Numerical investigation of the surfatron acceleration efficiency of charged particles by wave packets in space plasma

Shkevov, Rumen; Ерохин, Н. С.; Mikhailovskaya, L. A.; Zol’nikova, N. N.

doi:10.1016/j.jastp.2012.07.001

Cited by 5 publications

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“…3 and E OUT ≅ 1.40 GeV. In earlier works [Erokhin, et al, 1987, 1991, Loznikov, et al, 2010, Shkevov, et al 2013 was shown that the most effective particle acceleration takes place in the case when particle capture occurs on the left side of the wave packet, but from the other hand, the particle capture probability is higher when the charged particle is situated in the center of the wave packet structure, similar to the problem discussed in current paper.For the correct estimation of the particle energy growth, it is needed to calculate the relativistic factor value before and after surfatron acceleration period. As it was mentioned above, electron initial relativistic factor is γ (0) = 1.075 from where is received E INI ≅ 0.55 MeV resulting electron initial energy.…”

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“…Nonlinear effects from the interaction of the accelerating wave with the plasma are insignificant, if the wave amplitude E 0 is significantly lower than the field of relativistic nonlinearity, i.e. on the condition σ 2 << 1 [Erokhin, et al, 1987, 2007, Shkevov, et al, 2013.Let us consider the relativistic equations of motion of electrons with mass m e in the field of an electromagnetic wave E x = E 0 cos Ψ, Ψ = ωt -kx. It is supposed that β β β β = v/c, τ = ωt dimensionless time, ξ = ωx /c.…”

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“…The typical packet size in k-space is β g = v g / c << 1, β g -dimensionless wave packet group speed. For the wave phase on the particle trajectory, using (1), (2) and (3) we have the equation [Katsouleas and Dawson, 1983, Erokhin, et al, 1987, Kichigin, 1995, Shkevov, et al, 2013:where ρ = ωL / c >> 1, E x (x, t) is given above, β p0 = ω 0 /c k 0 , r 0 = γ β y is the initial particle momentum component along wave front and the integral of motion J = γ β y + u 0 β p0 (Ψ 0 -τ) is taken into account. There exists second integral of motion γ β z = const ≡ h. The electron velocity component β x in (4) is given by the expression β x = β p0 [1 -( dΨ 0 / dτ ) ].…”

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Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

Danov¹,

Georgieva²,

Kirov³

2018

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IIn ns st tr ru um me en nt ta at ti io on n f fo or r S Sp pa ac ce e W We ea at th he er r D Da at ta a P Pr ro oc ce es ss si in ng g a an nd d M Mo on ni it to or ri in ng g Sadovnichii V.A., Panasyuk M.I., Lipunov V.M., Bogomolov A.V., Bogomolov V.V. et.al. Monitoring of space radiation and other hazards in multi-satellite project `Universat-SOCRAT 123 S. Yerin, A. Stanislavsky, I. Bubnov, A. Konovalenko, P. Tokarsky, V. Zakharenko Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths 129 M.M. Kalinichenko, O.O. Konovalenko, A.I. Brazhenko, N.V Šterc, D. Roša, D. Maričić, D. Hržina, I. Romštajn, A. Chilingarian, T. Karapetyan, D. Cafuta, M. Horvat Abstract.A powerful series of solar flares is occurred in the minimum of solar activity 2017 September 4 -11 over the active region AR12673. This active region produces two large and many small flares. The flare X8.2 is followed by solar cosmic rays. The active region at that time is situated on the back side of the Sun disk behind the Western limb. The front of the accelerated protons flux arrives to the Earth with the delay not exceeding the proton flight time from the Sun. Such proton propagation can occur only along the lines of the interplanetary magnetic field. There is no reason to believe that the mechanisms of cosmic ray acceleration on the Sun and other stars are of different nature. The flux of relativistic electrons does not show any connection with the solar cosmic rays. The results of SDO spacecraft are used to study the pre-flare state and flare development. The source of flare radiation in the spectral lines of the highly ionized irons FeXXIV and FeXXIII is observed in the corona. The emission of these spectral lines sharp increases during flare X-ray radiation appearing. The energy release of a flare occurs in the corona above an active region. The temperature in the flare is greater than 20 MK. The size of the hot plasma cloud is ~10 10 cm. IntroductionThe solar constant indicates an amazing stability of the solar thermonuclear reactor. The solar constant is 1367 W/m 2 . The change of the solar constant during the 11-year cycle of solar activity does not exceed ~10 -3 . Against the backdrop of this amazing stability of the Sun's work the big solar flares are observed several times per a year. The flare energy release takes place in the corona over a complex active region with a magnetic flux greater than 10 22Mx. The energy of a solar flare can exceed 10 32 erg. The flare duration is from 10 to 100 minutes. The flare is a manifestation of a number of physical processes, including X-ray radiation, the ejection of the corona substance and proton acceleration to the relativistic energy of not less than 20 GeV [Balabin et al., 2005; Podgorny and Podgorny, 2016].The Sun is the only astronomical object that generates proton pulses with the relativistic energy. The solar proton acceleration takes place along a singular line of the current sheet above an active region. The electric ...

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