Electron antineutrino search at the Sudbury Neutrino Observatory

B. Aharmim; S. N. Ahmed; E. W. Beier; A. Bellerive; S. D. Biller; J. Boger; M. G. Boulay; T. J. Bowles; S. J. Brice; T. V. Bullard; Y. D. Chan; M. Chen; X. Chen; B. T. Cleveland; G. A. Cox; X. Dai; F. Dalnoki-Veress; P. J. Doe; R. S. Dosanjh; G. Doucas; M. R. Dragowsky; C. A. Duba; F. A. Duncan; M. Dunford; J. A. Dunmore; E. D. Earle; S. R. Elliott; H. C. Evans; G. T. Ewan; J. Farine; H. Fergani; F. Fleurot; J. A. Formaggio; M. M. Fowler; K. Frame; W. Frati; B. G. Fulsom; N. Gagnon; K. Graham; D. R. Grant; R. L. Hahn; A. L. Hallin; E. D. Hallman; A. S. Hamer; W. B. Handler; C. K. Hargrove; P. J. Harvey; R. Hazama; K. M. Heeger; W. J. Heintzelman; J. Heise; R. L. Helmer; R. J. Hemingway; A. Hime; M. A. Howe; P. Jagam; N. A. Jelley; J. R. Klein; L. L. Kormos; M. S. Kos; A. Krüger; C. B. Krauss; A. V. Krumins; T. Kutter; C. C.M. Kyba; H. Labranche; R. Lange; J. Law; I. T. Lawson; K. T. Lesko; J. R. Leslie; I. Levine; S. Luoma; R. MacLellan; S. Majerus; H. B. Mak; J. Maneira; A. D. Marino; N. McCauley; A. B. McDonald; S. McGee; G. McGregor; C. Mifflin; K. K.S. Miknaitis; G. G. Miller; B. A. Moffat; C. W. Nally; M. S. Neubauer; B. G. Nickel; A. J. Noble; E. B. Norman; N. S. Oblath; C. E. Okada; R. W. Ollerhead; J. L. Orrell; S. M. Oser; C. Ouellet; S. J.M. Peeters; A. W.P. Poon; K. Rielage; B. C. Robertson; R. G.H. Robertson; E. Rollin; S. S.E. Rosendahl; V. L. Rusu; M. H. Schwendener; O. Simard; J. J. Simpson; C. J. Sims; D. Sinclair; P. Skensved; M. W.E. Smith; N. Starinsky; R. G. Stokstad; L. C. Stonehill; R. Tafirout; Y. Takeuchi; G. Tešić; M. Thomson; T. Tsui; R. Van Berg; R. G. Van de Water; C. J. Virtue; B. L. Wall; D. Waller; C. E. Waltham; H. Wan Chan Tseung; D. L. Wark; N. West; J. B. Wilhelmy; J. F. Wilkerson; J. R. Wilson; P. Wittich; J. M. Wouters; M. Yeh; K. Zuber

doi:10.1103/PhysRevD.70.093014

Electron antineutrino search at the Sudbury Neutrino Observatory

B. Aharmim
, S. N. Ahmed
, E. W. Beier
, A. Bellerive
, S. D. Biller
, J. Boger
, M. G. Boulay
, T. J. Bowles
, S. J. Brice
, T. V. Bullard
, Y. D. Chan
, M. Chen
, X. Chen
, B. T. Cleveland
, G. A. Cox
, X. Dai
, F. Dalnoki-Veress
, P. J. Doe
, R. S. Dosanjh
, G. Doucas

