Statistical Properties of Small-scale Linear Magnetic Holes in the Martian Magnetosheath

Wu, Mingyu; Chen, Yi Jen; Du, Aimin; Wang, Guoqiang; Xiao, Shulong; Peng, E; Pan, Zihan; Chen, Yuanqiang; Zhang, Tielong

doi:10.3847/1538-4357/ac090b

Cited by 19 publications

(15 citation statements)

References 35 publications

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“…Different scales of MHs are also present in the magnetosheath of Mars as recently reported by Wu et al. ( 2021 ), with the near‐ubiquitous presence of small‐scale linear MHs in the magnetosheath of Mars lasting less than 1 s in the data.…”

Section: Introductionsupporting

confidence: 81%

Making Waves: Mirror Mode Structures Around Mars Observed by the MAVEN Spacecraft

et al. 2022

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We present an in‐depth analysis of a time interval when quasi‐linear mirror mode structures were detected by magnetic field and plasma measurements as observed by the NASA/Mars Atmosphere and Volatile EvolutioN spacecraft. We employ ion and electron spectrometers in tandem to support the magnetic field measurements and confirm that the signatures are indeed mirror modes. Wedged against the magnetic pile‐up boundary, the low‐frequency signatures last on average ∼10 $\sim 10$ s with corresponding sizes of the order of 15–30 upstream solar wind proton thermal gyroradii, or 10–20 proton gyroradii in the immediate wake of the quasi‐perpendicular bow shock. Their peak‐to‐peak amplitudes are of the order of 30–35 nT with respect to the background field, and appear as a mixture of dips and peaks, suggesting that they may have been at different stages in their evolution. Situated in a marginally stable plasma with β‖ ∼ 1, we hypothesize that these so‐called magnetic bottles, containing a relatively higher energy and denser ion population with respect to the background plasma, are formed upstream of the spacecraft behind the quasi‐perpendicular shock. These signatures are very reminiscent of magnetic bottles found at other unmagnetized objects such as Venus and comets, also interpreted as mirror modes. Our case study constitutes the first unmistakable identification and characterization of mirror modes at Mars from the joint points of view of magnetic field, electron and ion measurements. Up until now, the lack of high‐temporal resolution plasma measurements has prevented such an in‐depth study.

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Section: Introductionsupporting

confidence: 81%

Making Waves: Mirror Mode Structures Around Mars Observed by the MAVEN Spacecraft

et al. 2022

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“…In recent decades, electron-scale magnetic dips are reported to widely exist in the terrestrial current sheet (Ge et al 2011;Shustov et al 2019;Yao et al 2021), planetary magnetosheaths (Huang et al 2017;Goodrich et al 2021;Wu et al 2021), and solar wind (Wang et al 2020a(Wang et al , 2020b(Wang et al , 2021d. And electron-scale magnetic peaks are also revealed to exist in the terrestrial magnetosheath (Yao et al 2018) and solar wind (Wang et al 2021c.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

High-precision Calibration of the Fluxgate Magnetometer Offset Vector in the Terrestrial Magnetosheath

Wang

2022

ApJ

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High-precision magnetic field measurements are of great significance for the in-depth study of the physical processes in the astrophysical plasma environment. To obtain accurate natural magnetic fields, in-flight calibration is one key step to obtaining zero offset of the spaceborne fluxgate magnetometer (FGM). Mirror mode structures, widely existing in the solar wind and planetary magnetosheaths and magnetospheres, can be used to calculate the zero offset. However, it is difficult to obtain an accurate zero offset by the current methods using mirror mode structures in the planetary magnetosheath. Here, we develop a new method to calculate the zero offset of the spaceborne FGM using magnetic dips, which are a kind of mirror mode structure. This method is based on the assumption that the magnetic field is zero in the cross section of the magnetic dip. Our method is able to calculate the zero offset using only one magnetic dip. We test this method by using the data from the Magnetospheric Multiscale Mission, and find that the calculation errors of 78.1% of the estimated zero offsets are <0.5 nT when using 25 magnetic dips in the terrestrial magnetosheath. This suggests that our method is able to achieve a high accuracy of the zero offset in the planetary magnetosheath.

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“…The astrophysical plasma environment has many plasma physical processes, such as reconnections (Zhang et al 2012;Guo et al 2020;Lu et al 2020;Yu et al 2021), instabilities (Ma et al 2017;Zhang et al 2020;Cooper et al 2021), fieldaligned currents (Chen et al 2019a(Chen et al , 2019b(Chen et al , 2021, turbulence (Xiao et al 2018(Xiao et al , 2020a(Xiao et al , 2020b(Xiao et al , 2021, magnetic holes (Wu et al 2021;Chen et al 2022), waves (Wang et al 2014(Wang et al , 2015(Wang et al , 2017(Wang et al , 2019, and wave-particle interactions (Zhao et al 2020;Watt et al 2021). Some of these dynamics affect the evolution of planetary atmospheres and the solarterrestrial space environment (Zhang et al 2016;Milan et al 2017;Ohtani et al 2020;Smith et al 2020;Liu et al 2021), for example, magnetospheric substorms can affect communications and satellite security (Yang et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A New Method of Fluxgate Magnetometer Offset Vector Determination in the Solar Wind Using Any Magnetic Field Variations

Wang

2022

ApJ

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In-depth study of dynamic processes in the astrophysical plasma environment relies on high-precision measurement of the magnetic field. Fluxgate magnetometers (FGMs) are commonly used on spacecraft to measure the magnetic field. However, their zero offsets vary slowly with time, and therefore need regularly in-flight calibration. Traditional methods of calculating the zero offset are based on properties of Alfvén waves, mirror mode structures, or current sheets. Here, we develop a new method of calculating the zero offset using any interplanetary magnetic field (IMF) variations. We create an offset cube according to the possible range of the IMF strength. The average values of B L for the IMF variation events approximately obey the normal distribution if there are enough events, where B L is the magnetic field in the maximum variance direction. Any constant vector added to the natural magnetic field data of the events will make the standard deviation of the normal distribution larger. Thereby, the point is determined to be the zero offset so that the corresponding standard deviation at this point is the minimum in the offset cube. Our test results show that this method has a 95.5% probability of obtaining the zero offset with an error of less than 0.3 nT when 10–21 hr of data are used. Our method provides an option for the in-flight calibration of the spaceborne FGM in the solar wind when there are not enough Alfvén waves, mirror modes, or current sheets.

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Statistical Properties of Small-scale Linear Magnetic Holes in the Martian Magnetosheath

Cited by 19 publications

References 35 publications

Making Waves: Mirror Mode Structures Around Mars Observed by the MAVEN Spacecraft

Making Waves: Mirror Mode Structures Around Mars Observed by the MAVEN Spacecraft

High-precision Calibration of the Fluxgate Magnetometer Offset Vector in the Terrestrial Magnetosheath

A New Method of Fluxgate Magnetometer Offset Vector Determination in the Solar Wind Using Any Magnetic Field Variations

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