Structure of the Front of a Collisionless Oblique Interplanetary Shock Wave from High Time Resolution Measurements of Solar-Wind Plasma Parameters

Abstract. Recent studies of solar wind MHD turbulence show that current-sheet-like structures are common in the solar wind and they are a significant source of solar wind MHD turbulence intermittency. While numerical simulations have suggested that such structures can arise from non-linear interactions of MHD turbulence, a recent study by Borovsky (2006), upon analyzing one year worth of ACE data, suggests that these structures may represent the magnetic walls of flux tubes that separate solar wind plasma into distinct bundles and these flux tubes are relic structures originating from boundaries of supergranules on the surface of the Sun. In this work, we examine whether there are such structures in the Earth's magnetotail, an environment vastly different from the solar wind. We use high time resolution magnetic field data of the FGM instrument onboard Cluster C1 spacecraft. The orbits of Cluster traverse through both the solar wind and the Earth's magnetosheath and magnetotail. This makes its dataset ideal for studying differences between solar wind MHD turbulence and that inside the Earth's magnetosphere. For comparison, we also perform the same analysis when Cluster C1 is in the solar wind. Using a data analysis procedure first introduced in Li (2007, 2008), we find that current-sheet-like structures can be clearly identified in the solar wind. However, similar structures do not exist inside the Earth's magnetotail. This result can be naturally explained if these structures have a solar origin as proposed by Borovsky (2006). With such a scenario, current analysis of solar wind MHD turbulence needs to be improved to include the effects due to these curent-sheet-like structures.

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He++ behavior on the an interplanetary shock wave

10.5194/egusphere-egu21-6073 ◽

2021 ◽

Author(s):

Olga Sapunova ◽

Natalia Borodkova ◽

Yuri Yermolaev ◽

Georgii Zastenker

Keyword(s):

Shock Wave ◽

Relative Density ◽

Solar Wind Plasma ◽

Interplanetary Shock ◽

High Time Resolution ◽

Plasma Velocity ◽

Short Term ◽

Absolute Value ◽

Interplanetary Shock Wave ◽

Very High

In our study we analyzing the fine structure of interplanetary shock wave fronts recorded by the BMSW experiment, installed onboard the SPEKTR-R satellite. The high time resolution of the spectrometer (0.031 s for the plasma flux magnitude and direction and 1.5 s for velocity, temperature, and density) makes it possible to study the internal structure of the IPs front.BMSW experiment registered 55 IPs waves from 2011 to 2019. For 21 events (where the temperature was not very high), the parameters of twice-ionized helium (He++ or &#945;-particles) - density (absolute value and relative to protons content in the solar wind plasma), velocity, temperature. It is shown that the speed of He++ is slightly less (for about 5%) than the speed of protons, the relative density of He++ rarely exceeds 10%, and the temperature of He++ is about 2 times higher than the temperature of protons.On the IPs front, short-term and significant (up to 20%) jumps in the relative density of He++ were detected in several events. No dependence was found between Mms/proton beta and He++ density changing after IPs front. However, we detected that the lower Qbn parameter is, the more the relative density of He++ falls behind the IPs front.

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Higher-Order Statistics in Compressive Solar Wind Plasma Turbulence: High-Resolution Density Observations From the Magnetospheric MultiScale Mission

10.5194/egusphere-egu21-2032 ◽

2021 ◽

Author(s):

Owen Roberts ◽

Jessica Thwaites ◽

Luca Sorriso-Valvo ◽

Rumi Nakamura ◽

Zoltan Voros

Keyword(s):

Solar Wind ◽

Time Resolution ◽

Measurement Techniques ◽

Time Lag ◽

Solar Wind Plasma ◽

Density Fluctuations ◽

High Time ◽

High Time Resolution ◽

Time Lags ◽

Spacecraft Potential

Turbulent density fluctuations are investigated in the solar wind at sub-ion scales using calibrated spacecraft potential. The measurement technique using the spacecraft potential allows for a much higher time resolution and sensitivity when compared to direct measurements using plasma instruments. Using this novel method, density fluctuations can be measured with unprecedentedly high time resolutions for in situ measurements of solar wind plasma at 1 a.u. By investigating 1 h of high-time resolution data, the scale dependant kurtosis is calculated by varying the time lag &#964; to calculate increments between observations. The scale-dependent kurtosis is found to increase towards ion scales but then plateaus and remains fairly constant through the sub-ion range in a similar fashion to magnetic field measurements. The sub-ion range is also found to exhibit self-similar monofractal behavior contrasting sharply with the multi-fractal behavior at large scales. The scale-dependent kurtosis is also calculated using increments between two different spacecraft. When the time lags are converted using the ion bulk velocity to a comparable spatial lag, a discrepancy is observed between the two measurement techniques. Several different possibilities are discussed including a breakdown of Taylor&#8217;s hypothesis, high-frequency plasma waves, or intrinsic differences between sampling directions.