M. R. Dragowsky, C. A. Duba, F. A. Duncan, M. Dunford, J. A. Dunmore, E. D. Earle, S. R. Elliott, H. C. Evans, G. T. Ewan, J. Farine, H. Fergani, F. Fleurot, J. A. Formaggio, M. M. Fowler, K. Frame, W. Frati, B. G. Fulsom, N. Gagnon, K. Graham, D. R. Grant, R. L. Hahn, A. L. Hallin, E. D. Hallman, A. S. Hamer, W. B. Handler, C. K. Hargrove, P. J. Harvey, R. Hazama, K. M. Heeger, W. J. Heintzelman, J. Heise, R. L. Helmer, R. J. Hemingway, A. Hime, M. A. Howe, P. Jagam, N. A. Jelley, J. R. Klein, L. L. Kormos, M. S. Kos, A. Krüger, C. B. Krauss, A. V. Krumins, T. Kutter, C. C.M. Kyba, H. Labranche, R. Lange, J. Law, I. T. Lawson, K. T. Lesko, J. R. Leslie, I. Levine, S. Luoma, R. MacLellan, S. Majerus, H. B. Mak, J. Maneira, A. D. Marino, N. McCauley, A. B. McDonald, S. McGee, G. McGregor, C. Mifflin, K. K.S. Miknaitis, G. G. Miller, B. A. Moffat, C. W. Nally, M. S. Neubauer, B. G. Nickel, A. J. Noble, E. B. Norman, N. S. Oblath, C. E. Okada, R. W. Ollerhead, J. L. Orrell, S. M. Oser, C. Ouellet, S. J.M. Peeters, A. W.P. Poon, K. Rielage, B. C. Robertson, R. G.H. Robertson, E. Rollin, S. S.E. Rosendahl, V. L. Rusu, M. H. Schwendener, O. Simard, J. J. Simpson, C. J. Sims, D. Sinclair, P. Skensved, M. W.E. Smith, N. Starinsky, R. G. Stokstad, L. C. Stonehill, R. Tafirout, Y. Takeuchi, G. Tešić, M. Thomson, T. Tsui, R. Van Berg, R. G. Van de Water, C. J. Virtue, B. L. Wall, D. Waller, C. E. Waltham, H. Wan Chan Tseung, D. L. Wark, N. West, J. B. Wilhelmy, J. F. Wilkerson, J. R. Wilson, P. Wittich, J. M. Wouters, M. Yeh, K. Zuber

Producción científica: Article › revisión exhaustiva

43 Citas (Scopus)

Resumen

Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.

Idioma original	English
Publicación	Physical Review D - Particles, Fields, Gravitation and Cosmology
Volumen	70
N.º	9
DOI	https://doi.org/10.1103/PhysRevD.70.093014
Estado	Published - 2004

Nota bibliográfica

Funding Information:
This research was supported by the Natural Sciences and Engineering Research Council, Canada; Industry Canada; National Research Council, Canada; Northern ?> ?>Ontario Heritage Fund Corporation, Inco, Canada; ?> ?>Atomic Energy of Canada, Ltd.; Ontario Power ?> ?>Generation; the U.S. Department. of Energy; and ?> ?>Particle Physics and Astronomy Research Council, ?> ?>United Kingdom. We thank the SNO technical staff for ?> ?>their strong contributions.

Financiación

This research was supported by the Natural Sciences and Engineering Research Council, Canada; Industry Canada; National Research Council, Canada; Northern ?> ?>Ontario Heritage Fund Corporation, Inco, Canada; ?> ?>Atomic Energy of Canada, Ltd.; Ontario Power ?> ?>Generation; the U.S. Department. of Energy; and ?> ?>Particle Physics and Astronomy Research Council, ?> ?>United Kingdom. We thank the SNO technical staff for ?> ?>their strong contributions.

Financiadores
National Research Council Canada (NRCC)
Natural Sciences and Engineering Research Council of Canada
Industry Canada

ASJC Scopus subject areas

Nuclear and High Energy Physics
Physics and Astronomy (miscellaneous)

Acceder al documento

10.1103/PhysRevD.70.093014

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Aharmim, B., Ahmed, S. N., Beier, E. W., Bellerive, A., Biller, S. D., Boger, J., Boulay, M. G., Bowles, T. J., Brice, S. J., Bullard, T. V., Chan, Y. D., Chen, M., Chen, X., Cleveland, B. T., Cox, G. A., Dai, X., Dalnoki-Veress, F., Doe, P. J., Dosanjh, R. S., ... Zuber, K. (2004). Electron antineutrino search at the Sudbury Neutrino Observatory. Physical Review D - Particles, Fields, Gravitation and Cosmology, 70(9). https://doi.org/10.1103/PhysRevD.70.093014

