Origin of the soft X-ray emission after the impulsive phase of the March 26, 1991 solar flare

V. V. Akimov; H. Garsia; K. V. Getman; V. Kurt; M. A. Livshits

Origin of the soft X-ray emission after the impulsive phase of the March 26, 1991 solar flare

V. V. Akimov, H. Garsia, K. V. Getman, V. Kurt, M. A. Livshits

Astronomy & Astrophysics

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Abstract

This study is based on the GOES soft Χ-ray measurements in two energy bands for the March 26, 1991 solar flare. The hard γ-ray measurements during this flare suggest an additional energy release after the impulsive phase (Akimov et al. 1994). The Χ-ray data are used to determine the time behavior of the temperature and emission measure in the γ-ray source for the entire event. Based on a numerical solution of the system of gas-dynamical equations, we consider the energy balance in the source. We have found that the observed time behavior of the temperature in the second flare phase can be modeled only by assuming that there is additional heating of the upper part of the loop. The density at the top of the loop is 3 x 10¹⁰ cm^-3.

Original language	English (US)
Pages (from-to)	42-45
Number of pages	4
Journal	Astronomy Letters
Volume	25
Issue number	1
State	Published - Jan 1 1999

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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title = "Origin of the soft X-ray emission after the impulsive phase of the March 26, 1991 solar flare",

abstract = "This study is based on the GOES soft Χ-ray measurements in two energy bands for the March 26, 1991 solar flare. The hard γ-ray measurements during this flare suggest an additional energy release after the impulsive phase (Akimov et al. 1994). The Χ-ray data are used to determine the time behavior of the temperature and emission measure in the γ-ray source for the entire event. Based on a numerical solution of the system of gas-dynamical equations, we consider the energy balance in the source. We have found that the observed time behavior of the temperature in the second flare phase can be modeled only by assuming that there is additional heating of the upper part of the loop. The density at the top of the loop is 3 x 1010 cm-3.",

author = "Akimov, {V. V.} and H. Garsia and Getman, {K. V.} and V. Kurt and Livshits, {M. A.}",

year = "1999",

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T1 - Origin of the soft X-ray emission after the impulsive phase of the March 26, 1991 solar flare

AU - Akimov, V. V.

AU - Garsia, H.

AU - Getman, K. V.

AU - Kurt, V.

AU - Livshits, M. A.

PY - 1999/1/1

Y1 - 1999/1/1

N2 - This study is based on the GOES soft Χ-ray measurements in two energy bands for the March 26, 1991 solar flare. The hard γ-ray measurements during this flare suggest an additional energy release after the impulsive phase (Akimov et al. 1994). The Χ-ray data are used to determine the time behavior of the temperature and emission measure in the γ-ray source for the entire event. Based on a numerical solution of the system of gas-dynamical equations, we consider the energy balance in the source. We have found that the observed time behavior of the temperature in the second flare phase can be modeled only by assuming that there is additional heating of the upper part of the loop. The density at the top of the loop is 3 x 1010 cm-3.

AB - This study is based on the GOES soft Χ-ray measurements in two energy bands for the March 26, 1991 solar flare. The hard γ-ray measurements during this flare suggest an additional energy release after the impulsive phase (Akimov et al. 1994). The Χ-ray data are used to determine the time behavior of the temperature and emission measure in the γ-ray source for the entire event. Based on a numerical solution of the system of gas-dynamical equations, we consider the energy balance in the source. We have found that the observed time behavior of the temperature in the second flare phase can be modeled only by assuming that there is additional heating of the upper part of the loop. The density at the top of the loop is 3 x 1010 cm-3.

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Origin of the soft X-ray emission after the impulsive phase of the March 26, 1991 solar flare

Abstract

All Science Journal Classification (ASJC) codes

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