Upstream waves at Mars: Phobos observations

Russell, C. T.; Luhmann, J. G.; Schwingenschuh, K.; Riedler, W.; Yeroshenko, Ye.

doi:10.1029/gl017i006p00897

Cited by 142 publications

(89 citation statements)

References 12 publications

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“…High-frequency emissions, broadband electric noise, whistler modes and ULF fluctuations were typically recorded by the wave instrument before the Phobos-2 spacecraft crossed the bow shock. The enhanced level of magnetic field oscillations in the ULF range upstream the Martian bow shock was reported by Russell et al (1990) and Delva and Dubinin (1998). Simultaneous plasma observations have revealed the presence of both ions and electrons reflected from the bow shock and streaming back to the solar wind (Kiraly et al, 1991;Barabash and Lundin, 1991).…”

Section: Introductionmentioning

confidence: 79%

Wave observations at the foreshock boundary in the near-Mars space

et al. 2014

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Wave and plasma measurements carried out by the Phobos-2 spacecraft in the Martian environment indicate that a part of solar wind electrons and ions are reflected and accelerated at the Martian bow shock. These particles streaming back into the solar wind lead to the formation of the foreshock region upstream the planetary bow shock. It is shown that the general structure of the foreshock at Mars is similar to that of the foreshock region upstream the Earth's bow shock. However, the electric emissions observed at frequencies around 100 Hz at the leading edge of electron foreshock at Mars have been never reported for observations in the similar region at Earth. The burst of these waves occurs before the spacecraft enters the electron foreshock identified with the onset of electron plasma waves and calculations of the magnetic connection to the planetary bow shock.

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Section: Introductionmentioning

confidence: 79%

Wave observations at the foreshock boundary in the near-Mars space

et al. 2014

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“…It may be possible to detect these waves using the ARTEMIS vector magnetic field data. Waves from pickup ions have been identified in the plasma environments of many solar system bodies, including Venus, Mars, and even the moons of the giant planets (Russell et al 1990;Kivelson et al 1996;Paterson et al 1999;Grebowsky et al 2004;Dougherty et al 2006;Russell and Blanco-Cano 2007;Delva et al 2008), and their presence or absence can be used to constrain the local density of pickup ions, and therefore the source strength.…”

Section: Exospheric Ions and Plasma Pick-upmentioning

confidence: 99%

ARTEMIS Science Objectives

Sibeck¹,

Angelopoulos²,

Brain³

et al. 2011

The ARTEMIS Mission

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NASA's two spacecraft ARTEMIS mission will address both heliospheric and planetary research questions, first while in orbit about the Earth with the Moon and subsequently while in orbit about the Moon. Heliospheric topics include the structure of the Earth's magnetotail; reconnection, particle acceleration, and turbulence in the Earth's magnetosphere, at the bow shock, and in the solar wind; and the formation and structure of the D.G. Sibeck ( ) Code 674, GSFC/NASA,

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“…The proton gyrofrequency in a background field of B=4 nT is f P =eB/(2π m p )=61 mHz. These waves at the local proton gyrofrequency (PCWs) are low amplitude waves (≈0.15 nT), and they have been described by Russell et al (1990) using ASPERA data measured on Phobos-2 and by Brain et al (2002) using MGS magnetic field data. As Brain et al (2002) stated, these waves were not observed at larger subsolar distances than 3 R M from Mars.…”

Section: Romap Datamentioning

confidence: 99%

“…The first signature of the upstream waves in ROMAP data was obtained at 01:36 UT, when Rosetta was at a distance of about 2 R M from the surface of the planet. Russell et al (1990) concluded that these left-hand polarized waves were formed by ionization of the Martian hydrogen exosphere upstream of the shock. Barabash et al (1991) confirmed this conclusion by results from ASPERA, which observed ring distributions of pickup protons from the hydrogen corona.…”

Section: Romap Datamentioning

confidence: 99%

Rosetta swing-by at Mars – an analysis of the ROMAP measurements in comparison with results of 3-D multi-ion hybrid simulations and MEX/ASPERA-3 data

et al. 2009

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Abstract. The Rosetta spacecraft flew by Mars at a distance of 260 km on 25 February 2007 during a gravity assist manoeuvre. During the closest approach (CA) the lander magnetometer ROMAP was switched on. The dataset taken during this swingby provides insight into the plasma environment around Mars: in addition to a pronounced bow shock crossing Rosetta recorded the signature of the pile up region of draped magnetic field. Also the Rosetta measurements showed signatures of crustal magnetic field anomalies which can be verified by results of a crustal magnetic field model. In order to understand the measured field morphology, multi-ion hybrid simulations were performed. Some of the input parameters for the simulations were obtained from Mars Express (MEX) data which were contemporaneously collected during the Rosetta swingby. These simulations reproduces ROMAP magnetic field measurements and show that the interplanetary magnetic field pointed northward during the encounter. A spectral analysis shows upstream waves ahead of the bow shock and indicates the presence of the magnetic pile-up boundary (MPB). The multi-ion model reproduces the ion fluxes measured by MEX/ASPERA-3 and is in agreement with the measurements to within one order of magnitude.

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Upstream waves at Mars: Phobos observations

Cited by 142 publications

References 12 publications

Wave observations at the foreshock boundary in the near-Mars space

Wave observations at the foreshock boundary in the near-Mars space

ARTEMIS Science Objectives

Rosetta swing-by at Mars – an analysis of the ROMAP measurements in comparison with results of 3-D multi-ion hybrid simulations and MEX/ASPERA-3 data

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