@article{ef90785b6181425a818ef2080ecec6b9,

title = "Electron antineutrino search at the Sudbury Neutrino Observatory",

abstract = "Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]{\textquoteright}s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]{\textquoteright}s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90\% C.L.), which corresponds to 0.81\% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90\% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]{\textquoteright}s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90\% C.L.) is obtained.",

author = "B. Aharmim and Ahmed, \{S. N.\} and Beier, \{E. W.\} and A. Bellerive and Biller, \{S. D.\} and J. Boger and Boulay, \{M. G.\} and Bowles, \{T. J.\} and Brice, \{S. J.\} and Bullard, \{T. V.\} and Chan, \{Y. D.\} and M. Chen and X. Chen and Cleveland, \{B. T.\} and Cox, \{G. A.\} and X. Dai and F. Dalnoki-Veress and Doe, \{P. J.\} and Dosanjh, \{R. S.\} and G. Doucas and Dragowsky, \{M. R.\} and Duba, \{C. A.\} and Duncan, \{F. A.\} and M. Dunford and Dunmore, \{J. A.\} and Earle, \{E. D.\} and Elliott, \{S. R.\} and Evans, \{H. C.\} and Ewan, \{G. T.\} and J. Farine and H. Fergani and F. Fleurot and Formaggio, \{J. A.\} and Fowler, \{M. M.\} and K. Frame and W. Frati and Fulsom, \{B. G.\} and N. Gagnon and K. Graham and Grant, \{D. R.\} and Hahn, \{R. L.\} and Hallin, \{A. L.\} and Hallman, \{E. D.\} and Hamer, \{A. S.\} and Handler, \{W. B.\} and Hargrove, \{C. K.\} and Harvey, \{P. J.\} and R. Hazama and Heeger, \{K. M.\} and Heintzelman, \{W. J.\} and J. Heise and Helmer, \{R. L.\} and Hemingway, \{R. J.\} and A. Hime and Howe, \{M. A.\} and P. Jagam and Jelley, \{N. A.\} and Klein, \{J. R.\} and Kormos, \{L. L.\} and Kos, \{M. S.\} and A. Kr{\"u}ger and Krauss, \{C. B.\} and Krumins, \{A. V.\} and T. Kutter and Kyba, \{C. C.M.\} and H. Labranche and R. Lange and J. Law and Lawson, \{I. T.\} and Lesko, \{K. T.\} and Leslie, \{J. R.\} and I. Levine and S. Luoma and R. MacLellan and S. Majerus and Mak, \{H. B.\} and J. Maneira and Marino, \{A. D.\} and N. McCauley and McDonald, \{A. B.\} and S. McGee and G. McGregor and C. Mifflin and Miknaitis, \{K. K.S.\} and Miller, \{G. G.\} and Moffat, \{B. A.\} and Nally, \{C. W.\} and Neubauer, \{M. S.\} and Nickel, \{B. G.\} and Noble, \{A. J.\} and Norman, \{E. B.\} and Oblath, \{N. S.\} and Okada, \{C. E.\} and Ollerhead, \{R. W.\} and Orrell, \{J. L.\} and Oser, \{S. M.\} and C. Ouellet and Peeters, \{S. J.M.\} and Poon, \{A. W.P.\} and K. Rielage and Robertson, \{B. C.\} and Robertson, \{R. G.H.\} and E. Rollin and Rosendahl, \{S. S.E.\} and Rusu, \{V. L.\} and Schwendener, \{M. H.\} and O. Simard and Simpson, \{J. J.\} and Sims, \{C. J.\} and D. Sinclair and P. Skensved and Smith, \{M. W.E.\} and N. Starinsky and Stokstad, \{R. G.\} and Stonehill, \{L. C.\} and R. Tafirout and Y. Takeuchi and G. Te{\v s}i{\'c} and M. Thomson and T. Tsui and \{Van Berg\}, R. and \{Van de Water\}, \{R. G.\} and Virtue, \{C. J.\} and Wall, \{B. L.\} and D. Waller and Waltham, \{C. E.\} and Tseung, \{H. Wan Chan\} and Wark, \{D. L.\} and N. West and Wilhelmy, \{J. B.\} and Wilkerson, \{J. F.\} and Wilson, \{J. R.\} and P. Wittich and Wouters, \{J. M.\} and M. Yeh and K. Zuber",

