinson, Wilson III, et al, ), and spontaneous hot flow anomalies (Collinson et al, ).…”

Section: Introductionmentioning

confidence: 99%

Solar Wind Induced Waves in the Skies of Mars: Ionospheric Compression, Energization, and Escape Resulting From the Impact of Ultralow Frequency Magnetosonic Waves Generated Upstream of the Martian Bow Shock

et al. 2018

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Using data from the National Aeronautics and Space Administration Mars Atmosphere and Voltatile EvolutioN and the European Space Agency Mars Express spacecraft, we show that transient phenomena in the foreshock and solar wind can directly inject energy into the ionosphere of Mars. We demonstrate that the impact of compressive ultralow frequency waves in the solar wind on the induced magnetospheres drive compressional, linearly polarized, magnetosonic ultralow frequency waves in the ionosphere, and a localized electromagnetic "ringing" at the local proton gyrofrequency. The pulsations heat and energize ionospheric plasmas. A preliminary survey of events shows that no special upstream conditions are required in the interplanetary magnetic field or solar wind. Elevated ion densities and temperatures in the solar wind near to Mars are consistent with the presence of an additional population of Martian ions, leading to ion‐ion instablities, associated wave‐particle interactions, and heating of the solar wind. The phenomenon was found to be seasonal, occurring when Mars is near perihelion. Finally, we present simultaneous multipoint observations of the phenomenon, with the Mars Express observing the waves upstream, and Mars Atmosphere and Voltatile EvolutioN observing the response in the ionosphere. When these new observations are combined with decades of previous studies, they collectively provide strong evidence for a previously undemonstrated atmospheric loss process at unmagnetized planets: ionospheric escape driven by the direct impact of transient phenomena from the foreshock and solar wind.

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Short large‐amplitude magnetic structures (SLAMS) at Venus

Cited by 23 publications

References 51 publications

Solar Wind Interaction and Impact on the Venus Atmosphere

Solar Wind Interaction and Impact on the Venus Atmosphere

Jets Downstream of Collisionless Shocks

Solar Wind Induced Waves in the Skies of Mars: Ionospheric Compression, Energization, and Escape Resulting From the Impact of Ultralow Frequency Magnetosonic Waves Generated Upstream of the Martian Bow Shock

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