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Miroshnichenko, L. I.; Koning, C. A. de; Pérez-Enríquez, R.

doi:10.1023/a:1005279108725

Cited by 54 publications

(29 citation statements)

References 100 publications

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“…However, the shape of the SEP spectrum is typically very steep, and thus, the enhanced particle flux occurs mainly below $a few GeV/nucleon, with negligible fluxes beyond 100 GeV/nucleon. To investigate what effects such intense but short-lived particle enhancements may have on the venusian atmosphere, we have used measured spectra from an SEP event that occurred in October, 1989 -one of the most intense SEP events observed during the space age (Miroshnichenko et al, 2000). The ''worst week'' scenario corresponds to particle fluxes averaged over 180 h beginning at 1300 UTC on the 19th of October 1989, while the ''peak'' scenario corresponds to the peak fiveminute averaged fluxes as observed by the GOES spacecraft on October 20th, 1989 (Tylka et al, 1997).…”

Section: Resultsmentioning

confidence: 99%

Ionization of the venusian atmosphere from solar and galactic cosmic rays

Nordheim

Dartnell

Desorgher

et al. 2015

Icarus

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a b s t r a c tThe atmospheres of the terrestrial planets are exposed to solar and galactic cosmic rays, the most energetic of which are capable of affecting deep atmospheric layers through extensive nuclear and electromagnetic particle cascades. In the venusian atmosphere, cosmic rays are expected to be the dominant ionization source below $100 km altitude. While previous studies have considered the effect of cosmic ray ionization using approximate transport methods, we have for the first time performed full 3D Monte Carlo modeling of cosmic ray interaction with the venusian atmosphere, including the contribution of high-Z cosmic ray ions (Z = 1-28). Our predictions are similar to those of previous studies at the ionization peak near 63 km altitude, but are significantly different to these both above and below this altitude. The rate of atmospheric ionization is a fundamental atmospheric property and the results of this study have wide-reaching applications in topics including atmospheric electrical processes, cloud microphysics and atmospheric chemistry.

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Section: Resultsmentioning

confidence: 99%

Ionization of the venusian atmosphere from solar and galactic cosmic rays

Nordheim

Dartnell

Desorgher

et al. 2015

Icarus

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“…The appearance of the neutron-capture 2.22 MeV -ray line and the high ratio of the 2.22 MeV line to the 4Y7 MeV band were unexpected features of the occulted flare of the 1989 September 29 GLE (Vestrand & Forrest 1993;Miroshnichenko et al 2000). The likely location of the X9.8 soft X-ray flare was established as $W98…”

Section: Interplanetary Seps and Associated Flares Over The West Limbmentioning

confidence: 96%

Remote Sensing of Gamma‐Ray Emission from Solar Energetic Proton Interactions with the Solar Wind

Kahler¹,

Ragot²

2008

ApJ

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The properties of solar energetic particles (SEPs) in solar flares are studied through remote imaging in the radio, hard X-ray, and -ray energy ranges. However, the heliospheric SEP populations are observed only in situ by satellite measurements, which drastically limits our understanding of their spatial and temporal variations. Can those SEP populations be remotely imaged, as are the solar SEPs? We consider two possibilities for detecting faint -ray emission from SEP interactions with solar wind (SW) ions. First, the 6.13 and 4.44 MeV -ray lines of 16 O and 12 C, respectively, produced by the interactions of the SEPs from a large low-energy (E < 30 MeV) gradual event are calculated and found to be far below a detectable level. Then the expected 0 -decay -ray emission is calculated for the intense ground-level event (GLE) of 2005 January 20 and compared with (1) the observed Galactic and extragalactic background and (2) the expected near-solar emission from inverse-Compton scattering of solar photons by cosmic-ray electrons and from Galactic cosmic-ray collisions with the solar atmosphere. It appears feasible to detect the 0 -decay emission from that event with a detector of the size of the Large Area Telescope on GLAST. Earlier 1982 and 1991 flare observations of long-duration (hours) 0 -decays were attributed to E > 300 MeV protons captured in strong coronal loops, but we suggest that the observed emission was due to SEP-SW collisions following shock acceleration on open field lines.

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“…References. (1) Reeves et al (1992); Lario et al (2001); (2) Shea and Smart (1993); Kocharov et al (1995); (3) Gopalswamy et al 2010;2012a;(4) Mewaldt et al (2012); (5) Cliver et al (1993); Miroschnichenko et al (2000); (6) Liu et al (2008); (7) Gopalswamy et al (2014a) Table 1 lists these ESP and GLE events along with the >10 MeV SEP fluxes, which were in the range 2000 to 5000 pfu. The SEP fluxes were measures as the peak value before the onset of the associated ESP event.…”

Section: Event Intensitymentioning

confidence: 99%

The 2012 July 23 Backside Eruption: An Extreme Energetic Particle Event?

Gopalswamy

Yashiro

Thakur

et al. 2016

ApJ

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The backside coronal mass ejection (CME) of 2012 July 23 had a short Sun to Earth shock transit time (18.5 hours). The associated solar energetic particle (SEP) event had a >10 MeV proton flux peaking at ~5000 pfu, and the energetic storm particle (ESP) event was an order of magnitude larger, making it the most intense event in the space era at these energies. By a detailed analysis of the CME, shock, and SEP characteristics, we find that the July 23 event is consistent with a high-energy SEP event (accelerating particles to GeV energies). The time of maximum and fluence spectra in the range 10-100 MeV were very hard, similar to those of ground level enhancement (GLE) events. We found a hierarchical relationship between the CME initial speeds and the fluence spectral indices: CMEs with low initial speeds had SEP events with the softest spectra, while those with highest initial speeds had SEP events with the hardest spectra. CMEs attaining intermediate speeds result in moderately hard spectra. The July 23 event was in the group of hard-spectrum events. During the July 23 event, the shock speed (>2000 km s -1 ), the initial acceleration (~1.70 km s -2 ), and the shock formation height (~1.5 solar radii) were all typical of GLE events. The associated type II burst had emission components from metric to kilometric wavelengths suggesting a strong shock. These observation confirm that the 2012 July 23 event is likely to be an extreme event in terms of the energetic particles it accelerated.

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Cited by 54 publications

References 100 publications

Ionization of the venusian atmosphere from solar and galactic cosmic rays

Ionization of the venusian atmosphere from solar and galactic cosmic rays

Remote Sensing of Gamma‐Ray Emission from Solar Energetic Proton Interactions with the Solar Wind

The 2012 July 23 Backside Eruption: An Extreme Energetic Particle Event?

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