Analysis of electron auroras based on the Monte Carlo method: Application to active electron arc auroras observed by the sounding rocket at Syowa Station

Onda, Ken; Ejiri, Masaki; Itikawa, Yukikazu

doi:10.1029/1999ja900323

Cited by 5 publications

(2 citation statements)

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“…Using the plasmaspheric model [ Rasmussen et al , ], together with the Volland‐Stern electric field and the Maynerd‐Chen potential model as a function of the K p index [ Jordanova and Miyoshi , ; Jordanova et al , ; Miyoshi et al , ], the electron density became N e =36 electrons/cm 3 , which indicated the value at the boundary of the plasmapause. The estimated resonant energies using the plasmaspheric model are in the range 0.81–2.2 keV, and its highest resonant energy can contribute to N

_{2}^{+}

first negative emissions [ Onda et al , ; Sergienko et al , ]. The bounce periods of resonant electrons along the geomagnetic field line are less than 4.4 s for N e <10 electrons/cm 3 and 5.1 s when using the plasmaspheric model, which are shorter than the observed repetition periods of 7.5–10 s. Other workers also reported repetition periods of PA unrelated to the bounce period of energetic electrons [ Yamamoto , ; Nishiyama et al , ].…”

Section: Observations and Discussionmentioning

confidence: 99%

A direct link between chorus emissions and pulsating aurora on timescales from milliseconds to minutes: A case study at subauroral latitudes

et al. 2015

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A correlation was observed between chorus emissions and pulsating aurora (PA) from observations at Athabasca (L≈4.3) in Canada at 9:00–9:20 UT on 7 February 2013, using an electron multiplying charge‐coupled device camera and a VLF loop antenna with sampling rates of 110 Hz and 100 kHz, respectively. Pulsating aurora having a quasiperiodic variation in luminosity and a few hertz modulation was observed together with chorus emissions consisting of a group of successive rising‐tone elements. The repetition period and modulation frequency of the PA are in good agreement with those of the modulated chorus. After 9:11 UT, the temporal features of the aurora became aperiodic PA of indistinct modulation. Simultaneously, the rising‐tone chorus turned into chorus emissions consisting of numerous rising‐tone elements. The equatorial geomagnetic field inhomogeneity calculated using the Tsyganenko 2002 model shows a decreasing trend during the period. This result is consistent with nonlinear wave growth theory having a small geomagnetic field inhomogeneity, which contributes to a decrease in the threshold amplitude to trigger discrete chorus elements. These observations show a close connection between chorus emissions and PA on timescales from milliseconds for generation of discrete chorus elements on the microphysics of wave‐particle interaction to minutes for the variations of the geomagnetic field inhomogeneity related with the substorm activity.

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_{2}^{+}

Section: Observations and Discussionmentioning

confidence: 99%

A direct link between chorus emissions and pulsating aurora on timescales from milliseconds to minutes: A case study at subauroral latitudes

et al. 2015

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“…While the former method is suitable for estimating integrated quantities, such as excitation and heating rates, the latter method is required for comparison with observed particle fluxes or for studying anisotropy. The final type of calculation is the Monte Carlo approach, which is a stochastic method based on the tracking of numerous individual particles (e.g., Onda et al 1999;Solomon 1993).…”

Section: Modeling Of Auroral Energy Depositionmentioning

confidence: 99%

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

2008

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We discuss here the energy deposition of solar FUV, EUV and X-ray photons, energetic auroral particles, and pickup ions. Photons and the photoelectrons that they produce may interact with thermospheric neutral species producing dissociation, ionization, excitation, and heating. The interaction of X-rays or keV electrons with atmospheric neutrals may produce core-ionized species, which may decay by the production of characteristic X-rays or Auger electrons. Energetic particles may precipitate into the atmosphere, and their collisions with atmospheric particles also produce ionization, excitation, and heating, and auroral emissions. Auroral energetic particles, like photoelectrons, interact with the atmospheric species through discrete collisions that produce ionization, excitation, and heating of the ambient electron population. Auroral particles are, however, not restricted to the sunlit regions. They originate outside the atmosphere and are more energetic than photoelectrons, especially at magnetized planets. The spectroscopic analysis of auroral emissions is discussed here, along with its relevance to precipitating particle diagnostics. Atmospheres can also be modified by the energy deposited by the incident pickup ions with energies of eV's to MeV's; these particles may be of solar wind origin, or from a magnetospheric plasma. When the modeling of the energy deposition of the plasma is calculated, the subsequent modeling of the atmospheric processes, such as chemistry, emission, and the fate of hot recoil particles produced is roughly independent of the exciting radiation. However, calculating the spatial distribution of the energy deposition versus depth into the atmosphere produced by an incident plasma is much more complex than is the calculation of the solar excitation profile. Here, the nature of the energy deposition processes by the incident plasma are described as is the fate of the hot recoil particles produced by exothermic chemistry and by knock-on collisions by the incident ions.

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Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

Fox

Galand

Johnson

Space Sciences Series of ISSI

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Analysis of electron auroras based on the Monte Carlo method: Application to active electron arc auroras observed by the sounding rocket at Syowa Station

Cited by 5 publications

References 29 publications

A direct link between chorus emissions and pulsating aurora on timescales from milliseconds to minutes: A case study at subauroral latitudes

A direct link between chorus emissions and pulsating aurora on timescales from milliseconds to minutes: A case study at subauroral latitudes

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

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