(A) Neutrino fluxes and event ratios

Day-Night Asymmetry (${}^{8}\mathrm {B}$)

INSPIRE   PDGID:
S067SDN
$\mathit A$ = ($\phi _{{\mathrm {night}}}$ $−$ $\phi _{{\mathrm {day}}}$) $/$ $\phi _{{\mathrm {average}}}$

VALUE DOCUMENT ID TECN  COMMENT
$0.033$ $\pm0.010$ $\pm0.005$ 1
ABE
2016C
 SKAM SK combined; Based on ${{\mathit \phi}_{{ES}}}$
• • We do not use the following data for averages, fits, limits, etc. • •
$0.036$ $\pm0.016$ $\pm0.006$ 2
ABE
2016C
 SKAM SK-IV; Based on ${{\mathit \phi}_{{ES}}}$
$0.032$ $\pm0.011$ $\pm0.005$ 3
RENSHAW
2014
SKAM Based on ${{\mathit \phi}_{{ES}}}$
$0.063$ $\pm0.042$ $\pm0.037$ 4
CRAVENS
2008
SKAM Based on ${{\mathit \phi}_{{ES}}}$
$0.021$ $\pm0.020$ ${}^{+0.012}_{-0.013}$ 5
HOSAKA
2006
SKAM Based on ${{\mathit \phi}_{{ES}}}$
$0.017$ $\pm0.016$ ${}^{+0.012}_{-0.013}$ 6
HOSAKA
2006
SKAM Fitted in the LMA region
$-0.056$ $\pm0.074$ $\pm0.053$ 7
AHARMIM
2005A
 SNO From salty SNO ${{\mathit \phi}_{{CC}}}$
$-0.037$ $\pm0.063$ $\pm0.032$ 7
AHARMIM
2005A
 SNO From salty SNO ${{\mathit \phi}_{{CC}}}$; const. of no ${{\mathit \phi}_{{NC}}}$ asymmetry
$0.14$ $\pm0.063$ ${}^{+0.015}_{-0.014}$ 8
AHMAD
2002B
 SNO Derived from SNO ${{\mathit \phi}}_{\mathit CC}$
$0.07$ $\pm0.049$ ${}^{+0.013}_{-0.012}$ 9
AHMAD
2002B
 SNO Const. of no ${{\mathit \phi}}_{\mathit NC}$ asymmetry
1  ABE 2016C reports the combined day-night flux asymmetry results of the four phases of the Super-Kamiokande measurements. Amplitude fit method is used. See footnote to RENSHAW 2014 .
2  ABE 2016C reports the Super-Kamiokande-IV results for 1664 live days from September 2008 to February 2014. The analysis threshold for day-night flux asymmetry is recoil electron energy of 4.49 MeV (total electron energy of 5.0 MeV). Amplitude fit method is used. See footnote to RENSHAW 2014 .
3  RENSHAW 2014 obtains this result by using the "amplitude fit" introduced in SMY 2004 . The data from the Super-Kamiokande(SK)-I, -II, -III, and 1306 live days of the SK-IV measurements are used. The analysis threshold is recoil-electron kinetic energy of 4.5 MeV for SK-III, and SK-IV except for 250 live days in SK-III (6.0 MeV). The analysis threshold for SK-I and SK-II is the same as in the previous reports. (Note that in the previous SK solar-neutrino results, the analysis threshold is quoted as recoil-electron total energy.) This day-night asymmetry result is consistent with neutrino oscillations for $4 \times 10^{-5}$ eV${}^{2}$ $<$ $\Delta $m${}^{2}_{21}$ $<$ $7 \times 10^{-5}$ eV${}^{2}$ and large mixing values of $\theta _{12}$ at the 68$\%$ CL.
4  CRAVENS 2008 reports the Super-Kamiokande-II results for 791 live days from December 2002 to October 2005. The photocathode coverage of the detector is 19$\%$ (reduced from 40$\%$ of that of Super-Kamiokande-I due to an accident in 2001). The analysis threshold for the day and night fluxes is 7.5 MeV except for the first 159 live days (8.0 MeV).
5  HOSAKA 2006 reports the final results for 1496 live days with Super-Kamiokande-I between May 31, 1996 and July 15, 2001, and replace FUKUDA 2002 results. The analysis threshold is 5 MeV except for the first 280 live days (6.5 MeV).
6  This result with reduced statistical uncertainty is obtained by assuming two-neutrino oscillations within the LMA (large mixing angle) region and by fitting the time variation of the solar neutrino flux measured via ${{\mathit \nu}_{{e}}}$ elastic scattering to the variations expected from neutrino oscillations. For details, see SMY 2004 . There is an additional small systematic error of $\pm0.0004$ coming from uncertainty of oscillation parameters.
7  AHARMIM 2005A measurements were made with dissolved NaCl (0.195$\%$ by weight) in heavy water over the period between July 26, 2001 and August 28, 2003, with 176.5 days of the live time recorded during the day and 214.9 days during the night. This result is obtained with the spectral distribution of the CC events not constrained to the ${}^{8}\mathrm {B}$ shape.
8  AHMAD 2002B results are based on the charged-current interactions recorded between November 2, 1999 and May 28, 2001, with the day and night live times of 128.5 and 177.9 days, respectively. The complete description of the SNO Phase I data set is given in AHARMIM 2007 .
9  AHMAD 2002B results are derived from the charged-current interactions, neutral-current interactions, and ${{\mathit \nu}}{{\mathit e}}$ elastic scattering, with the total flux of active neutrinos constrained to have no asymmetry. The data were recorded between November 2, 1999 and May 28, 2001, with the day and night live times of 128.5 and 177.9 days, respectively. The complete description of the SNO Phase I data set is given in AHARMIM 2007 .
References:
ABE 2016C
PR D94 052010 Solar Neutrino Measurements in Super-Kamiokande-IV
RENSHAW 2014
PRL 112 091805 First Indication of Terrestrial Matter Effects on Solar Neutrino Oscillation
CRAVENS 2008
PR D78 032002 Solar Neutrino Measurements in Super-Kamiokande-II
HOSAKA 2006
PR D73 112001 Solar Neutrino Measurements in Super-Kamiokande-I
AHARMIM 2005A
PR C72 055502 Search for Periodicities in the ${}^{8}\mathrm {B}$ Solar Neutrino Flux Measured by the Sudbury Neutrino Observatory
AHMAD 2002B
PRL 89 011302 Measurement of Day and Night Neutrino Energy Spectra at SNO and Constraints on Neutrino Mixing Parameters