Gamma-ray spectral observations with YOHKOH

Yoshimori, M.; Suga, K.; Morimoto, K.; Hiraoka, T.; Sato, Jun; Kawabata, K.; Ohki, K.

doi:10.1086/191885

Cited by 23 publications

(5 citation statements)

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“…A comprehensive treatment of nuclear deexcitation gamma-ray line emission was given by Ramaty, Kozlovsky & Lingenfelter (1979) (hereafter RKL). This treatment has provided the theoretical framework for numerous investigations of gamma-ray lines observed with various space missions including the Solar Maximum Mission/Gamma Ray Spectrometer (Chupp 1984;Murphy et al 1991;Share & Murphy 1995), all four Compton Gamma Ray Observatory (CGRO) instruments , Hinotori (Yoshimori 1990), Yohkoh (Yoshimori et al 1994), GAMMA-1 (Leikov et al 1993) and GRANAT/Phebus (Trottet et al 1996). The results of these efforts have established gamma-ray spectroscopy as an important tool for exploration of high-energy processes in solar flares.…”

Section: Introductionmentioning

confidence: 99%

Nuclear Deexcitation Gamma‐Ray Lines from Accelerated Particle Interactions

Kozlovsky

Murphy

Ramaty

2002

ASTROPHYS J SUPPL S

142

161

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Total cross sections for the production of gamma-ray lines from nuclear deexcitation as a function of the projectile energy are evaluated and presented. Included are proton and α reactions with He, C, N, O, Ne, Mg, Al, Si, S, Ca and Fe. Such functions are essential for interpretation of gamma-ray line observations of astrophysical sites which contain large fluxes of energetic particles such as solar flares, the Earth's atmosphere, planetary atmospheres and surfaces, the interstellar medium and galactic nebulae.

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Section: Introductionmentioning

confidence: 99%

Nuclear Deexcitation Gamma‐Ray Lines from Accelerated Particle Interactions

Kozlovsky

Murphy

Ramaty

2002

ASTROPHYS J SUPPL S

142

161

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“…Recently, a variety of detailed SMM gamma-ray data have become available (Share & Murphy 1995, 1999. During the peak of solar cycle 22, solar-flare gamma-ray observations were carried out with the CGRO instruments OSSE , COMPTEL (Ryan & McConnell 1996), EGRET (Kanbach et al 1993;Mandzhavidze et al 1996;Dunphy et al 1999), and BATSE/CPD (charged particle detector; Ramaty et al 1994), as well as with the PHEBUS instrument on Granat (Barat et al 1994) and the gamma-ray spectrometer on Yohkoh (Yoshimori et al 1994). During the current maximum of cycle 23, both the CGRO and Yohkoh instruments continue to be operational, and, starting in 2000, observations with the imaging Ge spectrometer HESSI (Lin et al 1998) should become available.…”

Section: Introductionmentioning

confidence: 99%

Gamma-rays from Solar Flares

Ramaty¹,

Mandzhavidze²

2000

Symp. - Int. Astron. Union

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Abstract. Gamma-ray emission is the most direct diagnostic of energetic ions and relativistic electrons in solar flares. Analysis of solar flare gamma-ray data has shown: (i) ion acceleration is a major consequence of flare energy release, as the total flare energy in accelerated particles appears to be equipartitioned between~1 MeV/nucleon ions and~20 keV electrons, and amounts to an important fraction of the total energy release; (ii) there are flares for which over 50% of the energy is in Q particles and heavier ions; (iii) in both impulsive and gradual flares, the particles that interact at the Sun and produce gamma rays are essentially always accelerated by the same mechanism that operates in impulsive flares, probably stochastic acceleration through gyroresonant wave particle interaction; and (iv) gamma-ray spectroscopy can provide new information on solar abundances, for example the site of the FIP-bias onset and the photospheric 3He abundance. We propose a new technique for the investigation of mass motion and mixing in the solar atmosphere: the observations of gamma-ray lines from long-term radioactivity produced by flare accelerated particles.

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“…Prior to the launch o f t h e COMPTON Gamma Ray Observatory CGRO, most solar -ray line measurements had been made with the Solar Maximum Mission, Hinotori, Yohkoh, and GRANAT -ray spectrometers e.g., Chupp 1987;Yoshimori 1989;Yoshimori 1994;Vilmer 1994. With the launch of the CGRO in April of 1991, a new resource for high-energy solar measurements became available.…”

Section: Introductionmentioning

confidence: 99%

Accelerated Particle Composition and Energetics and Ambient Abundances from Gamma‐Ray Spectroscopy of the 1991 June 4 Solar Flare

Murphy

Grove

et al. 1997

ApJ

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The Oriented Scintillation Spectrometer Experiment OSSE on board the COMPTON Gamma Ray Observatory observed the 1991 June 4 X12+ solar are, one of the most intense nuclear gamma-ray line ares observed to date. Using these OSSE observations, we h a v e derived time pro les of the various components of gamma-ray emission and obtained information about the accelerated particle spectra and composition and about the ambient plasma at the are site. The main results are: 1 the nuclear reactions associated with the impulsive phase of the are continued for at least 2 hours and resulted from ions that were probably continuously accelerated rather than impulsively accelerated and trapped; 2 the total energy in these accelerated ions exceeded the energy in 0.1 MeV electrons; 3 the accelerated proton ratio was closer to 0.5 than to 0.1; 4 there is evidence for a decrease of the accelerated heavy ion-to-proton ratio as the are progressed 5 there is evidence for a temporal change in the composition of the are plasma; 6 the ratio of electron bremsstrahlung to the ux in narrow-ray lines decreased as the are progressed; 7 the high-energy 16 MeV component of the electron spectrum was much more impulsive than the lower-energy MeV component; 8 a model-dependent upper limit of 2.3 10 ,5 was obtained for the photospheric 3 He H abundance ratio; and 9 energetic ions may h a v e been present for several hours prior to and following the impulsive phase of the are.

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Gamma-ray spectral observations with YOHKOH

Cited by 23 publications

References 0 publications

Nuclear Deexcitation Gamma‐Ray Lines from Accelerated Particle Interactions

Nuclear Deexcitation Gamma‐Ray Lines from Accelerated Particle Interactions

Gamma-rays from Solar Flares

Accelerated Particle Composition and Energetics and Ambient Abundances from Gamma‐Ray Spectroscopy of the 1991 June 4 Solar Flare

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