scholarly journals Recent and Historical Solar Proton Events

Radiocarbon ◽  
1992 ◽  
Vol 34 (2) ◽  
pp. 255-262 ◽  
Author(s):  
M. A. Shea ◽  
D. F. Smart
Keyword(s):  
Solar Activity ◽  
Geomagnetic Storms ◽  
Solar Proton ◽  
Solar Proton Event ◽  
Proton Event ◽  
Event Data ◽  
The Earth ◽  
Solar Proton Events

A study of the solar proton event data between 1954 and 1986 indicates that the large fluence events at the Earth are usually associated with a sequence of solar activity and related geomagnetic storms. This association appears to be useful to infer the occurrence of major fluence proton events extending back to 1934, albeit in a non-homogeneous manner. We discuss the possibility of identifying major solar proton events prior to 1934, using geomagnetic records as a proxy.

scholarly journals EISCAT and ESRAD radars observations of polar mesosphere winter echoes during solar proton events on 11–12 November 2004

2013 ◽  
Vol 31 (7) ◽  
pp. 1177-1190 ◽  
Author(s):  
E. Belova ◽  
S. Kirkwood ◽  
T. Sergienko
Keyword(s):  
Power Spectrum ◽  
Electron Gas ◽  
Spectral Width ◽  
Solar Proton ◽  
Solar Proton Event ◽  
Complete Theory ◽  
Proton Event ◽  
Maximum Volume ◽  
Incoherent Scatter ◽  
Solar Proton Events

Abstract. Polar mesosphere winter echoes (PMWE) were detected by two radars, ESRAD at 52 MHz located near Kiruna, Sweden, and EISCAT at 224 MHz located near Tromsø, Norway, during the strong solar proton event on 11–12 November 2004. PMWE maximum volume reflectivity was estimated to be 3 × 10−15 m−1 for ESRAD and 2 × 10−18 m−1 for EISCAT. It was found that the shape of the echo power spectrum is close to Gaussian inside the PMWE layers, and outside of them it is close to Lorentzian, as for the standard ion line of incoherent scatter (IS). The EISCAT PMWE spectral width is about 5–7 m s−1 at 64–67 km and 7–10 m s−1 at 68–70 km. At the lower altitudes the PMWE spectral widths are close to those for the IS ion line derived from the EISCAT data outside the layers. At the higher altitudes the PMWE spectra are broader by 2–4 m s−1 than those for the ion line. The ESRAD PMWE spectral widths at 67–72 km altitude are 3–5 m s−1, that is, 2–4 m s−1 larger than ion line spectral widths modelled for the ESRAD radar. The PMWE spectral widths for both EISCAT and ESRAD showed no dependence on the echo strength. It was found that all these facts cannot be explained by turbulent origin of the echoes. We suggested that evanescent perturbations in the electron gas generated by the incident infrasound waves may explain the observed PMWE spectral widths. However, a complete theory of radar scatter from this kind of disturbance needs to be developed before a full conclusion can be made.

Study on Solar Proton Events in the Sun - Induced Earth’s Magnetic Field Atmospheric Variations

2017 ◽  
Vol 3 (06) ◽  
Author(s):  
M. V. Subramanian ◽  
S. Jagadesan ◽  
K. Aruna ◽  
S. Pari ◽  
S. Deivamalar
Keyword(s):  
Magnetic Field ◽  
Solar Flare ◽  
Solar Proton ◽  
Proton Event ◽  
Dst Index ◽  
Data Centre ◽  
Sunspot Numbers ◽  
The Earth ◽  
Solar Proton Events ◽  
Ap Index

Estimation has been made for the most powerful solar proton events recorded in the Earth environment during 1976 - 2015. This study has been done in association with other related activities such as Sunspot numbers and Solar flare index, the Earth’s magnetic field variation H constant, Dst index, Ap index and Kp index data from Kyoto data centre and OMNI data centre. We found that proton flux occurred after two days indicate the Dst index, Ap index and Kp index and Earth’s magnetic field H constant variations. This study has been done in association with other related activities such as sunspot numbers, solar flare activities. We found that the proton event occurred within 25 to 29 days after the cyclone was formed in the earth atmosphere. Earth atmospheric climate also changed.

Characteristics of source location and solar cycle distribution of the strong solar proton events (≥ 1000 pfu) from 1976 to 2018

2021 ◽  
Author(s):  
Gui-Ming Le ◽  
Ming-Xian Zhao ◽  
Qi Li ◽  
Gui-Ang Liu ◽  
Tian Mao ◽  
...  
Keyword(s):  
Solar Cycle ◽  
Geomagnetic Storms ◽  
Ground Level ◽  
Solar Proton ◽  
Western Hemisphere ◽  
Poor Correlation ◽  
The Sun ◽  
The Earth ◽  
Solar Proton Events ◽  
Northern And Southern Hemispheres

Abstract We studied the source locations and solar cycle distribution of strong solar proton events (≥ 1000 pfu) measured at the Earth from 1976 to 2018. There were 43 strong solar proton events (SPEs) during this period. 27.9 per cent of the strong SPEs were ground level enhancement (GLE) events. We detect more strong SPEs coming from the western hemisphere. The strong SPEs were distributed in the region of [E90-W90], extreme SPEs (≥10000 pfu) appeared within the longitudinal area from E30 to W75, while the SPEs with peak fluxes ≥ 20000 pfu concentrated in the range from E30 to W30 and were always accompanied by super geomagnetic storms (Dst ≤−250 nT). The northern and southern hemispheres of the Sun have 23 and 20 strong SPEs, respectively. The ranges S0–S19 and N0–N19 have 13 and 11 strong SPEs, respectively. S20–S45 and N20–N45 have 7 and 12 strong SPEs, respectively, indicating that the N-S asymmetry of strong SPEs mainly occurred in the areas with a latitude greater than 20○ of the two hemispheres of the Sun. The statistical results showed that 48.8 per cent, 51.2 per cent, and 76.7 per cent of the strong SPEs appeared during the rising phase, declining phase, and in the period from two years before to the three years after the solar maximum, respectively. The number of strong SPEs during a solar cycle has a poor correlation with the solar cycle size.

