Electrostatic waves driven by electron beam in lunar wake plasma

Sreeraj, T.; Singh, S. V.; Lakhina, G. S.

doi:10.1063/1.5032141

Cited by 13 publications

(15 citation statements)

References 34 publications

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“…c a and c T are strongly modified by the radiation pressure effects. Now substituting equation (14) into equation (12) and using identity…”

Section: Governing Plasma Model and Formalismmentioning

confidence: 99%

“…Influence of plasma parameters on the low frequency ion cyclotron and ion acoustic waves are investigated in [13]. More recently low frequency modes observed in lunar wake are focused in [14], kinetic Alfven waves excited by ion beam in the Earth's magnetosphere was studied in [15] to investigate the influence of plasma parameters on growth of low frequency waves, further it was shown in [16] that plasma parameters have significant signature on the helium cyclotron instability.…”

Section: Introductionmentioning

confidence: 99%

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Low-frequency plasma waves in a radiative dusty magnetoplasma

et al. 2020

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The impact of electromagnetic (thermal) radiation on the dispersive low-frequency waves is examined in a radiative dusty magnetoplasma. For this purpose, a magneto-hydrodynamic model along with the Maxwell equations is employed to describe the three-component radiative dusty plasma that contains inertialess electrons, dynamical positive ions and negatively charged static dust particulates. The behavior of the electrostatic and electromagnetic waves significantly changes in a plasma medium when a radiation pressure is taken into consideration, as compared to the waves in vacuum. After seeking a plane wave solution, a general dispersion relation is obtained to investigate different limiting cases of the low-frequency modes propagating parallel, perpendicular and oblique to the external magnetic field direction both analytically and numerically. The calculations reveal that the usual thermal and acoustic speeds (cT, ca) do not remain constant even if the temperature is kept constant, because of the radiation pressure which strongly depends on the equilibrium number density as well. The present results may prove a useful understanding for the new features of the dispersive dust-ion-acoustic and compressional Alfven waves in astrophysical dusty magnetoplasmas.

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“…c a and c T are strongly modified by the radiation pressure effects. Now substituting equation (14) into equation (12) and using identity…”

Section: Governing Plasma Model and Formalismmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Low-frequency plasma waves in a radiative dusty magnetoplasma

et al. 2020

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“…Solar wind pours out in space roughly 10 9 kg/s or one million tonnes of charged particles per second, within an energy range 1.5−10 keV and speed ≈ 250 to 750 km/s (Meyer-Vernet 2007). Interaction between solar wind and planetary objects explains how the structure, composition, chemistry, and energy change in theses environments (El-Labany et al 2006;Xi et al 2013;Popel et al 2013;Popel et al 2015;Popel et al 2017;Lakhina & Singh 2015;Sreeraj et al 2018;Moslem et al 2018). Of particular interest is the atmospheric escape from planets without a global magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Ionospheric losses of Venus in the solar wind

Salem

Moslem

Lazar

et al. 2020

Advances in Space Research

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The nature of ionospheric losses from Venus is of essential importance for understanding the ionosphere dynamics of this unmagnetized planet. A plausible mechanism that can explain the escape of charged particles involves the solar wind interaction with the upper atmospheric layers of Venus. The hydrodynamic approach proposed for plasma expansion in the present study comprises two populations of positive ions and the neutralizing electrons, which interact with the solar wind electrons and protons. The fluid equations describing the plasma are solved numerically using a self-similar approach. The behavior of plasma density, velocity, and electric potential, as well as their reliance upon solar wind parameters have been examined. It is found that for noon midnight sites, the oxygen ion-to-electron relative density may be the main factor to enhance the ionic loss. However, the other parameters, like hydrogen density and solar wind density and velocity seem to do not stimulate the runaway ions. For lower dawn-dusk region, the plasma are composed of hydrogen and oxygen ions as well as electrons, but for higher altitudes only hydrogen ions and electrons are encountered. All ionic densities play an important role either to reduce or boost the ionic loss. The streaming solar wind velocity has no effect on the plasma escaping for lower altitudes, but it reduces the expansion at higher altitudes.

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“…Through a nonlinear analysis of four component plasma modeled by hot protons, hot heavier ions (α-particles, He ++ ), electron beam, and superthermal electrons following kappa distribution, Rubia et al [26] have explained the low frequency part (<0.01f pe ) of observed spectrum of electrostatic waves in lunar wake [25]. Sreeraj et al [27] have undertaken linear analysis of the model proposed by Rubia et al [26] and have shown that fast and slow ion acoustic modes are driven unstable when a finite electron beam is introduced into the system. These are electron beam driven fast and slow ion-acoustic modes.…”

Section: Introductionmentioning

confidence: 99%

Linear analysis of electrostatic waves in the lunar wake plasma

Sreeraj¹,

Singh²,

Lakhina³

2020

Phys. Scr.

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Propagation characteristics of electrostatic electron and ion cyclotron waves, ion- and electron- acoustic waves in a four-component magnetized plasma comprising of protons, doubly charged Helium ions, beam electrons and superthermal electrons following a kappa distribution are presented. The model supports 12 plasma modes: two electron cyclotron (modes 1 and 12), two electron acoustic (modes 2 and 11), two fast ion acoustic (modes 3 and 10), two slow ion acoustic (modes 4 and 9), two proton cyclotron (modes 5 and 8) and two Helium cyclotron (modes 6 and 7). At parallel propagation, with increase in electron beam speed, mode 11 first merges with slow ion acoustic mode 4 and then with fast ion acoustic mode 3 and drives them unstable. For oblique propagation and without the electron streaming, coupling of various plasma modes occurs and it weakens with increase in the angle of propagation. Further, for oblique propagation with finite electron beam velocity, merging as well as coupling of various plasma modes are observed. Growth rates as well as wave numbers of the excited slow and fast ion acoustic modes are much smaller in magnetized plasma than in an unmagnetized one. The results are relevant to observations of electrostatic waves in the lunar wake.

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Electrostatic waves driven by electron beam in lunar wake plasma

Cited by 13 publications

References 34 publications

Low-frequency plasma waves in a radiative dusty magnetoplasma

Low-frequency plasma waves in a radiative dusty magnetoplasma

Ionospheric losses of Venus in the solar wind

Linear analysis of electrostatic waves in the lunar wake plasma

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