Plasma Waves Around Venus and Mars

Yadav, Vipin K.

doi:10.1080/02564602.2020.1819889

Cited by 17 publications

(14 citation statements)

References 102 publications

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“…In case of zero flows, the electric field amplitude drops to the range of (∼7.63-11.52 mV/m). The estimated electric field values where the streaming effect is excluded and the observed electric fields in the Venusian ionosphere by PVO are in agreement [19]. Also we found that greatest electric field amplitude corresponds to the lowest altitude for both cases.…”

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confidence: 86%

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Effect of streaming velocity, magnetic field, and higher-order correction on the nature of ion acoustic solitons in the Venusian ionosphere

2021

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Propagation properties of weakly nonlinear ion acoustic waves are investigated in a plasma at the Venusian ionosphere. The plasma model consists of two positive cold ions (oxygen O + and hydrogen H +), as well as isothermal electrons. The basic set of fluid equations is reduced to Zakharov-Kuznetsov (ZK) equation and linear inhomogeneous ZK-type equation (LIZKT) equation. The renormalization method is adopted to obtain solitary solutions of both equations. The effects of plasma parameters and higher-order correction on the nature of the solitary waves are investigated. It is found that the wave phase velocity is supersonic, which is in agreement with the observations. Furthermore, the higher-order correction enlarges the soliton amplitude, which is suitable for describing the solitary waves when the wave amplitude grows.

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confidence: 86%

“…IAW is one of the plasma modes observed in the Venusian environment. Many modes are also detected, such as ion cyclotron waves, Alfvenic waves, electron acoustic waves, whistler, and mirror modes [14][15][16][17][18][19]. Extensive work is devoted to interpret the different observed plasma phenomena at the Venusian environment.…”

Section: Introductionmentioning

confidence: 99%

Effect of streaming velocity, magnetic field, and higher-order correction on the nature of ion acoustic solitons in the Venusian ionosphere

2021

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“…Interestingly the rate of escape of the ions in the Venusian ionosphere, estimated by the various authors [45][46][47] based on the observations by ASPERA-4 and in distinct energy spectra are quite similar in their form and is in tune with this present investigation. It may be also possible that some shock like nonlinear resonant mechanisms can accelerate the process [48][49][50][51][52]…”

Section: An Possible Way Of the Particle Escape Processsupporting

confidence: 86%

Two-stream plasma instability as a potential mechanism for particle escape from the Venusian ionosphere

et al. 2022

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In this work we investigate the possibility of two-stream instability in the Venusian atmosphere to lead to momentum transfer to subsequent escape of Hydrogen and Oxygen ions from the ionosphere. We employ the hydrodynamic model and obtain the linear dispersion relation from which the two-stream instability is studied. Further the interaction of solar wind with the ions of Venus ionosphere from which the instability sets in, has been studied with the data from ASPERA-4 of Venus Express (VEX). The data supports the fact that the two-stream instability can provide sufficient energy to accelerate ions to escape velocity of the planet.

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“…Thus, the Doppler shifted frequencies corresponding to the peaks in the power spectra in the plasma rest frame compare well with the PVO observations of ion-acoustic waves with frequencies 5.4 kHz. The ion-acoustic solitons that are predicted by our model can explain the PVO observation of ion-acoustic waves in the frequency range of 100 Hz, 730 Hz, and 5.4 kHz (Scarf et al 1979;Strangeway 1991;Yadav 2020) with an electric field amplitude of 10 −1 -10 −2 mV m −1 . In addition, the model (see the H + ion-mode in Tables 2 and 3) can be relevant in explaining the Solar Orbiter observation of ESWs with a peakto-peak electric field amplitude of a few mV m −1 with a characteristic timescale of ∼0.5 ms in the magnetosheath region (Hadid et al 2021).…”

Section: Numerical Results and Discussionmentioning

confidence: 53%

“…The magnetosheath region between the shock and the ionopause comprises thermalized subsonic solar wind plasma, which is associated with piled-up and draped IMF (Futaana et al 2017). The dynamics of Venus's induced magnetosphere rely to a large extent on the solar activity (Zhang et al 2007;Yadav 2020).…”

Section: Introductionmentioning

confidence: 99%

Electrostatic Solitary Waves in the Venusian Ionosphere Pervaded by the Solar Wind: A Theoretical Perspective

Rubia

Singh

Lakhina

et al. 2023

ApJ

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Electrostatic solitary waves (ESWs) in the Venusian ionosphere that are impinged by the solar wind are investigated using a homogeneous, collisionless, and magnetized multicomponent plasma consisting of Venusian H+ and O+ ions, Maxwellian Venusian electrons and streaming solar wind protons, and suprathermal electrons following κ − distribution. The model supports the propagation of positive potential slow O+ and H+ ion-acoustic solitons. The evolution and properties of the solitons occurring in two sectors, viz., dawn-dusk and noon-midnight sector of the Venus ionosphere at an altitude of (200–2000) km, are studied. The theoretical model predicts positive potential solitons with amplitude ∼(0.067–56) mV, width ∼(1.7–53.21) m, and velocity ∼(1.48–8.33) km s−1. The bipolar soliton electric field has amplitude ∼(0.03–27.67) mV m−1 with time duration ∼(0.34–22) ms. These bipolar electric field pulses when Fourier transformed to the frequency domain occur as a broadband electrostatic noise, with frequency varying in the range of ∼9.78 Hz–8.77 kHz. Our results can explain the observed electrostatic waves in the frequency range of 100 Hz–5.4 kHz in the Venus ionosphere by the Pioneer Venus Orbiter mission. The model can also be relevant in explaining the recent observation of ESWs in the Venus magnetosheath by the Solar Orbiter during its first gravity assist maneuver of Venus.

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Plasma Waves Around Venus and Mars

Cited by 17 publications

References 102 publications

Effect of streaming velocity, magnetic field, and higher-order correction on the nature of ion acoustic solitons in the Venusian ionosphere

Effect of streaming velocity, magnetic field, and higher-order correction on the nature of ion acoustic solitons in the Venusian ionosphere

Two-stream plasma instability as a potential mechanism for particle escape from the Venusian ionosphere

Electrostatic Solitary Waves in the Venusian Ionosphere Pervaded by the Solar Wind: A Theoretical Perspective

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