Possible evidence for >= 10 GeV neutrons associated with the solar flare of 4 June 1991

被引：41

作者：

Chiba, N. ^{[2
]}

Dion, G. M. ^{[1
]}

Hayashida, N. ^{[1
]}

Honda, K. ^{[3
]}

Honda, M. ^{[1
]}

Inoue, N. ^{[4
]}

Kadota, K. ^{[5
]}

Kakimoto, F. ^{[5
]}

Kamata, K. ^{[6
]}

Kawaguchi, S. ^{[2
]}

Kawasumi, N. ^{[3
]}

Matsubara, Y. ^{[1
]}

Nagano, M. ^{[1
]}

Ohoka, H. ^{[1
]}

Teshima, M. ^{[1
]}

Tsushima, I. ^{[3
]}

Yoshida, S. ^{[5
]}

Yoshii, H. ^{[7
]}

Yoshikoshi, T. ^{[5
]}

机构：

[1] Univ Tokyo, Inst Cosm Ray Res, Tanashi, Tokyo 188, Japan

[2] Hirosaki Univ, Fac Gen Educ, Hirosaki, Aomori, Japan

[3] Yamanashi Univ, Fac Educ, Kofu, Yamanashi 400, Japan

[4] Saitama Univ, Dept Phys, Urawa, Saitama 338, Japan

[5] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 152, Japan

[6] Nishina Mem Fdn, Tokyo, Japan

[7] Ehime Univ, Fac Gen Educ, Matsuyama, Ehime, Japan

来源：

ASTROPARTICLE PHYSICS | 1992年 / 1卷 / 01期

关键词：

D O I：

10.1016/0927-6505(92)90006-L

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Neutrons associated with the solar flare of 4 June 1991 were observed by scintillation detectors of the Akeno Giant Air Shower Array (AGASA), which is about 900 m above sea level (920 g/cm(2)). The total area of plastic scintillators used for the present analysis is 182.6 m(2) and the excess counting rate is (0.35 +/- 0.1) per m(2)s. From attenuation of counting rates observed by scintillation detectors at Mt. Norikura and at Akeno, the excess signals can be interpreted as muons produced in the upper atmosphere by solar neutrons of energies above 10 GeV. The flux of solar neutrons above 10 GeV is about 1 similar to 2 per m(2)s at the top of the atmosphere and lasted for more than 20 minutes after the solar flare.

引用

页码：27 / 32

页数：6

共 12 条

[1] AKENO GIANT AIR SHOWER ARRAY (AGASA) COVERING 100 KM2 AREA [J].

CHIBA, N ;

HASHIMOTO, K ;

HAYASHIDA, N ;

HONDA, K ;

HONDA, M ;

INOUE, N ;

KAKIMOTO, F ;

KAMATA, K ;

KAWAGUCHI, S ;

KAWASUMI, N ;

MATSUBARA, Y ;

MURAKAMI, K ;

NAGANO, M ;

OGIO, S ;

OHOKA, H ;

SAITO, T ;

SAKUMA, Y ;

TSUSHIMA, I ;

TESHIMA, M ;

UMEZAWA, T ;

YOSHIDA, S ;

YOSHII, H .

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, 1992, 311 (1-2) :338-349

[2]

Hayashida N., 1991, P 22 INT COSM RAY C, V1, P309

[3]

Murakami K., 1979, Nuovo Cimento C, V2C, P635, DOI 10.1007/BF02557762

[4]

Murakami K., 1981, 6 NAG U COSM RAY LAB

[5]

Muraki Y., 1991, ICRRREPORT2489117 U

[6] GALACTIC COSMIC-RAY ANISOTROPY AND ITS MODULATION IN THE HELIOMAGNETOSPHERE, INFERRED FROM AIR SHOWER OBSERVATION AT MT NORIKURA [J].

NAGASHIMA, K ;

FUJIMOTO, K ;

SAKAKIBARA, S ;

FUJII, Z ;

UENO, H ;

MORISHITA, I ;

MURAKAMI, K .

NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-GEOPHYSICS AND SPACE PHYSICS, 1989, 12 (06) :695-749

[7]

Sakakibara S., 1991, COMMUNICATION

[8]

Sakakibara S., 1991, S STUD HEL SOL TERR, P47

[9]

Schwartz R.A., 1992, COMPTON OBSERVATORY, V3137, P457

[10]

Shibata S., 1992, COMMUNICATION

← 1 2 →