An atlas of 10?50ke V solar flare X-rays and tentative atlas of solar proton events observed by the OGO-I and OGO-III ionization chambers

Solar Physics ◽  
1969 ◽  
Vol 6 (1) ◽  
pp. 151-151 ◽  
Author(s):  
S. R. Kane ◽  
J. R. Winckler
Keyword(s):  
Solar Flare ◽  
Solar Proton ◽  
X Rays ◽  
Ionization Chambers ◽  
Solar Proton Events

Application of support vector machine combined with K-nearest neighbors in solar flare and solar proton events forecasting

2008 ◽  
Vol 42 (9) ◽  
pp. 1469-1474 ◽  
Author(s):  
Rong Li ◽  
Yanmei Cui ◽  
Han He ◽  
Huaning Wang
Keyword(s):  
Support Vector Machine ◽  
Solar Flare ◽  
Nearest Neighbors ◽  
Solar Proton ◽  
Support Vector ◽  
K Nearest Neighbors ◽  
Solar Proton Events

A Lunar-Month Modulation of Large Solar-Terrestrial Disturbances

1967 ◽  
Vol 1 (1) ◽  
pp. 11-12 ◽  
Author(s):  
S. F. Smerd
Keyword(s):  
Solar Flare ◽  
Random Distribution ◽  
Full Moon ◽  
Solar Rotation ◽  
Rotation Period ◽  
Solar Proton ◽  
The Sun ◽  
The Moon ◽  
Unexpected Effect ◽  
Solar Proton Events

Dodson and Hedeman discovered an unexpected effect in the occurrence of solar proton events as revealed by polarcap absorption (PCA). When the 48 events in Bailey’s Catalog of the Principal PCA Events, 1952-1963 are distributed with the phase of the moon there is a gap of several days near full moon; also, many more events occur when the moon waxes than when it wanes. Dodson and Hedeman did not find similar, apparent departures from random distribution either with a mean solar rotation period of 27.3 days or for solar flare events. They concluded that ‘at the present time it is not clear whether the 29.5 day “effect” is related to the sun or the moon or is only a statistical accident’.

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.

scholarly journals The observation of 10–50 KeV solar flare X-rays by the OGO satellites and their correlation with solar radio and energetic particle emission

1968 ◽  
Vol 35 ◽  
pp. 490-509
Author(s):  
R. L. Arnoldy ◽  
S. R. Kane ◽  
J. R. Winckler
Keyword(s):  
Magnetic Field ◽  
Solar Flare ◽  
Radio Emission ◽  
Total Energy ◽  
Total Duration ◽  
Microwave Emission ◽  
X Rays ◽  
Ionization Chambers ◽  
X Ray ◽  
Peak Intensity

More than 70 cases have been observed of energetic solar flare X-ray bursts by large ionization chambers on the OGO satellites in space. The ionization chambers have an energy range between 10 and 50 KeV for X-rays and are also sensitive to solar protons and electrons. A study has been made of the X-ray microwave relationship, and it is found that the total energy released in the form of X-rays between 10 and 50 KeV is approximately proportional to the peak or total energy simultaneously released in the form of microwave emission. For a given burst the rise time, decay time and total duration are similar for the 10–50 KeV X-rays and the 3 to 10 cm radio emission. Roughly exponential decay phases are observed for both emissions with time constants between 1 and 10 min. All 3 or 10 cm radio bursts with peak intensity greater than 80 solar flux units are accompanied by an X-ray burst greater than 3 × 10−7 ergs cm−2 sec−1 peak intensity. The probability of detecting such X-ray events is low unless the radio spectrum extends into the centimetric range of wavelengths. The best correlation between cm-λ and energetic X-rays is observed for the first event in a flare. Subsequent structure and second bursts may not correspond even when the radio emission is rich in the microwave component. The mechanism for the energetic X-rays is shown to be bremsstrahlung probably of fast electrons on a cooler plasma. If the radio emission is assumed to be synchrotron radiation then a relationship is developed between density and magnetic field which meets the observed quantitative results. One finds, on the average, that 5 × 10−54 joules m−2 (CPS)−1 of microwave energy at the Earth are required per electron at the Sun to provide the radio emission for the various events.A strong correlation between interplanetary solar flare electrons observed by satellite and X-ray bursts is shown to exist. This correlation is weak for solar proton events. One may infer a strong propagation asymmetry for solar flare electrons along the spiral interplanetary magnetic field.