note = "Funding Information: This research was supported by the Natural Sciences and Engineering Research Council, Canada; Industry Canada; National Research Council, Canada; Northern ?> ?>Ontario Heritage Fund Corporation, Inco, Canada; ?> ?>Atomic Energy of Canada, Ltd.; Ontario Power ?> ?>Generation; the U.S. Department. of Energy; and ?> ?>Particle Physics and Astronomy Research Council, ?> ?>United Kingdom. We thank the SNO technical staff for ?> ?>their strong contributions.",

year = "2004",

doi = "10.1103/PhysRevD.70.093014",

language = "English",

volume = "70",

number = "9",

}

Aharmim, B, Ahmed, SN, Beier, EW, Bellerive, A, Biller, SD, Boger, J, Boulay, MG, Bowles, TJ, Brice, SJ, Bullard, TV, Chan, YD, Chen, M, Chen, X, Cleveland, BT, Cox, GA, Dai, X, Dalnoki-Veress, F, Doe, PJ, Dosanjh, RS, Doucas, G, Dragowsky, MR, Duba, CA, Duncan, FA, Dunford, M, Dunmore, JA, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Formaggio, JA, Fowler, MM, Frame, K, Frati, W, Fulsom, BG, Gagnon, N, Graham, K, Grant, DR, Hahn, RL, Hallin, AL, Hallman, ED, Hamer, AS, Handler, WB, Hargrove, CK, Harvey, PJ, Hazama, R, Heeger, KM, Heintzelman, WJ, Heise, J, Helmer, RL, Hemingway, RJ, Hime, A, Howe, MA, Jagam, P, Jelley, NA, Klein, JR, Kormos, LL, Kos, MS, Krüger, A, Krauss, CB, Krumins, AV, Kutter, T, Kyba, CCM, Labranche, H, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Luoma, S, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Marino, AD, McCauley, N, McDonald, AB, McGee, S, McGregor, G, Mifflin, C, Miknaitis, KKS, Miller, GG, Moffat, BA, Nally, CW, Neubauer, MS, Nickel, BG, Noble, AJ, Norman, EB, Oblath, NS, Okada, CE, Ollerhead, RW, Orrell, JL, Oser, SM, Ouellet, C, Peeters, SJM, Poon, AWP, Rielage, K, Robertson, BC, Robertson, RGH, Rollin, E, Rosendahl, SSE, Rusu, VL, Schwendener, MH, Simard, O, Simpson, JJ, Sims, CJ, Sinclair, D, Skensved, P, Smith, MWE, Starinsky, N, Stokstad, RG, Stonehill, LC, Tafirout, R, Takeuchi, Y, Tešić, G, Thomson, M, Tsui, T, Van Berg, R, Van de Water, RG, Virtue, CJ, Wall, BL, Waller, D, Waltham, CE, Tseung, HWC, Wark, DL, West, N, Wilhelmy, JB, Wilkerson, JF, Wilson, JR, Wittich, P, Wouters, JM, Yeh, M & Zuber, K 2004, 'Electron antineutrino search at the Sudbury Neutrino Observatory', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 70, n.º 9. https://doi.org/10.1103/PhysRevD.70.093014

TY - JOUR

T1 - Electron antineutrino search at the Sudbury Neutrino Observatory

AU - Aharmim, B.

AU - Ahmed, S. N.

AU - Beier, E. W.

AU - Bellerive, A.

AU - Biller, S. D.

AU - Boger, J.

AU - Boulay, M. G.

AU - Bowles, T. J.

AU - Brice, S. J.

AU - Bullard, T. V.

AU - Chan, Y. D.

AU - Chen, M.

AU - Chen, X.

AU - Cleveland, B. T.

AU - Cox, G. A.

AU - Dai, X.

AU - Dalnoki-Veress, F.

AU - Doe, P. J.

AU - Dosanjh, R. S.

AU - Doucas, G.

AU - Dragowsky, M. R.

AU - Duba, C. A.

AU - Duncan, F. A.

AU - Dunford, M.

AU - Dunmore, J. A.

AU - Earle, E. D.

AU - Elliott, S. R.

AU - Evans, H. C.

AU - Ewan, G. T.

AU - Farine, J.

AU - Fergani, H.

AU - Fleurot, F.

AU - Formaggio, J. A.

AU - Fowler, M. M.

AU - Frame, K.

AU - Frati, W.

AU - Fulsom, B. G.

