On the time evolution of brightness, volume and height of a coronal source in an M-class flare
FIROZ, Kazi A. - Personal Name
GAN, W.Q. - Personal Name
LI, Y.P. - Personal Name
PACHECO, J. Rodríguez- - Personal Name
SU, Y. - Personal Name
We study brightness, volume and heights of the
X-ray thermal emission components for an M-class solar
flare on 17 May 2012. Based on the RHESSI data availabil-
ity, we present the results for 01:42–01:58 UT over the late-
flare phase. It is observed that the spatial evolution of the
thermal emission components 6–12 and 12–18 keV are well
associated with the hottest plasma in the corona. Results
show that the ascending height (∼1.35 × 10 4 km) and speed
(∼14.0 km s −1 ) of coronal source component 6–12 keV is
slightly smaller than the ascending height (∼1.45 × 10 4 km)
and speed (∼15.1 km s −1 ) of the coronal source component
12–18 keV. Mean flux intensity (I mean ) of the 6–12 keV
maintained a good fit (χ 2 = 0.41) with the correspond-
ing volume (V ) following strongly the power law [I mean =
(15.8 ± 0.21)V −1.28±0.03 ]. In contrast, the 12–18 keV main-
tained a weak fit (χ 2 = 2.37) following still the power law
[I mean = (0.19 ± 0.01)V −1.88±0.16 ]. The power law indices
(−1.28 ± 0.03; −1.88 ± 0.16) obtained by the observational
analysis slightly differ from the power law index (−1.67)
obtained by a theoretical model. The observations are con-
sistent with adiabatic expansion of the coronal source com-
ponent.
X-ray thermal emission components for an M-class solar
flare on 17 May 2012. Based on the RHESSI data availabil-
ity, we present the results for 01:42–01:58 UT over the late-
flare phase. It is observed that the spatial evolution of the
thermal emission components 6–12 and 12–18 keV are well
associated with the hottest plasma in the corona. Results
show that the ascending height (∼1.35 × 10 4 km) and speed
(∼14.0 km s −1 ) of coronal source component 6–12 keV is
slightly smaller than the ascending height (∼1.45 × 10 4 km)
and speed (∼15.1 km s −1 ) of the coronal source component
12–18 keV. Mean flux intensity (I mean ) of the 6–12 keV
maintained a good fit (χ 2 = 0.41) with the correspond-
ing volume (V ) following strongly the power law [I mean =
(15.8 ± 0.21)V −1.28±0.03 ]. In contrast, the 12–18 keV main-
tained a weak fit (χ 2 = 2.37) following still the power law
[I mean = (0.19 ± 0.01)V −1.88±0.16 ]. The power law indices
(−1.28 ± 0.03; −1.88 ± 0.16) obtained by the observational
analysis slightly differ from the power law index (−1.67)
obtained by a theoretical model. The observations are con-
sistent with adiabatic expansion of the coronal source com-
ponent.
Availability
| EB00000004150K | Available |
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E-Jurnal
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Subject(s)
Solar flares
Area/volume of the flare
Volume and mean intensity
Heights of the coronal sources
Total Thermal electrons in high-temperature plasma
contribution into the flare process
Adiabatic expansion
Theoretical model for thermal source
RHESSI X-ray
GOES X-ray
SDO/AIA images
Spatial and temporal evolution of the coronal sour
RHESSI image reconstruction algorithm
Specific Detail Info
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Statement of Responsibility
Kazi A. Firoz 1,2 · W.Q. Gan 1 · Y.P. Li 1 · J. Rodríguez-Pacheco 2 · Y. Su 1
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