Detection of Solar Neutrons and Solar Neutron Decay Protons

Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it i...
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Autor*in:	Yasushi Muraki [verfasserIn] Tatsumi Koi [verfasserIn] Satoshi Masuda [verfasserIn] Yutaka Matsubara [verfasserIn] Pedro Miranda [verfasserIn] Shoko Miyake [verfasserIn] Tsuguya Naito [verfasserIn] Ernesto Ortiz [verfasserIn] Akitoshi Oshima [verfasserIn] Takashi Sako [verfasserIn] Shoichi Shibata [verfasserIn] Hisanori Takamaru [verfasserIn] Munetoshi Tokumaru [verfasserIn] Jóse F. Valdés-Galicia [verfasserIn] Kyoko Watanabe [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	solar flare impulsive flare gradual flare solar cosmic rays solar energetic particles particle acceleration

Übergeordnetes Werk:	In: Universe - MDPI AG, 2015, 10(2023), 1, p 16
Übergeordnetes Werk:	volume:10 ; year:2023 ; number:1, p 16

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3390/universe10010016

Katalog-ID:	DOAJ096296011

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allfields	10.3390/universe10010016 doi (DE-627)DOAJ096296011 (DE-599)DOAJ5c4e51cfc6594fea864b82fa920494d2 DE-627 ger DE-627 rakwb eng QC793-793.5 Yasushi Muraki verfasserin aut Detection of Solar Neutrons and Solar Neutron Decay Protons 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare. solar flare impulsive flare gradual flare solar cosmic rays solar energetic particles particle acceleration Elementary particle physics Tatsumi Koi verfasserin aut Satoshi Masuda verfasserin aut Yutaka Matsubara verfasserin aut Pedro Miranda verfasserin aut Shoko Miyake verfasserin aut Tsuguya Naito verfasserin aut Ernesto Ortiz verfasserin aut Akitoshi Oshima verfasserin aut Takashi Sako verfasserin aut Shoichi Shibata verfasserin aut Hisanori Takamaru verfasserin aut Munetoshi Tokumaru verfasserin aut Jóse F. Valdés-Galicia verfasserin aut Kyoko Watanabe verfasserin aut In Universe MDPI AG, 2015 10(2023), 1, p 16 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:10 year:2023 number:1, p 16 https://doi.org/10.3390/universe10010016 kostenfrei https://doaj.org/article/5c4e51cfc6594fea864b82fa920494d2 kostenfrei https://www.mdpi.com/2218-1997/10/1/16 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 10 2023 1, p 16
spelling	10.3390/universe10010016 doi (DE-627)DOAJ096296011 (DE-599)DOAJ5c4e51cfc6594fea864b82fa920494d2 DE-627 ger DE-627 rakwb eng QC793-793.5 Yasushi Muraki verfasserin aut Detection of Solar Neutrons and Solar Neutron Decay Protons 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare. solar flare impulsive flare gradual flare solar cosmic rays solar energetic particles particle acceleration Elementary particle physics Tatsumi Koi verfasserin aut Satoshi Masuda verfasserin aut Yutaka Matsubara verfasserin aut Pedro Miranda verfasserin aut Shoko Miyake verfasserin aut Tsuguya Naito verfasserin aut Ernesto Ortiz verfasserin aut Akitoshi Oshima verfasserin aut Takashi Sako verfasserin aut Shoichi Shibata verfasserin aut Hisanori Takamaru verfasserin aut Munetoshi Tokumaru verfasserin aut Jóse F. Valdés-Galicia verfasserin aut Kyoko Watanabe verfasserin aut In Universe MDPI AG, 2015 10(2023), 1, p 16 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:10 year:2023 number:1, p 16 https://doi.org/10.3390/universe10010016 kostenfrei https://doaj.org/article/5c4e51cfc6594fea864b82fa920494d2 kostenfrei https://www.mdpi.com/2218-1997/10/1/16 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 10 2023 1, p 16
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allfieldsSound	10.3390/universe10010016 doi (DE-627)DOAJ096296011 (DE-599)DOAJ5c4e51cfc6594fea864b82fa920494d2 DE-627 ger DE-627 rakwb eng QC793-793.5 Yasushi Muraki verfasserin aut Detection of Solar Neutrons and Solar Neutron Decay Protons 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare. solar flare impulsive flare gradual flare solar cosmic rays solar energetic particles particle acceleration Elementary particle physics Tatsumi Koi verfasserin aut Satoshi Masuda verfasserin aut Yutaka Matsubara verfasserin aut Pedro Miranda verfasserin aut Shoko Miyake verfasserin aut Tsuguya Naito verfasserin aut Ernesto Ortiz verfasserin aut Akitoshi Oshima verfasserin aut Takashi Sako verfasserin aut Shoichi Shibata verfasserin aut Hisanori Takamaru verfasserin aut Munetoshi Tokumaru verfasserin aut Jóse F. Valdés-Galicia verfasserin aut Kyoko Watanabe verfasserin aut In Universe MDPI AG, 2015 10(2023), 1, p 16 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:10 year:2023 number:1, p 16 https://doi.org/10.3390/universe10010016 kostenfrei https://doaj.org/article/5c4e51cfc6594fea864b82fa920494d2 kostenfrei https://www.mdpi.com/2218-1997/10/1/16 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 10 2023 1, p 16
