High sensitivity search for (ν)over-bare's from the Sun and other sources at KamLAND -: art. no. 071301

被引：137

作者：

Eguchi, K ^{[1
]}

Enomoto, S

Furuno, K

Ikeda, H

Ikeda, K

Inoue, K

Ishihara, K

Iwamoto, T

Kawashima, T

Kishimoto, Y

Koga, M

Koseki, Y

Maeda, T

Mitsui, T

Motoki, M

Nakajima, K

Ogawa, H

Owada, K

Piquemal, F

Shimizu, I

Shirai, J

Suekane, F

Suzuki, A

Tada, K

Tajima, O

Takayama, T

Tamae, K

Watanabe, H

Busenitz, J

Djurcic, Z

McKinny, K

Mei, DM

Piepke, A

Yakushev, E

Berger, BE

Chan, YD

Decowski, MP

Dwyer, DA

Freedman, SJ

Fu, Y

Fujikawa, BK

Goldman, J

Heeger, KM

Lesko, KT

Luk, KB

Murayama, H

Nygren, DR

Okada, CE

Poon, AWP

Steiner, HM

机构：

[1] Tohoku Univ, Res Ctr Neutrino Sci, Sendai, Miyagi 9808578, Japan

[2] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA

[3] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[4] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA

[5] CALTECH, WK Kellogg Radiat Lab, Pasadena, CA 91125 USA

[6] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA

[7] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA

[8] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

[9] Univ New Mexico, Dept Phys, Albuquerque, NM 87131 USA

[10] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[11] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA

[12] Triangle Univ Nucl Lab, Durham, NC 27708 USA

[13] Duke Univ, Dept Phys, Durham, NC 27706 USA

[14] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA

[15] Univ N Carolina, Dept Phys, Chapel Hill, NC 27514 USA

[16] Inst High Energy Phys, Beijing 100039, Peoples R China

来源：

PHYSICAL REVIEW LETTERS | 2004年 / 92卷 / 07期

关键词：

D O I：

10.1103/PhysRevLett.92.071301

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Data corresponding to a KamLAND detector exposure of 0.28 kton yr has been used to search for (v) over bar (e)'s in the energy range 8.3<E-(v) over bare<14.8 MeV. No candidates were found for an expected background of 1.1+/-0.4 events. This result can be used to obtain a limit on (v) over bar (e) fluxes of any origin. Assuming that all (v) over bar (e) flux has its origin in the Sun and has the characteristic B-8 solar nu(e) energy spectrum, we obtain an upper limit of 3.7x10(2) cm(-2) s(-1) (90% C.L.) on the (v) over bar (e) flux. We interpret this limit, corresponding to 2.8x10(-4) of the standard solar model B-8 nu(e) flux, in the framework of spin-flavor precession and neutrino decay models.

引用

页数：5

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