Study of inertial kinetic Alfven waves around cusp region

Agarwal, Priyanka; Varma, P.; Tiwari, Meenakshi

doi:10.1016/j.pss.2010.11.006

Cited by 12 publications

(8 citation statements)

References 39 publications

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“…As here we have assumed that the plasma composed of multi-ions (H + , He + , O + ), so the density variation of each ion will also show its effect on wave nature. The expression ( 16) is similar to result obtained by Agarwal et al (2011), if multiions effect is ignored.…”

Section: Growth/damping Ratesupporting

confidence: 81%

“…( 13), it is clear that the frequency of inertial Alfvén wave is influenced by the plasma frequency of electrons, cyclotron frequency and plasma frequency of H + , He + and O + ions. If contribution of He + and O + ions are neglected, we recover the expression derive in reference (Agarwal et al 2011).…”

Section: Dispersion Relationmentioning

confidence: 98%

“…The net growth/damping length from Eqs. ( 26) and ( 28) reduces to the growth/damping length expression evaluated by Agarwal et al (2011).…”

Section: Perpendicular Growth/damping Lengthmentioning

confidence: 99%

“…These waves have been rigorously investigated considering Maxwellian distribution function of electrons and ions in AAR as well as laboratory plasma (Thompson and Lysak 1996;Chaston et al 2002;Dubinin et al 2005;Watt et al 2006;Rankin 2007, 2008;Parks et al 2015). Agarwal et al (2011Agarwal et al ( , 2014 have investigated frequency and damping rate of IAW in cusp and plasma sheet boundary layer region considering finite ion gyroradius effect. Recently, Kumar et al (2015) have developed simulation model to investigate the density cavitation by IAW using FAST observations at 1700 km altitude.…”

Section: Introductionmentioning

confidence: 99%

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Inertial Alfvén waves in auroral acceleration region with H+, He+ and O+ ions plasma

Tamrakar

Varma

Tiwari

2019

Astrophys Space Sci

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The propagation of inertial Alfvén wave is investigated in cold, low-β, homogeneous and bi-Maxwellian plasma consisting of multi-ions (H + , He + and O + ). Kinetic approach is adopted to derive the dispersion relation, damping rate, group velocity and growth/ damping length of the wave. Figures are exhibited with respect to ck ⊥ /ω pe . Effects of density variation with multi-ions are analysed on frequency, damping rate, parallel and perpendicular components of group velocity and growth/ damping length of the inertial Alfvén wave. It is found that varying densities of multi-ions significantly influence the frequency, damping rate and group velocity of inertial Alfvén wave. The wave frequency is observed between 0.5 to 18 s −1 pertaining to observational data. The increasing density of heavy ions reduces the frequency of waves. The presence of He + and O + enhances the damping of wave showing more transfer of energy from wave to particles leading to increase in electron acceleration. The order of parallel and perpendicular group velocity is found to be 10 9 cm/s and 10 5 cm/s respectively. Maximum perpendicular growth length is observed corresponding to the minimum damping rate of wave at ck ⊥ /ω pe < 1, signifying the dynamics in transverse direction to the magnetic field which are more significant in the present analysis. The parameters relevant to auroral acceleration region are used for graphical analysis. The applications of present study may be towards the electron acceleration in the dynamics of auroral acceleration region consisting of heavy ions in background plasma.

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Section: Growth/damping Ratesupporting

confidence: 81%

Section: Dispersion Relationmentioning

confidence: 98%

“…The net growth/damping length from Eqs. ( 26) and ( 28) reduces to the growth/damping length expression evaluated by Agarwal et al (2011).…”

Section: Perpendicular Growth/damping Lengthmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Inertial Alfvén waves in auroral acceleration region with H+, He+ and O+ ions plasma

Tamrakar

Varma

Tiwari

2019

Astrophys Space Sci

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“…This should be distinguished from the standard inertial Alfvén wave derived under the conditions β e ≪ m e /m i and β i ≪ 1 (e.g., Lysak & Lotko 1996), which are not satisfied here. Note also that the term "inertial kinetic Alfvén wave" has occasionally been applied to the standard inertial Alfvén wave (Shukla et al 2009;Agarwal et al 2011), although the conditions assumed in these works are essentially the same as in Lysak & Lotko (1996) and different from those leading to Equation (5).…”

Section: Nature Of Fluctuations At Kd Ementioning

confidence: 99%

Nature of Kinetic Scale Turbulence in the Earth's Magnetosheath

Chen

Boldyrev

2017

ApJ

147

167

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We present a combined observational and theoretical analysis to investigate the nature of plasma turbulence at kinetic scales in the Earth's magnetosheath. In the first decade of the kinetic range, just below the ion gyroscale, the turbulence was found to be similar to that in the upstream solar wind: predominantly anisotropic, lowfrequency and kinetic Alfvén in nature. A key difference, however, is that the magnetosheath ions are typically much hotter than the electrons, T i ≫ T e , which, together with β i ∼ 1, leads to a change in behaviour in the second decade, close to electron scales. The turbulence here is characterised by an increased magnetic compressibility, following a mode we term the inertial kinetic Alfvén wave, and a steeper spectrum of magnetic fluctuations, consistent with the prediction E B (k ⊥ ) ∝ k −11/3 ⊥ that we obtain from a set of nonlinear equations. This regime of plasma turbulence may also be relevant for other astrophysical environments with T i ≫ T e , such as the solar corona, hot accretion flows, and regions downstream of collisionless shocks.

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