Particle propagation effects on solar flare X- and ?-ray time profiles

Solar Physics ◽  
1986 ◽  
Vol 105 (2) ◽  
Author(s):  
JamesM. Ryan
Keyword(s):  
Solar Flare ◽  
Time Profiles ◽  
Propagation Effects ◽  
Particle Propagation

Particle propagation effects on wave growth in a solar flux tube

1986 ◽  
Vol 308 ◽  
pp. 424 ◽  
Author(s):  
S. M. White ◽  
D. B. Melrose ◽  
G. A. Dulk
Keyword(s):  
Flux Tube ◽  
Solar Flux ◽  
Wave Growth ◽  
Propagation Effects ◽  
Particle Propagation

scholarly journals The solar energetic particle propagation of solar flare events on 24thsolar cycle.

2017 ◽  
Vol 901 ◽  
pp. 012016
Author(s):  
P. Paluk ◽  
T. Khumlumlert ◽  
N. Kanlayaprasit ◽  
N. Aiemsa-ad
Keyword(s):  
Solar Flare ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Particle Propagation

scholarly journals Particle propagation in clumpy supernova remnants

2019 ◽  
Vol 209 ◽  
pp. 01033
Author(s):  
Silvia Celli
Keyword(s):  
Gamma Rays ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Numerical Study ◽  
Background Plasma ◽  
Strong Impact ◽  
Propagation Effects ◽  
Particle Propagation

The presence of dense clumps in the environment where a supernova remnant expands might have a strong impact in shaping the observed hadronic gamma-ray spectrum. A detailed numerical study about the penetration of relativistic protons into clumps which are engulfed by a supernova remnant shock is here presented, taking into account the magneto-hydrodynamical properties of the background plasma. This has strong implications for the formation of the spectrum of hadronic gamma rays, which does not reflect anymore the acceleration spectrum of protons, resulting substantially modified by propagation effects. A hadronic scenario including dense clumps inside the remnant shell is shown to adequately reproduce the broadband gamma-ray spectrum of the Galactic supernova remnant RX J1713-3946.7 from GeV to TeV energies.

scholarly journals The morphology of average solar flare time profiles from observations of the Sun’s lower atmosphere

2021 ◽  
Vol 502 (3) ◽  
pp. 3922-3931
Author(s):  
Larisa K Kashapova ◽  
Anne-Marie Broomhall ◽  
Alena I Larionova ◽  
Elena G Kupriyanova ◽  
Ilya D Motyk
Keyword(s):  
Solar Flare ◽  
Power Law ◽  
Solar Flares ◽  
Lower Atmosphere ◽  
Decay Phase ◽  
Dense Layer ◽  
Time Profiles ◽  
Spectral Bands ◽  
The Impact ◽  
M Dwarf

ABSTRACT We study the decay phase of solar flares in several spectral bands using a method based on that successfully applied to white light flares observed on an M4 dwarf. We selected and processed 102 events detected in the Sun-as-a-star flux obtained with SDO/AIA images in the 1600 and 304 Å channels and 54 events detected in the 1700 Å channel. The main criterion for the selection of time profiles was a slow, continuous flux decay without significant new bursts. The obtained averaged time profiles were fitted with analytical templates, using different time intervals, that consisted of a combination of two independent exponents or a broken power law. The average flare profile observed in the 1700 Å channel decayed more slowly than the average flare profile observed on the M4 dwarf. As the 1700 Å emission is associated with a similar temperature to that usually ascribed to M dwarf flares, this implies that the M dwarf flare emission comes from a more dense layer than solar flare emission in the 1700 Å band. The cooling processes in solar flares were best described by the two exponents model, fitted over the intervals t1 = [0, 0.5]t1/2 and t2 = [3, 10]t1/2, where t1/2 is time taken for the profile to decay to half the maximum value. The broken power-law model provided a good fit to the first decay phase, as it was able to account for the impact of chromospheric plasma evaporation, but it did not successfully fit the second decay phase.

scholarly journals The X-ray Light-Curves and CME onset of a M2.5 flare of July 6, 2006

2016 ◽  
Vol 12 (S328) ◽  
pp. 240-242
Author(s):  
J. E. Mendoza-Torres ◽  
J. E. Pérez-León
Keyword(s):  
Solar Flare ◽  
Radio Emission ◽  
Light Curves ◽  
Main Peak ◽  
Physical Parameters ◽  
X Ray ◽  
Time Profiles ◽  
Chromospheric Evaporation ◽  
Mass Ejection ◽  
Compact Sources

AbstractA M2.5 solar flare observed by RHESSI in the 6-100 keV range on July 6, 2006 led to a Coronal Mass Ejection (CME). Two compact sources at 12-100 keV are seen at the beginning of the flare, whose further evolution fits well in a loop. Also, time-profiles of the flare at radio wavelengths are compared. The X-ray light-curves at different bands in the 6-100 keV range and radio time profiles show some peaks superimposed on smooth variations. The aim of this work is to compare the X-ray light-curves, of fluxes integrated over the whole source, with the physical parameters of the sources of the flare. Yashiro and Gopalswamy (2009) have found that the fraction of flares that produce CME increases with the flare energy. Here, we look for the characteristics of an M2.5 flare that could make it a generator of a CME. The idea is, in future works, to look in the light-curves of similar flares at other stars for these features. It is found that the CME onset takes place around the time when an X-ray source at 12-25 keV of Chromospheric evaporation stagnates at the loop apex, before the main peak at the light-curve at 25-50 keV and at the radio emission curves. Probably, the amount of evaporated plasma could play some role in triggering the CME.

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