Mirror mode structures and ELF plasma waves in the Giacobini-Zinner magnetosheath

Tsurutani, B. T.; Lakhina, G. S.; Smith, E. J.; Buti, B.; Moses, S. L.; Coroniti, F. V.; Brinca, A. L.; Slavin, J. A.; Zwickl, R. D.

doi:10.5194/npg-6-229-1999

Cited by 35 publications

(28 citation statements)

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“…For water ions at a magnetic field strength of B m ≈ 20 nT this leads to T mm ≈ 9 α s. With the measured T mm mentioned above this leads to 11 ≤ α ≤ 16, which is similar to what was found by Tsurutani et al (1999) at comet 21P/Giacobini-Zinner, α GZ ≈ 12, but much larger than what was found by Schmid et al (2014) at comet 1P/Halley, α H ≈ 1-2. Taking the ion velocity as measured by IES, the Larmor radius for water ions becomes ρ H 2 O, i ≈ 280 km.…”

Section: Crossing From 6 To 7 June: Mirror-mode Wavessupporting

confidence: 70%

“…This could imply that the freshly mass-loaded magnetospheric magnetic field is mirror-mode unstable (see e.g. Hasegawa, 1969;Tsurutani et al, 1999;Schmid et al, 2014;Volwerk et al, 2014). As the resolution of the plasma data is too low to check the pressure balance over the MM structures, the magnetic-field-only method by Lucek et al (1999) is used to investigate the data for MM waves.…”

Section: Crossing From 6 To 7 June: Mirror-mode Wavesmentioning

confidence: 99%

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Mass-loading, pile-up, and mirror-mode waves at comet 67P/Churyumov-Gerasimenko

et al. 2016

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Abstract. The data from all Rosetta plasma consortium instruments and from the ROSINA COPS instrument are used to study the interaction of the solar wind with the outgassing cometary nucleus of 67P/Churyumov-Gerasimenko. During 6 and 7 June 2015, the interaction was first dominated by an increase in the solar wind dynamic pressure, caused by a higher solar wind ion density. This pressure compressed the draped magnetic field around the comet, and the increase in solar wind electrons enhanced the ionization of the outflow gas through collisional ionization. The new ions are picked up by the solar wind magnetic field, and create a ring/ringbeam distribution, which, in a high-β plasma, is unstable for mirror mode wave generation. Two different kinds of mirror modes are observed: one of small size generated by locally ionized water and one of large size generated by ionization and pick-up farther away from the comet.

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Section: Crossing From 6 To 7 June: Mirror-mode Wavessupporting

confidence: 70%

Section: Crossing From 6 To 7 June: Mirror-mode Wavesmentioning

confidence: 99%

Mass-loading, pile-up, and mirror-mode waves at comet 67P/Churyumov-Gerasimenko

et al. 2016

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“…The shock compression has been argued to be a source of free energy that generates peak-like MMs and likely both sources need to be available in order to generate the largest amplitude MMs (Tsurutani et al, 2011b). In the heliosheath and cometosheaths, the ion pickup process is also identified as a free energy source (e.g., Tsurutani et al, 1999Tsurutani et al, , 2011aSchmid et al, 2014).…”

Section: M Ala-lahti Et Al: Mirror Mode Wave Occurrence In Icme-mentioning

confidence: 99%

“…They are frequently observed in heliospheric plasma, in particular in different sheath structures. They are the most widely studied in the planetary magnetosheaths (e.g., Tsurutani et al, 1982;Hellinger et al, 2003;Soucek et al, 2008Soucek et al, , 2015Volwerk et al, 2008;Génot et al, 2009b;Herčík et al, 2013;Schmid et al, 2014;Volwerk et al, 2016), but also found in cometosheaths (e.g., Russell et al, 1991;Glassmeier et al, 1993;Tsurutani et al, 1999;Schmid et al, 2014), in the heliosheath (e.g., Liu et al, 2007;Génot, 2008;Tsurutani et al, 2011a) and ahead of the dipolarization front (Wang et al, 2016). MMs are also studied in the solar wind (e.g., Hellinger et al, 2006Hellinger et al, , 2017Bale et al, 2009;Russell et al, 2009), behind interplanetary shocks ) and in addition in interplanetary coronal mass ejections (ICMEs; Siu-Tapia et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

et al. 2018

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Abstract. We present a comprehensive statistical analysis of mirror mode waves and the properties of their plasma surroundings in sheath regions driven by interplanetary coronal mass ejection (ICME). We have constructed a semiautomated method to identify mirror modes from the magnetic field data. We analyze 91 ICME sheath regions from January 1997 to April 2015 using data from the Wind spacecraft. The results imply that similarly to planetary magnetosheaths, mirror modes are also common structures in ICME sheaths. However, they occur almost exclusively as dip-like structures and in mirror stable plasma. We observe mirror modes throughout the sheath, from the bow shock to the ICME leading edge, but their amplitudes are largest closest to the shock. We also find that the shock strength (measured by Alfvén Mach number) is the most important parameter in controlling the occurrence of mirror modes. Our findings suggest that in ICME sheaths the dominant source of free energy for mirror mode generation is the shock compression. We also suggest that mirror modes that are found deeper in the sheath are remnants from earlier times of the sheath evolution, generated also in the vicinity of the shock.

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“…Top: total magnetic field with low-pass filtered (background) magnetic field as a dashed line; middle: electron density; bottom: angles α/γ between minimum/maximum variance direction with the background magnetic field. (Tsurutani et al, 1999). Using VEGA 1 and 2 plasma data Tátrallyay et al (2000b) have shown the presence of sloweddown solar wind plasma and picked up cometary ions at distances between 1.5 to 0.5 million km from the comet, within the bow shock.…”

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confidence: 99%

A comparison between VEGA 1, 2 and Giotto flybys of comet 1P/Halley: implications for Rosetta

et al. 2014

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Abstract. Three flybys of comet 1P/Halley, by VEGA 1, 2 and Giotto, are investigated with respect to the occurrence of mirror mode waves in the cometosheath and field line draping in the magnetic pile-up region around the nucleus. The time interval covered by these flybys is approximately 8 days, which is also the approximate length of an orbit or flyby of Rosetta around comet 67P/Churyumov-Gerasimenko. Thus any significant changes observed around Halley are changes that might occur for Rosetta during one pass of 67P/CG. It is found that the occurrence of mirror mode waves in the cometosheath is strongly influenced by the dynamical pressure of the solar wind and the outgassing rate of the comet. Field line draping happens in the magnetic pile-up region. Changes in nested draping regions (i.e. regions with different B x directions) can occur within a few days, possibly influenced by changes in the outgassing rate of the comet and thereby the conductivity of the cometary ionosphere.

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Mirror mode structures and ELF plasma waves in the Giacobini-Zinner magnetosheath

Cited by 35 publications

References 0 publications

Mass-loading, pile-up, and mirror-mode waves at comet 67P/Churyumov-Gerasimenko

Mass-loading, pile-up, and mirror-mode waves at comet 67P/Churyumov-Gerasimenko

Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

A comparison between VEGA 1, 2 and Giotto flybys of comet 1P/Halley: implications for Rosetta

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