Solar Neutron Event in Association with a Large Solar Flare on 2000 November 24

Watanabe, Kyoko; Muraki, Y.; Matsubara, Y.; Murakami, Kazuaki; Sako, T.; Tsuchiya, H.; Masuda, S.; Yoshimori, M.; Ohmori, N.; Miranda, P.; Martinic, N.; Ticona, R.; Velarde, A.; Kakimoto, F.; Ogio, S.; Tsunesada, Y.; Tokuno, H.; Shirasaki, Y.

doi:10.1086/375685

Cited by 30 publications

(59 citation statements)

References 21 publications

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“…a In solar cycle 23, the 24 November 2000 (Watanabe et al 2003) solar neutron event detected by the NM-64 was the smallest X-class among the six successful detections in this solar cycle.…”

Section: Endnotementioning

confidence: 99%

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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“…a In solar cycle 23, the 24 November 2000 (Watanabe et al 2003) solar neutron event detected by the NM-64 was the smallest X-class among the six successful detections in this solar cycle.…”

Section: Endnotementioning

confidence: 99%

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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“…Hereafter we define T PS = t P − t S . Both these cases have been considered in some past studies (Chupp et al 1982;Muraki et al 1992;Shibata 1994;Watanabe et al 2003;Bieber et al 2005). (981128) flares, respectively, while left-lower and right-lower panels indicate those for the M3.9 (990604) and M2.0 (000408) flares, respectively.…”

Section: Nm Light Curvesmentioning

confidence: 99%

“…This is because the light curves of the 4-7 MeV nuclear gamma-ray emission, which obviously reflect ion acceleration at the Sun, are approximately described by a Gaussian function (e.g., Chupp et al 1990;Watanabe et al 2003). Furthermore, according to various solar X-ray and gamma-ray observations (e.g., Forrest & Chupp 1983;Watanabe et al 2006), the rise and peak times of the 4-7 MeV nuclear gamma-ray light curve are roughly similar to those of the HXR emission.…”

Section: Nm Light Curvesmentioning

confidence: 99%

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Upper limits on the solar-neutron flux at the Yangbajing neutron monitor from BATSE-detected solar flares

Tsuchiya

Miyasaka

Takahashi

et al. 2007

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Aims. The purpose of this work is to search the data from Yangbajing neutron monitor obtained between 1998 October and 2000 June for the solar neutrons associated with solar flares. Methods. Using the onset times of 166 BATSE-detected flares with the GOES peak flux (1-8 Å) higher than 1.0 × 10 −5 Wm −2 , we prepared a light curve of the Yangbajing neutron monitor for each flare, spanning ±1.5 h from the BATSE onset time. Based on the light curves, a systematic search for solar neutrons in energies above 100 MeV from the 166 flares was performed. No statistically significant signals due to solar neutrons were found. Therefore, we put upper limits on the ≥100 MeV solar-neutron flux for 18 events consisting of 2 X and 16 M class flares. The calculation assumed a power-law shaped neutron energy spectrum and three types of neutron emission profiles at the Sun. Results. Compared with the other positive neutron detections associated with X-class flares, typical 95% confidence level upper limits for the two X-class flares are found to be comparable to the lowest and second lowest neutron fluxes at the top of the atmosphere. In addition, the upper limits for M-class flares scatter in the range of 10 −2 to 1 neutrons cm −2 s −1 . This provides the first upper limits on the solar-neutron flux from M-class solar flares, using space observatories, as well as ground-based neutron monitors.

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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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Solar Neutron Event in Association with a Large Solar Flare on 2000 November 24

Cited by 30 publications

References 21 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

Upper limits on the solar-neutron flux at the Yangbajing neutron monitor from BATSE-detected solar flares

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

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