AU - Gagnon, N.

AU - Graham, K.

AU - Grant, D. R.

AU - Hahn, R. L.

AU - Hallin, A. L.

AU - Hallman, E. D.

AU - Hamer, A. S.

AU - Handler, W. B.

AU - Hargrove, C. K.

AU - Harvey, P. J.

AU - Hazama, R.

AU - Heeger, K. M.

AU - Heintzelman, W. J.

AU - Heise, J.

AU - Helmer, R. L.

AU - Hemingway, R. J.

AU - Hime, A.

AU - Howe, M. A.

AU - Jagam, P.

AU - Jelley, N. A.

AU - Klein, J. R.

AU - Kormos, L. L.

AU - Kos, M. S.

AU - Krüger, A.

AU - Krauss, C. B.

AU - Krumins, A. V.

AU - Kutter, T.

AU - Kyba, C. C.M.

AU - Labranche, H.

AU - Lange, R.

AU - Law, J.

AU - Lawson, I. T.

AU - Lesko, K. T.

AU - Leslie, J. R.

AU - Levine, I.

AU - Luoma, S.

AU - MacLellan, R.

AU - Majerus, S.

AU - Mak, H. B.

AU - Maneira, J.

AU - Marino, A. D.

AU - McCauley, N.

AU - McDonald, A. B.

AU - McGee, S.

AU - McGregor, G.

AU - Mifflin, C.

AU - Miknaitis, K. K.S.

AU - Miller, G. G.

AU - Moffat, B. A.

AU - Nally, C. W.

AU - Neubauer, M. S.

AU - Nickel, B. G.

AU - Noble, A. J.

AU - Norman, E. B.

AU - Oblath, N. S.

AU - Okada, C. E.

AU - Ollerhead, R. W.

AU - Orrell, J. L.

AU - Oser, S. M.

AU - Ouellet, C.

AU - Peeters, S. J.M.

AU - Poon, A. W.P.

AU - Rielage, K.

AU - Robertson, B. C.

AU - Robertson, R. G.H.

AU - Rollin, E.

AU - Rosendahl, S. S.E.

AU - Rusu, V. L.

AU - Schwendener, M. H.

AU - Simard, O.

AU - Simpson, J. J.

AU - Sims, C. J.

AU - Sinclair, D.

AU - Skensved, P.

AU - Smith, M. W.E.

AU - Starinsky, N.

AU - Stokstad, R. G.

AU - Stonehill, L. C.

AU - Tafirout, R.

AU - Takeuchi, Y.

AU - Tešić, G.

AU - Thomson, M.

AU - Tsui, T.

AU - Van Berg, R.

AU - Van de Water, R. G.

AU - Virtue, C. J.

AU - Wall, B. L.

AU - Waller, D.

AU - Waltham, C. E.

AU - Tseung, H. Wan Chan

AU - Wark, D. L.

AU - West, N.

AU - Wilhelmy, J. B.

AU - Wilkerson, J. F.

AU - Wilson, J. R.

AU - Wittich, P.

AU - Wouters, J. M.

AU - Yeh, M.

AU - Zuber, K.

N1 - Funding Information: This research was supported by the Natural Sciences and Engineering Research Council, Canada; Industry Canada; National Research Council, Canada; Northern ?> ?>Ontario Heritage Fund Corporation, Inco, Canada; ?> ?>Atomic Energy of Canada, Ltd.; Ontario Power ?> ?>Generation; the U.S. Department. of Energy; and ?> ?>Particle Physics and Astronomy Research Council, ?> ?>United Kingdom. We thank the SNO technical staff for ?> ?>their strong contributions.

PY - 2004

Y1 - 2004

N2 - Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.

AB - Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.

UR - https://www.scopus.com/pages/publications/42749105454

UR - https://www.scopus.com/pages/publications/42749105454#tab=citedBy

U2 - 10.1103/PhysRevD.70.093014

DO - 10.1103/PhysRevD.70.093014

M3 - Article

AN - SCOPUS:42749105454

SN - 1550-7998

VL - 70

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

IS - 9

ER -

Electron antineutrino search at the Sudbury Neutrino Observatory

Resumen

Nota bibliográfica

Financiación

ASJC Scopus subject areas

Acceder al documento

Otros archivos y enlaces

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