Ground level enhancements of solar cosmic rays during the last three solar cycles

Белов, А. В.; Eroshenko, E.; Kryakunova, O. N.; Kurt, V. G.; Yanke, V. G.

doi:10.1134/s0016793210010032

Cited by 52 publications

(49 citation statements)

References 16 publications

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“…This event was the second strongest ever observed by the ground-based NMs with an increase exceeding 20-fold in 5-min data (54-fold in 1-min data) of the South Pole NM (Mewaldt, 2006;Plainaki et al, 2007;Belov et al, 2010). It was characterized by a shortlasting anisotropic component with a very hard spectrum followed by prolonged isotropic emission of SEPs with a softer spectrum (McCracken et al, 2008).…”

Section: Sep Event Of 20 January 2005mentioning

confidence: 97%

Ionization effect of solar particle GLE events in low and middle atmosphere

Kovaltsov²,

et al. 2011

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Abstract. Using a new reconstruction of the solar proton energy spectra for Ground Level Enhancement (GLE) events, based on fits to measurements from ground-based and satellite-borne instruments covering a wide energy range, we quantitatively evaluate the possible ionization effects in the low and middle atmosphere for 58 out of the 66 GLE events recorded by the world-wide neutron monitor network since 1956. The ionization computations are based on the numerical 3D CRAC:CRII model. A table of the ionization effect caused by the GLE events at different atmospheric heights is provided. It is shown that the direct ionization effect is negligible or even negative, due to the accompanying Forbush decreases, in all low-and mid-latitude regions. The ionization effect is important only in the polar atmosphere, where it can be dramatic in the middle and upper atmosphere (above 30 km) during major GLE events.

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Section: Sep Event Of 20 January 2005mentioning

confidence: 97%

Ionization effect of solar particle GLE events in low and middle atmosphere

Kovaltsov²,

et al. 2011

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“…The purpose of this study is to present two new high energy solar Active region c GLE onset d 58 40 23 1998-08-24 2150 2212 N35E09 8307 2250 59 41 23 2000-07-14 1003 1024 N22W07 9077 1030 60 42 23 2001-04-15 1319 1350 S20W84 9415 1400 61 42 23 2001-04-18 0211 0214 W115 9415 0235 62 43 23 2001-11-04 1603 1620 N07W19 9684 1700 63 44 23 2001-12-26 0432 0540 N08W54 9742 0530 64 45 23 2002-08-24 0049 0112 S02W81 10069 0120 65 46 23 2003-10-28 0951 1110 S16E08 10486 1120 66 46 23 2003-10-29 2037 2049 S15W02 10486 2105 67 46 Notes. (a) GLE1-32: Ha onset and maximum from Cliver et al (1982); GLE33-69: X-ray onset and maximum from Belov et al (2010); GLE70: X-ray onset and maximum from NOAA STP X-ray database; GLE71: X-ray onset and maximum from Gopalswamy et al (2013). ( Dodson and Hedeman (1969).…”

Section: Introductionmentioning

confidence: 99%

Two solar proton fluence models based on ground level enhancement observations

Raukunen

Vainio

Tylka

et al. 2018

J. Space Weather Space Clim.

158

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-Solar energetic particles (SEPs) constitute an important component of the radiation environment in interplanetary space. Accurate modeling of SEP events is crucial for the mitigation of radiation hazards in spacecraft design. In this study we present two new statistical models of high energy solar proton fluences based on ground level enhancement (GLE) observations during solar cycles 19-24. As the basis of our modeling, we utilize a four parameter double power law function (known as the Band function) fits to integral GLE fluence spectra in rigidity. In the first model, the integral and differential fluences for protons with energies between 10 MeV and 1 GeV are calculated using the fits, and the distributions of the fluences at certain energies are modeled with an exponentially cut-off power law function. In the second model, we use a more advanced methodology: by investigating the distributions and relationships of the spectral fit parameters we find that they can be modeled as two independent and two dependent variables. Therefore, instead of modeling the fluences separately at different energies, we can model the shape of the fluence spectrum. We present examples of modeling results and show that the two methodologies agree well except for a short mission duration (1 year) at low confidence level. We also show that there is a reasonable agreement between our models and three well-known solar proton models (JPL, ESP and SEPEM), despite the differences in both the modeling methodologies and the data used to construct the models.

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“…GLEs are produced in conjunction with intense flares and extremely fast coronal mass ejections (CMEs; Belov et al 2010;Gopalswamy et al 2012). The acceleration mechanisms are thought to be related to the flare, which usually means magnetic reconnection, or to the shock wave generated by the CME.…”

Section: Introductionmentioning

confidence: 99%

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

Klein

Masson

Bouratzis

et al. 2014

A&A

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Context. The highest energies of solar energetic nucleons detected in space or through gamma-ray emission in the solar atmosphere are in the GeV range. Where and how the particles are accelerated is still controversial. Aims. We search for observational information on the location and nature of the acceleration region(s) by comparing the timing of relativistic protons detected on Earth and radiative signatures in the solar atmosphere during the particularly well-observed 2005 Jan. 20 event.Methods. This investigation focusses on the post-impulsive flare phase, where a second peak was observed in the relativistic proton time profile by neutron monitors. This time profile is compared in detail with UV imaging and radio spectrography over a broad frequency band from the low corona to interplanetary space. Results. It is shown that the late relativistic proton release to interplanetary space was accompanied by a distinct new episode of energy release and electron acceleration in the corona traced by the radio emission and by brightenings of UV kernels. These signatures are interpreted in terms of magnetic restructuring in the corona after the coronal mass ejection passage. Conclusions. We attribute the delayed relativistic proton acceleration to magnetic reconnection and possibly to turbulence in largescale coronal loops. While Type II radio emission was observed in the high corona, no evidence of a temporal relationship with the relativistic proton acceleration was found.

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Ground level enhancements of solar cosmic rays during the last three solar cycles

Cited by 52 publications

References 16 publications

Ionization effect of solar particle GLE events in low and middle atmosphere

Ionization effect of solar particle GLE events in low and middle atmosphere

Two solar proton fluence models based on ground level enhancement observations

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

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