MGS MAG/ER observations at the magnetic pileup boundary of Mars: draping enhancement and low frequency waves

Bertucci, C.; Mazelle, C.; Crider, D. H.; Mitchell, David; Sauer, K.; Acuña, M. H.; Connerney, J. E. P.; Lin, R. P.; Ness, N. F.; Winterhalter, D.

doi:10.1016/j.asr.2003.04.054

Cited by 62 publications

(44 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Bertucci et al, 2004, Brain et al, 2003. At the top of the region of planetary plasma is a second boundary, the photoelectron boundary (PEB), which is the upper altitude limit of planetary photoelectrons and the lower altitude limit of shocked magnetosheath electrons; the PEB was detected in both MGS and Mars Express data.…”

Section: Introductionmentioning

confidence: 93%

Observations of magnetic anomaly signatures in Mars Express ASPERA-3 ELS data

Soobiah

Coates

Linder

et al. 2006

Icarus

View full text Add to dashboard Cite

Section: Introductionmentioning

confidence: 93%

Observations of magnetic anomaly signatures in Mars Express ASPERA-3 ELS data

Soobiah

Coates

Linder

et al. 2006

Icarus

View full text Add to dashboard Cite

“…Mirror mode waves are found not only in the solar wind at different distances from the Sun, but also in the magnetosheaths of Earth (Tsurutani et al 1982), Mars (Bertucci et al 2004) and Jupiter (Erdös and Balogh 1993). Mirror mode waves are compressional, may have large amplitudes and propagate almost perpendicular to the ambient magnetic field.…”

Section: Magnetosheath Mantle and Tailmentioning

confidence: 99%

Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

View full text Add to dashboard Cite

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.

show abstract

“…They used this definition of the IMB due to the lack of magnetic field instruments aboard Mars Express, avoiding conflicts with defined features such as the magnetic pile-up boundary (Vignes et al, 2000). Based on their analysis of MGS magnetic field data, Bertucci et al (2004) identify a significant magnetic field enhancement near the MPB. It is confirmed (Bertucci et al, 2005a) that the MPB is a well-defined plasma boundary which can be characterized as a tangential discontinuity.…”

Section: Introductionmentioning

confidence: 99%

Physics of the Ion Composition Boundary: a comparative 3-D hybrid simulation study of Mars and Titan

et al. 2007

View full text Add to dashboard Cite

Abstract. The plasma environments of Mars and Titan have been studied by means of a 3-D hybrid simulation code, treating the electrons as a massless, charge-neutralizing fluid, whereas ion dynamics are covered by a kinetic approach. As neither Mars nor Titan possesses a significant intrinsic magnetic field, the upstream plasma flow interacts directly with the planetary ionosphere. The characteristic features of the interaction region are determined as a function of the alfvénic, sonic and magnetosonic Mach number of the impinging plasma. For the Martian interaction with the solar wind as well as for the case of Titan being located outside Saturn's magnetosphere in times of high solar wind dynamic pressure, all three Mach numbers are larger than 1. In such a scenario, the interaction gives rise to a so-called Ion Composition Boundary, separating the ionospheric plasma from the ambient flow and being highly asymmetric with respect to the direction of the convective electric field. The formation of these features is explained by analyzing the Lorentz forces acting on ionospheric and ambient plasma particles. Titan's plasma environment is highly variable and allows various different combinations of the three Mach numbers. Therefore, the Ion Composition Boundary may vanish under certain circumstances. The relevant physical mechanism is illustrated as a function of the Mach numbers in the upstream plasma flow.

show abstract

MGS MAG/ER observations at the magnetic pileup boundary of Mars: draping enhancement and low frequency waves

Cited by 62 publications

References 25 publications

Observations of magnetic anomaly signatures in Mars Express ASPERA-3 ELS data

Observations of magnetic anomaly signatures in Mars Express ASPERA-3 ELS data

Solar Wind Interaction and Impact on the Venus Atmosphere

Physics of the Ion Composition Boundary: a comparative 3-D hybrid simulation study of Mars and Titan

Contact Info

Product

Resources

About