(A) Neutrino fluxes and event ratios

${{\mathit \nu}_{{{e}}}}$ Capture Rates from Radiochemical Experiments

INSPIRE   JSON  (beta) PDGID:
S067SNU
1 SNU (Solar Neutrino Unit) = $10^{-36}$ captures per atom per second.

VALUE (SNU) DOCUMENT ID TECN  COMMENT
• • We do not use the following data for averages, fits, limits, etc. • •
$73.4$ ${}^{+6.1}_{-6.0}$ ${}^{+3.7}_{-4.1}$ 1
KAETHER
2010
GALX reanalysis
$67.6$ $\pm4.0$ $\pm3.2$ 2
KAETHER
2010
GNO+GALX reanalysis combined
$65.4$ ${}^{+3.1}_{-3.0}$ ${}^{+2.6}_{-2.8}$ 3
ABDURASHITOV
2009
SAGE ${}^{71}\mathrm {Ga}$ $\rightarrow$ ${}^{71}\mathrm {Ge}$
$62.9$ ${}^{+5.5}_{-5.3}$ $\pm2.5$ 4
ALTMANN
2005
GNO ${}^{71}\mathrm {Ga}$ $\rightarrow$ ${}^{71}\mathrm {Ge}$
$69.3$ $\pm4.1$ $\pm3.6$ 5
ALTMANN
2005
GNO GNO + GALX combined
$77.5$ $\pm6.2$ ${}^{+4.3}_{-4.7}$ 6
HAMPEL
1999
GALX ${}^{71}\mathrm {Ga}$ $\rightarrow$ ${}^{71}\mathrm {Ge}$
$2.56$ $\pm0.16$ $\pm0.16$ 7
CLEVELAND
1998
HOME ${}^{37}\mathrm {Cl}$ $\rightarrow$ ${}^{37}\mathrm {Ar}$
1  KAETHER 2010 reports the reanalysis results of a complete GALLEX data (GALLEX I+II+III+IV, reported in HAMPEL 1999) based on the event selection with a new pulse shape analysis, which provides a better background reduction than the rise time analysis adopted in HAMPEL 1999.
2  Combined result of GALLEX I+II+III+IV reanalysis and GNO I+II+III (ALTMANN 2005).
3  ABDURASHITOV 2009 reports a combined analysis of 168 extractions of the SAGE solar neutrino experiment during the period January 1990 through December 2007, and updates the ABDURASHITOV 2002 result. The data are consistent with the assumption that the solar neutrino production rate is constant in time. Note that a $\sim{}15\%$ systematic uncertainty in the overall normalization may be added to the ABDURASHITOV 2009 result, because calibration experiments for gallium solar neutrino measurements using intense ${}^{51}\mathrm {Cr}$ (twice by GALLEX and once by SAGE) and ${}^{37}\mathrm {Ar}$ (by SAGE) result in an average ratio of $0.87$ $\pm0.05$ of the observed to calculated rates.
4  ALTMANN 2005 reports the complete result from the GNO solar neutrino experiment (GNO I+II+III), which is the successor project of GALLEX. Experimental technique of GNO is essentially the same as that of GALLEX. The run data cover the period 20 May 1998 through 9 April 2003.
5  Combined result of GALLEX I+II+III+IV (HAMPEL 1999) and GNO I+II+III.
6  HAMPEL 1999 report the combined result for GALLEX I+II+III+IV (65 runs in total), which update the HAMPEL 1996 result. The GALLEX$~$IV result (12 runs) is $118.4$ $\pm17.8$ $\pm6.6$ SNU. (HAMPEL 1999 discuss the consistency of partial results with the mean.) The GALLEX experimental program has been completed with these runs. The total run data cover the period 14 May 1991 through 23 January 1997. A total of 300 ${}^{71}\mathrm {Ge}$ events were observed. Note that a $\sim{}15\%$ systematic uncertainty in the overall normalization may be added to the HAMPEL 1999 result, because calibration experiments for gallium solar neutrino measurements using intense ${}^{51}\mathrm {Cr}$ (twice by GALLEX and once by SAGE) and ${}^{37}\mathrm {Ar}$ (by SAGE) result in an average ratio of $0.87$ $\pm0.05$ of the observed to calculated rates.
7  CLEVELAND 1998 is a detailed report of the ${}^{37}\mathrm {Cl}$ experiment at the Homestake Mine. The average solar neutrino-induced ${}^{37}\mathrm {Ar}$ production rate from 108 runs between 1970 and 1994 updates the DAVIS 1989 result.
References