Solar and interplanetary control of the location of the Venus bow shock

Russell, C. T.; Chou, Eric; Luhmann, J. G.; Gazis, P. R.; Brace, L. H.; Hoegy, W. R.

doi:10.1029/ja093ia06p05461

Cited by 123 publications

(155 citation statements)

References 19 publications

Supporting

Mentioning

144

Contrasting

Order By: Relevance

“…Fitting the observed bow shock locations for 20 Zhang et al (2008a) found that L ≈ 2.14 and ≈ 0.621, which leads to a terminator distance of R BS,t ≈ 2.14 R V , which is slightly smaller than the value R BS,t ≈ 2.40 R V which was found by Russell et al (1988) for solar maximum conditions using Pioneer Venus Orbiter data, with an eccentricity ≈ 0.609.…”

Section: Bow Shock Locationmentioning

confidence: 72%

“…First, there are more events for solar maximum (a total of 1857 events) than for solar minimum (a total of 1637 events). Also, it can be seen that the events for solar maximum already appear more distant from Venus as the nominal solar maximum bow shock location (Russell et al, 1988) is at greater distances than the solar minimum bow shock location .…”

Section: Statistical Studymentioning

confidence: 93%

See 1 more Smart Citation

Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

et al. 2016

View full text Add to dashboard Cite

Abstract. The observational rate of mirror mode waves in Venus's magnetosheath for solar maximum conditions is studied and compared with previous results for solar minimum conditions. It is found that the number of mirror mode events is approximately 14 % higher for solar maximum than for solar minimum. A possible cause is the increase in solar UV radiation, ionizing more neutrals from Venus's exosphere and the outward displacement of the bow shock during solar maximum. Also, the solar wind properties (speed, density) differ for solar minimum and maximum. The maximum observational rate, however, over Venus's magnetosheath remains almost the same, with only differences in the distribution along the flow line. This may be caused by the interplay of a decreasing solar wind density and a slightly higher solar wind velocity for this solar maximum. The distribution of strengths of the mirror mode waves is shown to be exponentially falling off, with (almost) the same coefficient for solar maximum and minimum. The plasma conditions in Venus's magnetosheath are different for solar minimum as compared to solar maximum. For solar minimum, mirror mode waves are created directly behind where the bow shock will decay, whereas for solar maximum all created mirror modes can grow.

show abstract

Section: Bow Shock Locationmentioning

confidence: 72%

Section: Statistical Studymentioning

confidence: 93%

Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

et al. 2016

View full text Add to dashboard Cite

show abstract

“…In the case of the solar wind interaction with Venus, the location of the BS is very sensitive to the upstream solar wind parameters, the orientation of the interplanetary magnetic field, and the solar cycle and the solar EUV flux (Russell et al, 1988). On the other hand, although the location of the Martian BS has been found to be highly variable, the solar activity and the solar EUV flux does not play a decisive role on the BS variations.…”

Section: The Bow Shockmentioning

confidence: 93%

Simulated solar wind plasma interaction with the Martian exosphere: influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary

Modolo

Chanteur²,

Dubinin³

et al. 2006

Ann. Geophys.

View full text Add to dashboard Cite

Abstract. The solar wind plasma interaction with the Martian exosphere is investigated by means of 3-D multi-species hybrid simulations. The influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary is examined by comparing two simulations describing the two extreme states of the solar cycle. The hybrid formalism allows a kinetic description of each ions species and a fluid description of electrons. The ionization processes (photoionization, electron impact and charge exchange) are included self-consistently in the model where the production rate is computed locally, separately for each ionization act and for each neutral species. The results of simulations are in a reasonable agreement with the observations made by Phobos 2 and Mars Global Surveyor spacecraft. The position of the bow shock and the magnetic pile-up boundary is weakly dependent of the solar EUV flux. The motional electric field creates strong asymmetries for the two plasma boundaries.

show abstract

“…We have not been able to study the influence of the solar wind magnetosonic Mach number since we do not have upstream magnetic field measurements. At Venus for instance, the magnetosonic Mach number has been shown to be of importance in determining the position of the BS (Russell et al, 1988) and it is expected that it should play a role at Mars too.…”

Section: Discussionmentioning

confidence: 99%

Plasma boundary variability at Mars as observed by Mars Global Surveyor and Mars Express

et al. 2009

View full text Add to dashboard Cite

Abstract. We have used Mars Express (MEX) and MarsGlobal Surveyor (MGS) simultaneous and non-simultaneous measurements to study the Martian plasma environment. In particular, we have derived quantitative expressions for the altitude of the terminator bow shock (BS) and magnetic pileup boundary (MPB) as functions of solar wind dynamic pressure, crustal magnetic fields and solar EUV flux. We have also studied the influence of the interplanetary magnetic field (IMF) direction. Through simultaneous two-spacecraft case studies we have shown that the dynamic pressure has a strong influence on the location and shape of these boundaries, which is also confirmed through a large statistical study. A higher dynamic pressure pushes the boundaries downward. The IMF direction has a weaker but still significant influence on both boundaries and causes them to move outward in the hemisphere of locally upward electric field. However, the MPB in the Southern Hemisphere is found to actually move inward when the electric field is directed locally upward. The crustal magnetic fields in the Southern Hemisphere have a strong influence on the MPB and cause it to move to higher altitudes over strong crustal magnetic fields. The influence of the crustal magnetic fields on the BS is more ambiguous since there are few crossings over the strongest crustal fields, but there appears to be at least a small trend of a higher BS for stronger crustal fields. An increased solar EUV flux has been found to cause the BS to move outward and the MPB to move inward.

show abstract

Solar and interplanetary control of the location of the Venus bow shock

Cited by 123 publications

References 19 publications

Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

Simulated solar wind plasma interaction with the Martian exosphere: influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary

Plasma boundary variability at Mars as observed by Mars Global Surveyor and Mars Express

Contact Info

Product

Resources

About