X-ray emission from solar flares

Jain, Rajmal; Aggarwal, Malini; Sharma, Rashmi

doi:10.1007/s12036-008-0016-z

Cited by 11 publications

(23 citation statements)

References 18 publications

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“…Thus to calculate the peak plasma temperature and the DEM we have employed the least- 2 fitting to the SOXS X-ray spectra in OSPEX as described earlier by Jain et al (2008).…”

Section: Spectra Analysismentioning

confidence: 99%

“…Thus it is extremely important to characterize the soft X-ray emission below 10 keV. Further, the X-ray emission between 10 and 25 keV should in principle include both thermal and non-thermal contributions (Aschwanden, 2007;Jain et al, 2008). Therefore, the characterization of flare plasma up to 25 keV with high spectral resolution observations becomes further important.…”

Section: Introductionmentioning

confidence: 99%

“…Therefore, the characterization of flare plasma up to 25 keV with high spectral resolution observations becomes further important. Jain et al (2008) showed that the X-ray bursts associated with solar flares above 25 keV come mostly from the non-thermal bremsstrahlung while the X-ray emission between 10 and 25 keV in principle includes both thermal and non-thermal contributions. Both types of X-ray emission occur during solar flares and the clear demarcation line between the two processes provides quantitative estimation of energy release by each process in solar flares.…”

Section: Introductionmentioning

confidence: 99%

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Energy-Dependent Timing of Thermal Emission in Solar Flares

et al. 2011

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We report solar flare plasma to be multi-thermal in nature based on the theoretical model and study of the energy-dependent timing of thermal emission in ten M-class flares. We employ high-resolution X-ray spectra observed by the Si detector of the "Solar X-ray Spectrometer" (SOXS). The SOXS onboard the Indian GSAT-2 spacecraft was launched by the GSLV-D2 rocket on 8 May 2003. Firstly we model the spectral evolution of the X-ray line and continuum emission flux F() from the flare by integrating a series of isothermal plasma flux.We find that multi-temperature integrated flux F() is a power-law function of  with a spectral index () ≈ -4.65. Next, based on spectral-temporal evolution of the flares we find that the emission in the energy range E= 4 -15 keV is dominated by temperatures of T= 12 -50 MK, while the multi-thermal power-law DEM index () varies in the range of -4.4 and -5.7. The temporal evolution of the X-ray flux F(,t) assuming a multi-temperature plasma governed by thermal conduction cooling reveals that the temperature-dependent cooling time varies between 296 and 4640 s and the electron density (n e ) varies in the range of n e = (1.77-29.3)*10 10 cm -3 . Employing temporal evolution technique in the current study as an alternative method for separating thermal from non-thermal components in the energy spectra, we measure the break-energy point ranging between 14 and 21±1.0 keV.

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“…Thus to calculate the peak plasma temperature and the DEM we have employed the least- 2 fitting to the SOXS X-ray spectra in OSPEX as described earlier by Jain et al (2008).…”

Section: Spectra Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Energy-Dependent Timing of Thermal Emission in Solar Flares

et al. 2011

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“…3. We analysed 2-5 spectra depending on the duration of each microflare under study and found that the best fit to the spectra is by thermal for energy range 4-8 keV, while the continuum of the spectra at energies > 8 keV fits well by broken power-law (Jain et al 2008). This result shows that the microflares are most likely the product of both mechanism viz., thermal and non-thermal, which is an indicator of hybrid mechanism in microflares as proposed earlier by Jain et al (2006b).…”

Section: Discussionmentioning

confidence: 82%

Microflares as possible sources for coronal heating

et al. 2008

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We present a preliminary study of 27 microflares observed by Solar X-ray Spectrometer (SOXS) mission during July 2003 to August 2006. We found that all 27 microflares show the Fe-line feature peaking around 6.7 keV, which is an indicator of the presence of coronal plasma temperature ≥ 9 MK. On the other hand, the spectra of microflares show hybrid model of thermal and non-thermal emission, which further supports them as possible sources of coronal heating. Our results based on the analysis show that the energy relapsed by the microflares is good enough for heating of the active corona. We discuss our results in the light of the hybrid model of microflares production.

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“…The SOXS provides solar flare observations in X-ray waveband in the energy range of 4-56 keV. [27][28][29][30].…”

Section: Selection Criteria and Datamentioning

confidence: 99%

A Correlative Study of Geomagnetic Storms Associated with Solar Wind and IMF Features During Solar Cycle 23

Rathore¹,

Kaushik²,

Firoz³

et al. 2011

IJAPM

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Abstract-A geomagnetic storm is a global disturbance in Earth's magnetic field usually occurred due to abnormal conditions in the interplanetary magnetic field (IMF) and solar wind plasma emissions caused by various solar phenomenon. Furthermore the magnitude of these geomagnetic effects largely depend upon the configuration and strength of potentially geo-effective solar/interplanetary features. In the present study the identification of 220 geomagnetic storms associated with disturbance storm time (Dst) decrease of more than -50 nT to -300 nT, have been made, which are observed during 1996-2007, the time period spanning over solar cycle 23. The study is made statistically between the Dst strength (used as an indicator of the geomagnetic activity) and the peak value obtained by solar wind plasma parameters and IMF B as well as its components. We have used the hourly values of Dst index and the wind measurements taken by various satellites. Our results inferred that yearly occurrences of geomagnetic storms are strongly correlated with 11-year sunspot cycle. We observed that IMF B is highly geo-effective during the main phase of magnetic storms, while it more significant at the time of storm peak, which is further contributed by southward component of IMF Bz, substantiating earlier findings. The correlation between Dst and wind velocity is higher, as compared with IMF Bz and ion density. It has been verified that geomagnetic storm intensity is correlated well with the total magnetic field strength of IMF better than with its southward component.

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X-ray emission from solar flares

Cited by 11 publications

References 18 publications

Energy-Dependent Timing of Thermal Emission in Solar Flares

Energy-Dependent Timing of Thermal Emission in Solar Flares

Microflares as possible sources for coronal heating

A Correlative Study of Geomagnetic Storms Associated with Solar Wind and IMF Features During Solar Cycle 23

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