Structure and variations of solar wind-Mars interaction region

Bogdanov, A. V.; Вайсберг, О. Л.

doi:10.1029/ja080i004p00487

Cited by 62 publications

(10 citation statements)

References 13 publications

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“…This study extends the initial Phobos 2 bow shock analyses [Riedler et al, 1989;Schwingenschuh et al, 1990] the passage of an interplanetary shock pair over the spacecraft. Unusually distant dayside bow shock crossings were also reported by Mars 2 and 3 and used to argue in favor of the existence of modest intrinsic magnetic field which can expand outward during intervals of weak solar wind dynamic pressure [Dolginov et al, 1973;Bogdanov and Vaisberg, 1975;Dolginov, 1978;Slavin et al, 1983]. The Phobos 2 observations appear to confirm that such events occur at a rate of about once per month.…”

Section: Introductionmentioning

confidence: 81%

The solar wind interaction with Mars: Mariner 4, Mars 2, Mars 3, Mars 5, and Phobos 2 observations of bow shock position and shape

Slavin

Schwingenschuh²,

Riedler³

et al. 1991

J. Geophys. Res.

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Observations taken by Mariner 4, Mars 2, Mars 3, Mars 5, and Phobos 2 are used to model the shape, position, and variability of the Martian bow shock for the purpose of better understanding the interaction of this planet with the solar wind. Emphasis is placed upon comparisons with the results of similar analyses at Venus, the only planet known to have no significant intrinsic magnetic field. Excellent agreement is found between Mars bow shock models derived from the earlier Mariner‐Mars data set (24 crossings in 1964–1974) and the far more extensive observations recently returned by Phobos 2 (94 crossings in 1989). The best fit model to the aggregate data set locates the subsolar bow shock at a planetocentric distance of 1.56±0.04 RM. Mapped into the terminator plane, the average distance to the Martian bow shock is 2.66±0.05 RM. Compared with Venus, the bow wave at Mars is significantly more distant in the terminator plane, 2.7 RM versus 2.4 RV, and over twice as variable in location with a standard deviation of 0.49 RM versus 0.21 RV at Venus. The Mars 2, 3, and 5 and Phobos 2 data also contain a small number of very distant dayside shock crossings with inferred subsolar obstacle radii derived from gasdynamic modeling of 2000 to 4000 km. Such distant bow shock occurrences do not appear to take place at Venus and may be associated with the expansion of a small Martian magnetosphere under the influence of unusually low solar wind pressure. Finally, the altitude of the Venus bow shock has a strong solar cycle dependence believed to be due to the effect of solar EUV on the neutral atmosphere and mass loading. Comparison of the Phobos 2 shock observations near solar maximum (Rz = 141) with the Mariner‐Mars measurements taken much farther from solar maximum (Rz = 59) indicates that the Martian bow shock location is independent of solar cycle phase and, hence, solar EUV flux. These results are interpreted in terms of a hybrid solar wind interaction model in which this planet possesses a weak, but significant, intrinsic magnetic field.

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Section: Introductionmentioning

confidence: 81%

The solar wind interaction with Mars: Mariner 4, Mars 2, Mars 3, Mars 5, and Phobos 2 observations of bow shock position and shape

Slavin

Schwingenschuh²,

Riedler³

et al. 1991

J. Geophys. Res.

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“…From 1971 to 1974 the Soviet Mars missions (2, 3, 5) also measured the bow shock and the underlying sheath using magnetometers and ion and electron instruments (e.g. Bogdanov and Vaisberg, 1975;Dolginov et al, 1976). Additionally, they made the first measurements of the "ion cushion", identified in Figure 1 as the MPR.…”

Section: Introductionmentioning

confidence: 99%

Mars Global Surveyor Measurements of the Martian Solar Wind Interaction

Brain

2006

Space Sci Rev

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The solar wind at Mars interacts with the extended atmosphere and small-scale crustal magnetic fields. This interaction shares elements with a variety of solar system bodies, and has direct bearing on studies of the long-term evolution of the Martian atmosphere, the structure of the upper atmosphere, and fundamental plasma processes. The magnetometer (MAG) and electron reflectometer (ER) on Mars Global Surveyor (MGS) continue to make many contributions toward understanding the plasma environment, thanks in large part to a spacecraft orbit that had low periapsis, had good coverage of the interaction region, and has been long-lived in its mapping orbit. The crustal magnetic fields discovered using MGS data perturb plasma boundaries on timescales associated with Mars' rotation and enable a complex magnetic field topology near the planet. Every portion of the plasma environment has been sampled by MGS, confirming previous measurements and making new discoveries in each region. The entire system is highly variable, and responds to changes in solar EUV flux, upstream pressure, IMF direction, and the orientation of Mars with respect to the Sun and solar wind flow. New insights from MGS should come from future analysis of new and existing data, as well as multi-spacecraft observations.

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“…Measurements of the Martian bow shock have been reported since the earliest missions to Mars, such as the Mariner 4 flyby (in 1964 [e.g., Smith et al , ; Dryer and Heckman , ; Spreiter and Rizzi , ]), Mars 2, 3, 5 orbiters (1971–1974 [e.g., Gringauz et al , , ; Vaisberg et al , ; Bogdanov and Vaisberg , ; Dolginov et al , ; Russell , , , , ]), and the Phobos 2 orbiter (in 1989 [e.g. Riedler et al , ; Schwingenschuh et al , ; Trotignon et al , , , ]).…”

Section: Introductionmentioning

confidence: 99%

Annual variations in the Martian bow shock location as observed by the Mars Express mission

et al. 2016

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The Martian bow shock distance has previously been shown to be anticorrelated with solar wind dynamic pressure but correlated with solar extreme ultraviolet (EUV) irradiance. Since both of these solar parameters reduce with the square of the distance from the Sun, and Mars' orbit about the Sun increases by ∼0.3 AU from perihelion to aphelion, it is not clear how the bow shock location will respond to variations in these solar parameters, if at all, throughout its orbit. In order to characterize such a response, we use more than 5 Martian years of Mars Express Analyser of Space Plasma and EneRgetic Atoms (ASPERA‐3) Electron Spectrometer measurements to automatically identify 11,861 bow shock crossings. We have discovered that the bow shock distance as a function of solar longitude has a minimum of 2.39RM around aphelion and proceeds to a maximum of 2.65RM around perihelion, presenting an overall variation of ∼11% throughout the Martian orbit. We have verified previous findings that the bow shock in southern hemisphere is on average located farther away from Mars than in the northern hemisphere. However, this hemispherical asymmetry is small (total distance variation of ∼2.4%), and the same annual variations occur irrespective of the hemisphere. We have identified that the bow shock location is more sensitive to variations in the solar EUV irradiance than to solar wind dynamic pressure variations. We have proposed possible interaction mechanisms between the solar EUV flux and Martian plasma environment that could explain this annual variation in bow shock location.

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Structure and variations of solar wind-Mars interaction region

Cited by 62 publications

References 13 publications

The solar wind interaction with Mars: Mariner 4, Mars 2, Mars 3, Mars 5, and Phobos 2 observations of bow shock position and shape

The solar wind interaction with Mars: Mariner 4, Mars 2, Mars 3, Mars 5, and Phobos 2 observations of bow shock position and shape

Mars Global Surveyor Measurements of the Martian Solar Wind Interaction

Annual variations in the Martian bow shock location as observed by the Mars Express mission

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