scholarly journals Prediction of Solar Proton Event Fluence spectra from their Peak flux spectra

2020 ◽  
Vol 10 ◽  
pp. 1 ◽  
Author(s):  
Sigiava Aminalragia-Giamini ◽  
Piers Jiggens ◽  
Anastasios Anastasiadis ◽  
Ingmar Sandberg ◽  
Angels Aran ◽  
...  
Keyword(s):  
Ionizing Radiation ◽  
Space Weather ◽  
Solar Proton ◽  
Solar Proton Event ◽  
Ongoing Study ◽  
Proton Event ◽  
Physical Mechanisms ◽  
High Energies ◽  
Peak Flux ◽  
Solar Proton Events

Solar Proton Events (SPEs) are of great importance and significance for the study of Space Weather and Heliophysics. These populations of protons are accelerated at high energies ranging from a few MeVs to hundreds of MeVs and can pose a significant hazard both to equipment on board spacecrafts as well as astronauts as they are ionizing radiation. The ongoing study of SPEs can help to understand their characteristics, relative underlying physical mechanisms, and help in the design of forecasting and nowcasting systems which provide warnings and predictions. In this work, we present a study on the relationships between the Peak Flux and Fluence spectra of SPEs. This study builds upon existing work and provides further insights into the characteristics and the relationships of SPE Peak flux and Fluence spectra. Moreover it is shown how these relationships can be quantified in a sound manner and exploited in a simple methodology with which the Fluence spectrum of an SPE can be well predicted from its given Peak spectrum across two orders of magnitude of proton energies, from 5 MeV to 200 MeV. Finally it is discussed how the methodology in this work can be easily applied to forecasting and nowcasting systems.

Solar induced earthquakes – review and new results

2020 ◽  
Author(s):  
Sergey Pulinets ◽  
Galina Khachikyan
Keyword(s):  
Energy Transfer ◽  
Solar Activity ◽  
Geomagnetic Storms ◽  
Electromagnetic Emission ◽  
Solar Proton ◽  
Galactic Cosmic Rays ◽  
Earthquake Activity ◽  
Induced Earthquakes ◽  
Unique Identifier ◽  
The Earth

<p>A lot of information has been accumulated recently demonstrating impacts of solar activity on the Earth’s seismicity. We observe the transition from correlation-driven papers to the more physical based works. The effects of solar influence could be separated by agents of energy transfer which could be electromagnetic emission of the Sun, particle fluxes of solar wind, solar proton events, modification of radiation belts and indirect impacts through the intermediate agent, such as atmosphere disturbances and modification of atmosphere circulation as effect of solar activity. Effects of the galactic cosmic rays should be taken into account including the Forbush decreases, which are result of geomagnetic storms. MHD electromagnetic sounding stimulating the earthquake activity could be considered as a physical model of the geomagnetic storms effect on the seismic activity.</p><p>The most intriguing effects discovered recently is the inducing the strong M>7 earthquakes by the precipitation from additional radiation belt at L-shell 1.5-1.8 formed after the strong geomagnetic storm. Precipitation of relativistic particles from this shell induces the strong earthquakes with delay nearly 2 months.</p><p>One very importing agent of geosphere coupling including the energy transfer int the lithosphere is the Global Electric Circuite.</p><p>It is difficult to explain the observed phenomena by simple transformation of solar energy into mechanical deformation, it seems that more plausible explanation is the pumping of energy into the Earth’s crust volume being in a metastable state.</p><p>This work was supported by the Ministry of Education and Science of the Russian Federation in accordance with Subsidy Agreement No. 05.585.21.0008. The unique identifier is RFMEFI58519X0008</p>

List of Solar Proton Events in the 24 Cycle of Solar Activity (2009 ‒ 2019)

2019 ◽  
Author(s):  
◽  
Vitaly Ishkov ◽  
Yury Logachev ◽  
Galina Bazilevskaya ◽  
Elena Daibog ◽  
...  
Keyword(s):  
Solar Activity ◽  
Solar Proton ◽  
Solar Proton Events

scholarly journals Enhancement of stratospheric aerosols after solar proton event

1996 ◽  
Vol 14 (11) ◽  
pp. 1119-1123 ◽  
Author(s):  
O. I. Shumilov ◽  
E. A. Kasatkina ◽  
K. Henriksen ◽  
E. V. Vashenyuk
Keyword(s):  
Considerable Increase ◽  
Ground Level ◽  
Solar Proton ◽  
Stratospheric Aerosol ◽  
Nucleation Mechanism ◽  
Solar Proton Event ◽  
Proton Event ◽  
Aerosol Layer ◽  
Event Type ◽  
Lidar Measurements

Abstract. The lidar measurements at Verhnetulomski observatory (68.6°N, 31.8°E) at Kola peninsula detected a considerable increase of stratospheric aerosol concentration after the solar proton event of GLE (ground level event) type on the 16/02/84. This increase was located at precisely the same altitude range where the energetic solar protons lost their energy in the atmosphere. The aerosol layer formed precipitated quickly (1–2 km per day) during 18, 19, and 20 February 1984, and the increase of R(H) (backscattering ratio) at 17 km altitude reached 40% on 20/02/84. We present the model calculation of CN (condensation nuclei) altitude distribution on the basis of an ion-nucleation mechanism, taking into account the experimental energy distribution of incident solar protons. The meteorological situation during the event was also investigated.

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