Gamma-ray radiation with energy 2.223 MeV and the density distribution in the solar atmosphere during flares

Kuzhevskij, B. M.; Miroshnichenko, L. I.; Troitskaia, E. V.

doi:10.1134/1.1985954

Cited by 10 publications

(19 citation statements)

References 19 publications

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“…Model 5 presents the enhanced density in the most part of depths interval under consideration. In our study we used in the calculations only models 1 and 5 -see figure 2 [4,8]. Model 5 is a specially selected form best describes the vertical profile of the density of the solar atmosphere during flares and is combined of dashed part and two parts of model 1.…”

Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

“…Model 5 is a specially selected form best describes the vertical profile of the density of the solar atmosphere during flares and is combined of dashed part and two parts of model 1. Modeling technique of such flares, for example, was developed in [8,9,12,13]. Now we apply our method to the flare under consideration.…”

Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

“…At the figures 3 (a, b) we present the comparison of the observable data and calculated ones in the supposition of usual average concentration ratio κ=n( 3 Не)/n(Н)=2×10 -5 , m is number of the solar atmosphere density model and T is accelerated ions spectral index. Preliminary consideration of this case was done in [8]. Figures show the graphs of models with uniform angular distribution in the lower hemisphere of neutron ejection.…”

Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

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The results of January 20, 2005 solar flare study by narrow gamma lines

Troitskaya

Arkhangelskaja

Arkhangelskiy

2017

J. Phys.: Conf. Ser.

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Abstract.We have studied some properties of the powerful solar flare of January 20, 2005 by methods of nuclear lines analysis. The results of temporal profiles investigation in corresponding to neutron capture energy bands allow the supposition about predominant acceleration of 3 He ions in the corona, their subsequent propagation to the low chromosphere and the photosphere where the area of 2.223 MeV γ-line effective productions is located. The characteristics of accelerated 3 He ions propagation processes and the basic explanation of observable properties of this solar flare due to the variations of 3 He content are discussed in the presented article.

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Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

Section: January 20 2005 Event As 3 He-reach Flarementioning

confidence: 99%

See 1 more Smart Citation

The results of January 20, 2005 solar flare study by narrow gamma lines

Troitskaya

Arkhangelskaja

Arkhangelskiy

2017

J. Phys.: Conf. Ser.

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“…The idea of such an approach was first suggested in 1986 (see Kuzhevskij and Troitskaia, 1995). Later on, by using 2.223-MeV line data on two large flares, 6 November 1997 and 22 March 1991, some evidence of the effect of density enhancement (EDE) under the flare site was obtained (Kuzhevskij, Miroshnichenko, and Troitskaia, 2005).…”

Section: Introductionmentioning

confidence: 97%

“…More recently, Kuzhevskij, Kuzhetsov, and Troitskaia (1998), , Troitskaia (2001, 2002), Gan et al (2003), Troitskaia et al (2003) and Kuzhevskij, Miroshnichenko, and Troitskaia (2005) have developed a new independent approach (SINP code) to determine, by the time profile data of the 2.223-MeV line, the most probable profile of plasma density in the solar photosphere and adjoining levels during the period of a flare. The idea of such an approach was first suggested in 1986 (see Kuzhevskij and Troitskaia, 1995).…”

Section: Introductionmentioning

confidence: 98%

Solar Plasma Density and Spectrum of Accelerated Particles Derived From the 2.223-Mev Line of a Solar Flare

et al. 2007

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The time profile of the neutron capture line of 2.223 MeV for the flare of 16 December 1988 (its third peak) is analyzed. The enhancements of plasma density in the deep photospheric layers of the Sun under the flare region (an effect of density enhancement) have been deduced by the SINP calculation code. These enhancements are studied based on several modified models of the lower chromosphere, photosphere, and convection zone. Additionally, the case has been examined when the neutron source is placed at the top of the photosphere. The energy spectrum of accelerated particles (protons) is shown to evolve with time. Assuming a stochastic mechanism of acceleration and a Bessel function for the spectrum, we find the spectral index αT to increase from 0.005 to 0.1 during the decay phase of the burst; i.e., the proton spectrum becomes harder. Density enhancements found in the flare of 16 December 1988 are consistent with our previous results on the density enhancement effects deduced for two other flares, 6 November 1997 and 22 March 1991. It is suggested that density enhancements in the deep layers of the photosphere may be rather common features of powerful solar flares. B.M. Kuzhevskij is deseased. E.V. Troitskaia ( ) · B.M. Kuzhevskij

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Solar Cosmic Rays

Miroshnichenko

2015

Astrophysics and Space Science Library

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Gamma-ray radiation with energy 2.223 MeV and the density distribution in the solar atmosphere during flares

Cited by 10 publications

References 19 publications

The results of January 20, 2005 solar flare study by narrow gamma lines

The results of January 20, 2005 solar flare study by narrow gamma lines

Solar Plasma Density and Spectrum of Accelerated Particles Derived From the 2.223-Mev Line of a Solar Flare

Solar Cosmic Rays

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