Steepened Magnetosonic Waves at Comet Giacobini-Zinner

Tsurutani, B. T.; Thorne, R. M.; Smith, E. J.; Gosling, J. T.; Matsumoto, Hiroshi

doi:10.1029/sp027p0085

Cited by 6 publications

(7 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As discussed in section 3, the ion‐density and the ion‐temperature fluctuations are found to be anticorrelated. Such anticorrelation between electron temperature and density fluctuations was used by Thomsen et al [] and Tsurutani et al [] to distinguish upstream waves from viscous like subshocks. Since our wave also has this feature, upstream subshocks are not a possibility for our wave.…”

Section: Discussionmentioning

confidence: 99%

“…When these ion populations interact with the solar wind, they can lead to generation of low‐frequency (LF) plasma waves via resonance, usually with a frequency near the ion gyrofrequency [ Russell , ]. Upstream LF waves excited by newly born pickup ions have been observed at Mars [ Russell et al , ] and at comets [ Brinca and Tsurutani , ; Brinca , ; Le et al , ; Mazelle and Neubauer , ; Tan et al , ; Thorne and Tsurutani , ; Tsurutani and Smith , ; Tsurutani et al , ]. These pickup ions are formed by photoionization or electron impact ionization of neutrals in the exospheres of planets and comets.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

MAVEN observation of an obliquely propagating low‐frequency wave upstream of Mars

et al. 2016

View full text Add to dashboard Cite

We report Mars Atmosphere and Volatile EvolutioN mission observations of a large amplitude low‐frequency plasma wave that propagated oblique to the ambient magnetic field upstream of Mars along with a non‐solar‐wind plasma component that had a flow velocity perpendicular to the magnetic field. We consider nine possibilities for this wave that include various combinations of its propagation direction, polarization in the solar wind frame, and ion source responsible for its generation. Using the observed wave parameters and the measured plasma parameters as constraints, we uniquely identify the wave by systematically discarding these possibilities. We determine that the wave is a right‐hand polarized wave that propagated upstream in the solar wind frame. We find two possibilities for the ion source that can be responsible for this wave generation. They are either newly born pickup protons or reflected solar wind protons from the bow shock. We determine that the observed non‐solar‐wind component is not responsible for the wave generation, and it is likely that the non‐solar‐wind component was merely perturbed by the passage of the wave.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

MAVEN observation of an obliquely propagating low‐frequency wave upstream of Mars

et al. 2016

View full text Add to dashboard Cite

show abstract

“…As they convect deeper into the foreshock, they enter regions of higher ion density. These ions alter the index of refraction for the medium causing transverse modes to become compressive, and thus the waves can steepen [e.g., Collinson et al , ; Wilson et al , ; Tsubouchi and Lembège , ; Tsurutani et al , , and references therein]. They become more oblique and compressional the deeper they go.…”

Section: Assessment Of Shfa Formation Conditions At Mars and Venusmentioning

confidence: 99%

Spontaneous hot flow anomalies at Mars and Venus

Collinson

Sibeck

Omidi³

et al. 2017

JGR Space Physics

View full text Add to dashboard Cite

We report the first observations of Spontaneous Hot Flow Anomalies (SHFAs) at Venus and Mars, demonstrating their existence in the foreshocks of other planets beyond Earth. Using data from the ESA Venus Express and the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft, we present magnetic and plasma observations from events at both planets, exhibiting properties similar to “classical” Hot Flow Anomalies, with bounding shock‐like compressive regions and a hot and diffuse core. However, these explosive foreshock transients were observed without any attendant interplanetary magnetic field discontinuity, consistent with SHFAs observed at Earth and our hybrid simulations.

show abstract

“…As they convect deeper into the foreshock, they enter regions of higher diffuse ion density. These ions alter the index of refraction for the medium causing transverse modes to become compressive, and thus the waves can steepen [e.g., Wilson et al , 2009; Tsubouchi and Lembège , 2004; Tsurutani et al , 1987, and references therein]. They become more oblique and compressional the deeper they go.…”

Section: Introductionmentioning

confidence: 99%

Short large‐amplitude magnetic structures (SLAMS) at Venus

Collinson¹,

Wilson²,

Sibeck³

et al. 2012

J. Geophys. Res.

View full text Add to dashboard Cite

[1] We present the first observation of magnetic fluctuations consistent with short large-amplitude magnetic structures (SLAMS) in the foreshock of the planet Venus. Three monolithic magnetic field spikes were observed by the Venus Express on 11 April 2009. The structures were 1.5-11 s in duration, had magnetic compression ratios between 3 and 6, and exhibited elliptical polarization. These characteristics are consistent with the SLAMS observed at Earth, Jupiter, and Comet Giacobini-Zinner, and thus we hypothesize that it is possible SLAMS may be found at any celestial body with a foreshock.

show abstract

Steepened Magnetosonic Waves at Comet Giacobini-Zinner

Cited by 6 publications

References 41 publications

MAVEN observation of an obliquely propagating low‐frequency wave upstream of Mars

MAVEN observation of an obliquely propagating low‐frequency wave upstream of Mars

Spontaneous hot flow anomalies at Mars and Venus

Short large‐amplitude magnetic structures (SLAMS) at Venus

Contact Info

Product

Resources

About