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Fine Structure of Interplanetary Shock Front—Results from BMSW Experiment with High Time Resolution

Journal of Geophysical Research Space Physics ◽

10.1029/2018ja026255 ◽

2019 ◽

Vol 124 (11) ◽

pp. 8191-8207 ◽

Cited By ~ 1

Author(s):

N.L. Borodkova ◽

V.G. Eselevich ◽

G.N. Zastenker ◽

O.V. Sapunova ◽

Yu.I. Yermolaev ◽

...

Keyword(s):

Fine Structure ◽

Shock Front ◽

Time Resolution ◽

Interplanetary Shock ◽

High Time ◽

High Time Resolution

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Interaction of interplanetary shock wave with the solar wind

Journal of Atmospheric and Solar-Terrestrial Physics ◽

10.1016/j.jastp.2020.105340 ◽

2020 ◽

Vol 207 ◽

pp. 105340

Author(s):

I.A. Molotkov ◽

B. Atamaniuk

Keyword(s):

Shock Wave ◽

Solar Wind ◽

Interplanetary Shock ◽

Interplanetary Shock Wave

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High Time Resolution Spectroscopic Observations of Stellar Shock Waves

Symposium - International Astronomical Union ◽

10.1017/s0074180900035026 ◽

1988 ◽

Vol 132 ◽

pp. 205-208

Author(s):

P. L. Cottrell ◽

W. A. Lawson ◽

S. M. Smith

Keyword(s):

Shock Wave ◽

Shock Waves ◽

Absorption Line ◽

Time Resolution ◽

High Time ◽

High Time Resolution ◽

Minimum Radius ◽

Maximum Light ◽

Spectroscopic Observations ◽

Line Splitting

An absorption line–splitting phenomenon, first reported by Cottrell and Lambert (1982a), has been shown to occur at about maximum light in the semi-regular pulsations of the R Coronae Borealis (RCB) star, RY Sgr (Lawson 1986). This has been interpreted as a shock wave propagating through the photospheric layers (Lawson and Cottrell 1986). We present spectroscopic observations of this star, taken to coincide with this line–splitting event. A sequence obtained during 1986 October revealed that this event extended over about 6 days (out of a period of about 40 days) and began at about the bluest B-V. This colour maximum, which corresponds to maximum photospheric temperatures and minimum radius, leads the V maximum by about 6 days.

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A high time resolution study of the solar wind-magnetosphere energy coupling function

Planetary and Space Science ◽

10.1016/0032-0633(82)90162-3 ◽

1982 ◽

Vol 30 (6) ◽

pp. 537-543 ◽

Cited By ~ 12

Author(s):

S.-I. Akasofu ◽

J.F. Carbary ◽

C.-I. Meng ◽

J.P. Sullivan ◽

R.P. Lepping

Keyword(s):

Solar Wind ◽

Time Resolution ◽

Energy Coupling ◽

Coupling Function ◽

High Time ◽

High Time Resolution ◽

Resolution Study

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Magnetopause boundary structure deduced from the high-time resolution particle experiment on the Equator-S spacecraft

Annales Geophysicae ◽

10.1007/s00585-999-1574-3 ◽

1999 ◽

Vol 17 (12) ◽

pp. 1574-1581 ◽

Cited By ~ 1

Author(s):

G. K. Parks ◽

S. Datta ◽

M. McCarthy ◽

R. P. Lin ◽

H. Reme ◽

...

Keyword(s):

Solar Wind ◽

Time Resolution ◽

Boundary Region ◽

Control Device ◽

Electron Energy Spectrum ◽

Wind Pressure ◽

High Time ◽

Boundary Structure ◽

High Time Resolution ◽

Magnetospheric Configuration And Dynamics

Abstract. An electrostatic analyser (ESA) onboard the Equator-S spacecraft operating in coordination with a potential control device (PCD) has obtained the first accurate electron energy spectrum with energies ≈7 eV–100 eV in the vicinity of the magnetopause. On 8 January, 1998, a solar wind pressure increase pushed the magnetopause inward, leaving the Equator-S spacecraft in the magnetosheath. On the return into the magnetosphere approximately 80 min later, the magnetopause was observed by the ESA and the solid state telescopes (the SSTs detected electrons and ions with energies ≈20–300 keV). The high time resolution (3 s) data from ESA and SST show the boundary region contains of multiple plasma sources that appear to evolve in space and time. We show that electrons with energies ≈7 eV–100 eV permeate the outer regions of the magnetosphere, from the magnetopause to ≈6Re. Pitch-angle distributions of ≈20–300 keV electrons show the electrons travel in both directions along the magnetic field with a peak at 90° indicating a trapped configuration. The IMF during this interval was dominated by Bx and By components with a small Bz.Key words. Magnetospheric physics (magnetopause · cusp · and boundary layers; magnetospheric configuration and dynamics; solar wind · magnetosphere interactions)

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