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authorswithroles_txt_mv	Yasushi Muraki @@aut@@ Tatsumi Koi @@aut@@ Satoshi Masuda @@aut@@ Yutaka Matsubara @@aut@@ Pedro Miranda @@aut@@ Shoko Miyake @@aut@@ Tsuguya Naito @@aut@@ Ernesto Ortiz @@aut@@ Akitoshi Oshima @@aut@@ Takashi Sako @@aut@@ Shoichi Shibata @@aut@@ Hisanori Takamaru @@aut@@ Munetoshi Tokumaru @@aut@@ Jóse F. Valdés-Galicia @@aut@@ Kyoko Watanabe @@aut@@
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callnumber-first	Q - Science
author	Yasushi Muraki
spellingShingle	Yasushi Muraki misc QC793-793.5 misc solar flare misc impulsive flare misc gradual flare misc solar cosmic rays misc solar energetic particles misc particle acceleration misc Elementary particle physics Detection of Solar Neutrons and Solar Neutron Decay Protons
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topic_title	QC793-793.5 Detection of Solar Neutrons and Solar Neutron Decay Protons solar flare impulsive flare gradual flare solar cosmic rays solar energetic particles particle acceleration
topic	misc QC793-793.5 misc solar flare misc impulsive flare misc gradual flare misc solar cosmic rays misc solar energetic particles misc particle acceleration misc Elementary particle physics
topic_unstemmed	misc QC793-793.5 misc solar flare misc impulsive flare misc gradual flare misc solar cosmic rays misc solar energetic particles misc particle acceleration misc Elementary particle physics
topic_browse	misc QC793-793.5 misc solar flare misc impulsive flare misc gradual flare misc solar cosmic rays misc solar energetic particles misc particle acceleration misc Elementary particle physics
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title	Detection of Solar Neutrons and Solar Neutron Decay Protons
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title_full	Detection of Solar Neutrons and Solar Neutron Decay Protons
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author_browse	Yasushi Muraki Tatsumi Koi Satoshi Masuda Yutaka Matsubara Pedro Miranda Shoko Miyake Tsuguya Naito Ernesto Ortiz Akitoshi Oshima Takashi Sako Shoichi Shibata Hisanori Takamaru Munetoshi Tokumaru Jóse F. Valdés-Galicia Kyoko Watanabe
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title_sort	detection of solar neutrons and solar neutron decay protons
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title_auth	Detection of Solar Neutrons and Solar Neutron Decay Protons
abstract	Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare.
abstractGer	Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare.
abstract_unstemmed	Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare.
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title_short	Detection of Solar Neutrons and Solar Neutron Decay Protons
url	https://doi.org/10.3390/universe10010016 https://doaj.org/article/5c4e51cfc6594fea864b82fa920494d2 https://www.mdpi.com/2218-1997/10/1/16 https://doaj.org/toc/2218-1997
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author2	Tatsumi Koi Satoshi Masuda Yutaka Matsubara Pedro Miranda Shoko Miyake Tsuguya Naito Ernesto Ortiz Akitoshi Oshima Takashi Sako Shoichi Shibata Hisanori Takamaru Munetoshi Tokumaru Jóse F. Valdés-Galicia Kyoko Watanabe
author2Str	Tatsumi Koi Satoshi Masuda Yutaka Matsubara Pedro Miranda Shoko Miyake Tsuguya Naito Ernesto Ortiz Akitoshi Oshima Takashi Sako Shoichi Shibata Hisanori Takamaru Munetoshi Tokumaru Jóse F. Valdés-Galicia Kyoko Watanabe
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up_date	2024-07-03T19:22:16.881Z
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Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). 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Detection of Solar Neutrons and Solar Neutron Decay Protons

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