The Cosmic Ray Solar Flare Increase of 16 February 1984

1984 ◽  
Vol 5 (4) ◽  
pp. 593-594
Author(s):  
A. G. Fenton ◽  
K. B. Fenton ◽  
J. E. Humble
Keyword(s):  
Solar Activity ◽  
Solar Cycle ◽  
Solar Flare ◽  
Cosmic Ray ◽  
Ground Level ◽  
Solar Proton ◽  
Solar Proton Events

Six solar proton events have been observed by ground level cosmic ray detectors so far during solar cycle 21, a little less than one per year. All of these have been much smaller than the giant events observed in solar cycle 19. As with many other aspects of solar activity, the reason for the differences from cycle to cycle remain unknown.

A Conjunctive Study of Solar Flare 20010402 and Related Solar Proton Events by the Observation of SZ2/XD and ZY1/CBMC

2004 ◽  
Vol 47 (5) ◽  
pp. 837-842 ◽  
Author(s):  
Yu-Qian MA ◽  
Huan-Yu WANG ◽  
Cheng-Mo ZhaNG ◽  
Yu-Peng Xu ◽  
Jin-Zhou WANG ◽  
...  
Keyword(s):  
Solar Flare ◽  
Solar Proton ◽  
Solar Proton Events

National primary standard of air kerma, air kerma rate, exposure, exposure rate and energy flux for X-rays and gamma radiation GET 8-2019

2020 ◽  
pp. 8-12
Author(s):  
Alexandr V. Oborin ◽  
Anna Y. Villevalde ◽  
Sergey G. Trofimchuk
Keyword(s):  
Gamma Radiation ◽  
Energy Flux ◽  
Primary Standard ◽  
Average Energy ◽  
Ion Pair ◽  
X Rays ◽  
Exposure Rate ◽  
Ionization Chambers ◽  
Air Kerma ◽  
Air Kerma Rate

The results of development of the national primary standard of air kerma, air kerma rate, exposure, exposure rate and energy flux for X-rays and gamma radiation GET 8-2011 in 2019 are presented according to the recommendations of the ICRU Report No. 90 “Key Data for Ionizing-Radiation Dosimetry: Measurement Standards and Applications”. The following changes are made to the equations for the units determination with the standard: in the field of X-rays, new correction coefficients of the free-air ionization chambers are introduced and the relative standard uncertainty of the average energy to create an ion pair in air is changed; in the field of gamma radiation, the product of the average energy to create an ion pair in air and the electron stopping-power graphite to air ratio for the cavity ionization chambers is changed. More accurate values of the units reproduced by GET 8-2019 are obtained and new metrological characteristics of the standard are stated.

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

Localization of the solar flare SF900610 in X-rays with the WATCH instrument of the GRANAT observatory

2002 ◽  
Vol 28 (12) ◽  
pp. 853-856
Author(s):  
O. V. Terekhov ◽  
A. G. Kuzmin ◽  
A. V. Shevchenko ◽  
S. Yu. Sazonov ◽  
R. A. Sunyaev ◽  
...  
Keyword(s):  
Solar Flare ◽  
X Rays

Effect of solar proton events in 1978 and 1979 on the odd nitrogen abundance in the middle atmosphere

1988 ◽  
Vol 93 (D6) ◽  
pp. 7084-7090 ◽  
Author(s):  
Charles H. Jackman ◽  
Paul E. Meade
Keyword(s):  
Middle Atmosphere ◽  
Solar Proton ◽  
Nitrogen Abundance ◽  
Solar Proton Events ◽  
Odd Nitrogen
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