Resonant heating of the ionospheric plasma by powerful radiopulses aboard the Intercosmos-19 and Cosmos-1809 satellites

Shuiskaya, F.K.; Galperin, Yu. I.; Serov, A. O.; Baranets, N.V.; Kushnerevsky, Yu.V.; Vasilev, G. V.; Пулинец, С. А.; Fligel, M. D.; Selegey, V.V.

doi:10.1016/0032-0633(90)90081-z

Cited by 22 publications

(12 citation statements)

References 6 publications

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“…Data from the monostatic radio sounders have been analyzed using nonlinear plasma turbulence concepts. [14][15][16] SAEs observed monostatically at pumping frequencies near and above f c and f p are interpreted as the result of collapse of Langmuir or Bernstein wave cavitons.…”

Section: B Plasma Nonlinearities Strong Turbulence and Heatingmentioning

confidence: 99%

“…16 To locate the region of validity of this theory, it is assumed that ponderomotive effects force the rf sheath out to a radius r where the ambient thermal energy density nT equals the electrostatic energy density in the near rf field 0 E 0 2 /4. Approximating 13 the very near field magnitude E ϭV 0 /4r and solving for E…”

Section: B Plasma Nonlinearities Strong Turbulence and Heatingmentioning

confidence: 99%

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OEDIPUS-C observations of electrons accelerated by radio frequency fields at whistler-mode frequencies

et al. 1999

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Simultaneous measurements of transmitted 500 kHz electric fields and of electron fluxes nonlinearly energized by those fields were made during the ionospheric flight of the rocket double payload OEDIPUS C. Given the local plasma parameters, 500 kHz corresponded to the whistler mode of cold-plasma propagation. As the separation between each payload end increased from 153 to 537 m, enhanced electron fluxes were detected at energies up to 20 keV, at the receiver end of the tether. Rf (radio frequency) electric fields created by the OEDIPUS-C transmitter have been computed for positions close to the whistler-mode group resonance cone and also for locations very close to the active dipoles. Test-particle trajectory tracings show that linear acceleration can account for the energy increases of electrons with starting energies up to about 100 eV. Neither resonant field-particle interactions of background energetic electrons nor strong turbulence of the background thermal particles explain the creation of sounder-accelerated electrons at 1–10 keV. The calculated magnitudes of the very near potentials, up to 550 V, point to acceleration by intense fields in the rf sheath region.

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Section: B Plasma Nonlinearities Strong Turbulence and Heatingmentioning

confidence: 99%

Section: B Plasma Nonlinearities Strong Turbulence and Heatingmentioning

confidence: 99%

OEDIPUS-C observations of electrons accelerated by radio frequency fields at whistler-mode frequencies

et al. 1999

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“…SAE electrons detected in a plasma with low electron density (typically on the nightside of the Martian ionosphere) are presumably generated by nonlinear wave-wave and wave-particle interaction (Pulinets and Selegei, 1986;Shuiskaya et al, 1990), while SAE electrons detected in the dense plasma on the dayside are accelerated by sounder induced spacecraft potential (James, 1983(James, , 1987. This study showed that intense fluxes (up to 5 · 10 6 particles/eV/s/cm 2 /str) of SAE can be created even in plasmas with very weak magnetic field (B <4 nT).…”

Section: Resultsmentioning

confidence: 99%

“…The suggested explanation involved cyclotron heating of the plasma surrounding the satellite by the high-power transmitter pulse with subsequent development of the Haris instability (Oya, 1971) or nonlinear Landau damping (Kiwamoto and Benson, 1979) that produces the observed diffuse echoes. Due to the fact that SAP are typically detected when the frequency of the transmitter is close to one of the fundamental plasma resonances, several models based on resonant wave-particle and wave-wave interactions were suggested (see James et al, 1999, Shuiskaya et al, 1990, and Voshchepynets et al, 2019, for a review). Due to the fact that SAP are typically detected when the frequency of the transmitter is close to one of the fundamental plasma resonances, several models based on resonant wave-particle and wave-wave interactions were suggested (see James et al, 1999, Shuiskaya et al, 1990, and Voshchepynets et al, 2019, for a review).…”

Section: Discussionmentioning

confidence: 99%

Observations of Sounder Accelerated Electrons by Mars Express

et al. 2020

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The electron sensor of the Analyzer of Space Plasmas and Energetic Atoms experiment detects accelerated electrons during pulses of radio emissions from the powerful topside sounder: the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) on board the Mars Express spacecraft. Accelerated electrons are observed at energies up to 400 eV at the times when MARSIS transmits at a frequency between the local plasma frequency and its harmonics (up to 4 times the plasma frequency). When the electron density and magnetic field strength are low (∼ 10 3 cm −3 , ∼ 10 nT), the accelerated electrons are almost monoenergetic electron beams. An increase in density and magnetic field (∼ 3 · 10 3 cm −3 , ∼ 50 nT) leads to substantial broadening of the energy spectrum of the accelerated electrons. It is concluded that in the latter case, electrons are accelerated by the variable spacecraft potential resulting from the imbalance of the electron and ion currents to the MARSIS antenna during transmission.

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“…The strongest electron heating has been observed when the emission frequency is in the same frequency interval as some eigenmode of the plasma, such as electron whistlers or electron Bernstein modes, suggesting that these eigenmodes are involved in the electron heating mechanism. The electrons could be heated by nonlinear wave‐particle interactions [ Pulinets and Selegey , 1986; Shuiskaya et al , 1990]; however, James et al [1999] argued that this process may not work for the OC sounder. They arrived at this conclusion by considering strong Langmuir turbulence described within the framework of the Zakharov equations, which ignored a possible increase of the electron thermal energy density due to the interaction of the electrons with the vacuum potential, the very near field (VNF), of the antenna or linearly damped transient wave modes which we here call the near field.…”

Section: Introductionmentioning

confidence: 99%

Particle‐in‐cell simulations of electron acceleration by a simple capacitative antenna in collisionless plasma

et al. 2004

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[1] We examine the electron acceleration by a localized electrostatic potential oscillating at high frequencies by means of particle-in-cell (PIC) simulations, in which we apply oscillating electric fields to two neighboring simulation cells. We derive an analytic model for the direct electron heating by the externally driven antenna electric field, and we confirm that it approximates well the electron heating obtained in the simulations. In the simulations, transient waves accelerate electrons in a sheath surrounding the antenna. This increases the Larmor radii of the electrons close to the antenna, and more electrons can reach the antenna location to interact with the externally driven fields. The resulting hot electron sheath is dense enough to support strong waves that produce high-energy sounder-accelerated electrons (SAEs) by their nonlinear interaction with the ambient electrons. By increasing the emission amplitudes in our simulations to values that are representative for the ones of the sounder on board the OEDIPUS C (OC) satellites, we obtain electron acceleration into the energy range which is comparable to the 20 keV energies of the SAE observed by the OC mission. The emission also triggers stable electrostatic waves oscillating at frequencies close to the first harmonic of the electron cyclotron frequency. We find this to be an encouraging first step of examining SAE generation with kinetic numerical simulation codes.

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Resonant heating of the ionospheric plasma by powerful radiopulses aboard the Intercosmos-19 and Cosmos-1809 satellites

Cited by 22 publications

References 6 publications

OEDIPUS-C observations of electrons accelerated by radio frequency fields at whistler-mode frequencies

OEDIPUS-C observations of electrons accelerated by radio frequency fields at whistler-mode frequencies

Observations of Sounder Accelerated Electrons by Mars Express

Particle‐in‐cell simulations of electron acceleration by a simple capacitative antenna in collisionless plasma

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