Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Sako, T.; Watanabe, Kyoko; Muraki, Y.; Matsubara, Y.; Tsujihara, H.; Yamashita, M.; Sakai, Takehiro; Shibata, S.; Galicia, J. F. Valdés; González, L. X.; Hurtado, A.; Musalém, O.; Miranda, P.; Martinic, N.; Ticona, R.; Velarde, A.; Kakimoto, F.; Ogio, S.; Tsunesada, Y.; Tokuno, H.; Tanaka, Yasuyuki; Yoshikawa, Ichiro; Terasawa, T.; Saito, Y.; Mukai, T.; Gros, M.

doi:10.1086/509145

Cited by 41 publications

(27 citation statements)

References 15 publications

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“…They will be attenuated in the Earth's atmosphere (Shibata 1994). We still cover the case if neutrons are produced for more than 20 min as it occurred in the solar neutron event of 7 September 2005 (Sako et al 2006). The remaining two time intervals (2.5 h before and after the onset) of the work window are used to estimate the background.…”

Section: Analysis Methodsmentioning

confidence: 99%

“…Before we proceed with the collected data during the current solar cycle, we applied the analysis method previously described to a solar neutron event that occurred in the past solar cycle. During solar cycle 23, the NMs and SNTs have observed six solar neutron events Sako et al 2006). Here, we will discuss the event which occurred on 7 September 2005 (hereafter the Bolivia-Mexico event).…”

Section: Analysis Methodsmentioning

confidence: 99%

“…In this case, we obtained a significant excess equivalent to 32σ . More details can be found in Sako et al (2006). be produced at the same time (δ-emission) as SXRs.…”

Section: Upper Limit Of the Number Of Solar Neutronsmentioning

confidence: 99%

“…During the declining phase of solar cycle 23, we were able to observe six solar neutron events associated with solar flares Sako et al 2006). Proceeding with our effort to collect more solar neutron events, we directed our attention to the current solar cycle, which started in October 2009 and reached its first peak in August 2013.…”

Section: Introductionmentioning

confidence: 99%

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Search for solar neutrons at Mount Chacaltaya associated with M- and X-class flares during the rising period of solar cycle 24

López

Matsubara

2015

Earth Planet Sp

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To better understand the acceleration mechanism of high-energy particles that are driven by solar flares, we examined solar neutron signals. We have performed a statistical analysis by reviewing the data collected by a neutron monitor during the period of January 2010 to August 2013. This detector operates at Mount Chacaltaya in Bolivia at 5,200 m above sea level. Our aim is to search for solar neutron events in association with large solar flares observed by the GOES satellite. We report that our analysis did not yield any positive excess due to solar neutrons that are statistically significant. Hence, we calculated the upper limit of the number of solar neutrons for the X2.8-class solar flare which occurred on 13 May 2013. We performed a similar calculation with a solar neutron event that occurred on 7 September 2005. Our upper limit is seven times less than the one produced by the real signal.

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Section: Analysis Methodsmentioning

confidence: 99%

Section: Analysis Methodsmentioning

confidence: 99%

“…In this case, we obtained a significant excess equivalent to 32σ . More details can be found in Sako et al (2006). be produced at the same time (δ-emission) as SXRs.…”

Section: Upper Limit Of the Number Of Solar Neutronsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Search for solar neutrons at Mount Chacaltaya associated with M- and X-class flares during the rising period of solar cycle 24

López

Matsubara

2015

Earth Planet Sp

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“…They can travel to the Earth [18], but it is not easy to observe them. Usually, solar neutrons are observed by neutron monitors and solar neutron telescopes located on the Earth [19,20,21]. However, the neutron detectors have to be located on the sunlit side of the Earth, and they have to be able to penetrate through the attenuation caused by the Earth's atmosphere to be detected.…”

Section: Introductionmentioning

confidence: 99%

Capability of the accelerated protons as the origin of white-light emission of solar flare

Watanabe¹,

Masuda²,

Ohno³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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In association with strong solar flares, we sometimes observe enhancements of visible continuum radiation, which is known as a "white-light flare". As most white-light (WL) events show close correlations in time and location with hard X-rays and/or radio emission, there is some consensus that WL emission originates from accelerated particles, especially non-thermal electrons. One model proposes that WL is emitted near the photosphere; however, non-thermal electrons are thermalized in the chromosphere and cannot reach the photosphere. Thus, there is a problem: how can the energy of non-thermal electrons − and/or other accelerated particles such as high-energy protons − propagate to the photosphere and produce WL emission? In the present study, we investigate the possibility that accelerated protons may produce the WL emission of solar flares. We found 51 WL events observed by Hinode/SOT. Among them, gamma-rays with energies greater than 1 MeV were observed only in the X1.8-class flare on October 23, 2012 and in the M7.9-class flare on June 25, 2015. Focusing on these flare events, we compare the energetics of WL emission and of accelerated ion fluxes. We find that it is difficult for accelerated ions to provide sufficient energy to account for WL emission.

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Properties of Energetic Ions in the Solar Atmosphere from γ-Ray and Neutron Observations

Vilmer¹,

MacKinnon²,

Hurford³

2011

High-Energy Aspects of Solar Flares

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Gamma-rays and neutrons are the only sources of information on energetic ions present during solar flares and on properties of these ions when they interact in the solar atmosphere. The production of γ-rays and neutrons results from convolution of the nuclear cross-sections with the ion distribution functions in the atmosphere. The observed γ-ray and neutron fluxes thus provide useful diagnostics for the properties of energetic ions, yielding strong constraints on acceleration mechanisms as well as properties of the interaction sites. The problem of ion transport between the accelerating and interaction sites must also be addressed to infer as much information as possible on the properties of the primary ion accelerator. In the last couple of decades, both theoretical and observational developments have led to substantial progress in understanding the origin of solar γ-rays and neutrons. This chapter reviews recent developments in the study of solar γ-rays and of solar neutrons at the time of the RHESSI era. The unprecedented quality of the RHESSI data reveals γray line shapes for the first time and provides γ-ray images. Our previous understanding of the properties of energetic ions based on measurements from the former solar cycles is also summarized. The new results -obtained owing both to the gain in spectral resolution (both with RHESSI and with the non solar-dedicated INTEGRAL/SPI instrument) and to the pioneering imaging technique in the γ-ray domain -are presented in the context of this previous knowledge. Still open questions are emphasized in the last section of the chapter and future perspectives on this field are briefly discussed.

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Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Cited by 41 publications

References 15 publications

Search for solar neutrons at Mount Chacaltaya associated with M- and X-class flares during the rising period of solar cycle 24

Search for solar neutrons at Mount Chacaltaya associated with M- and X-class flares during the rising period of solar cycle 24

Capability of the accelerated protons as the origin of white-light emission of solar flare

Properties of Energetic Ions in the Solar Atmosphere from γ-Ray and Neutron Observations

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