Solar Flare Protection for Manned Lunar Missions: Analysis of the October 1989 Proton Flare Event

1991 ◽  
Author(s):  
Lisa C. Simonsen ◽  
John E. Nealy ◽  
Herbert H. Sauer ◽  
Lawrence W. Townsend
Keyword(s):  
Solar Flare ◽  
Flare Event ◽  
Lunar Missions

Spectroscopic analysis of the solar flare event on 2002 August 3 with the use of RHESSI and RESIK data

2008 ◽  
Vol 42 (5) ◽  
pp. 822-827 ◽  
Author(s):  
S. Gburek ◽  
T. Mrozek ◽  
M. Siarkowski ◽  
J. Sylwester
Keyword(s):  
Solar Flare ◽  
Spectroscopic Analysis ◽  
Flare Event

scholarly journals First Light Detection of a Single Solar Radio Burst Type III due to Solar Flare Event

2014 ◽  
Vol 30 ◽  
pp. 51-58 ◽  
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Solar Flare ◽  
Total Energy ◽  
Radio Burst ◽  
Solar Radio ◽  
Solar Radio Burst ◽  
Single Type ◽  
Mass Motion ◽  
Light Detection ◽  
Flare Event ◽  
Type Iii

The eruption mechanism of solar flares and type III are currently an extremely active area of research, especially during the solar cycle is towards maximum. In this case, the total energy of solar burst type III is of the order of solar flare with the explosion of the energy can up to 1015 ergs. The solar flare event is one of the most spectacular explosions that still be on-going study in the solar physics world. This event occurred at 2:000 UT on 15th April 2012 is due to the explosion of the magnetic energy in from the chromosphere and converted into the heating, mass motion and particle acceleration which can be detected by solar radio burst type III. In this work, we will highlight our first light detection of very tiny solar radio burst type III, which has been observed at the National Space Centre, Banting, Selangor detected by the Compound Low Cost Low Frequency Transportable Observatories (CALLISTO) system at 5:53:23. The region of the data is from 150 − 400 MHz in radio region. This burst is drifted from 150 MHz till 260 MHz. It represents a total energy of 6.2035 × 10-7 eV − 1.0753 × 10-6 eV. This fast drift burst is a continuity of the acceleration of the particles which is intermittent, and can be observed since the explosion of the solar flare. Although the burst is very tiny, it is still significant because this burst is the first detection of a single type III burst from our site. Still, the acceleration of the particles can be detected from Earth in the radio region within 3 hours period of observation at the post stage of solar flare.

Energy spectra of high energy electrons and hard X-rays as observed onboard the space probe Venera 11 during the solar flare event of April 13 1979

1981 ◽  
Vol 1 (3) ◽  
pp. 73-76 ◽  
Author(s):  
E.I. Daibog ◽  
E.A. Devicheva ◽  
S.V. Golenetskii ◽  
Yu.A. Guryan ◽  
V.G. Kurt ◽  
...  
Keyword(s):  
Solar Flare ◽  
High Energy ◽  
Energy Spectra ◽  
X Rays ◽  
Space Probe ◽  
Flare Event ◽  
High Energy Electrons

scholarly journals September 2017 Solar Flare Event: Rapid Heating of the Martian Neutral Upper Atmosphere From the X-Class Flare as Observed by MAVEN

2018 ◽  
Vol 45 (17) ◽  
pp. 8803-8810 ◽  
Author(s):  
M. K. Elrod ◽  
S. M. Curry ◽  
E. M. B. Thiemann ◽  
S. K. Jain
Keyword(s):  
Solar Flare ◽  
Rapid Heating ◽  
Upper Atmosphere ◽  
Flare Event ◽  
Class Flare

scholarly journals Fundamental and Second Harmonic Bands of Solar Radio Burst Type II Caused by X1.8 - Class Solar Flares

2014 ◽  
Vol 33 ◽  
pp. 208-217 ◽  
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Solar Flare ◽  
Solar Flares ◽  
Drift Rate ◽  
Second Harmonic ◽  
Low Cost ◽  
Low Frequency ◽  
Electromagnetic Spectrum ◽  
Driving Mechanism ◽  
Type Ii ◽  
Flare Event

An extreme 2012 October 23 solar flare event marked on the onset of the CALLISTO data, being one of the highest solar flare event that successfully detected. The formation of harmonic solar burst type II in meter region and their associated with X1.8-class solar flares has been reported. This burst has been observed at the National Space Centre, Banting, detected by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) system in the range of 150-400 MHz in the low frequency band. It occurred between 3.17:45 UT to 3.19:00 UT within 1 minute 15 seconds. The Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory CALLISTO spectrometer is a solar dedicated spectrometer system that has been installed all over the world to monitor the Sun activity in 24 hours. The growth of this burst is often accompanied by abundance enhancement of particles which may take the form of multiple independent drifting bands or other forms of fine structure. Due to the results, the drift rate of this burst is 2.116 MHz s–1, which is considered as a slow drift rate. These drifting bands are approximately having a frequency ratio 2:1. This burst is a particular interest, though of sporadic and infrequent occurrence. The splitting is due to the effect of magnetic splitting, analogous to the Zeeman Effect. This is one of the examples which the type II burst is not always associated with CMEs event. The combination of radio and x-ray region give a complete view of the solar flare eruption from e active region AR1598. Both different electromagnetic spectrum shows the exact time. Other interesting results is that this type II burst is not associated with CMEs as usual, but due to the very high solar flare event with a fundamental form at more than 100 MHz. An extension of the present work will be a detailed study of the possible triggering and the driving mechanism of solar flare explosion.

The proton scattering mean free path for the May 7, 1978, solar flare event

1991 ◽  
Vol 96 (A5) ◽  
pp. 7897 ◽  
Author(s):  
H. Debrunner ◽  
H. Grädel ◽  
J. A. Lockwood
Keyword(s):  
Solar Flare ◽  
Free Path ◽  
Mean Free Path ◽  
Proton Scattering ◽  
Flare Event
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