${{\boldsymbol \nu}}$ MAGNETIC MOMENT INSPIRE search

The coupling of neutrinos to an electromagnetic field is a characterized by a 3${\times }$3 matrix $\lambda $ of the magnetic ($\mu $) and electric ($\mathit d$) dipole moments ($\lambda $ = $\mu - \mathit id$). For Majorana neutrinos the matrix $\lambda $ is antisymmetric and only transition moments are allowed, while for Dirac neutrinos $\lambda $ is a general 3${\times }$3 matrix. In the standard electroweak theory extended to include neutrino masses (see FUJIKAWA 1980 ) ${{\mathit \mu}_{{\nu}}}$ = 3${{\mathit e}}{{\mathit G}_{{F}}}{\mathit m}_{{{\mathit \nu}}}/(8{{\mathit \pi}}{}^{2}\sqrt {2 }$) = 3.2${\times }10^{-19}({\mathit m}_{{{\mathit \nu}}}$/eV)${{\mathit \mu}_{{B}}}$, i.e. it is unobservably small given the known small neutrino masses. In more general models there is no longer a proportionality between neutrino mass and its magnetic moment, even though only massive neutrinos have nonvanishing magnetic moments without fine tuning.

Laboratory bounds on $\lambda $ are obtained via elastic ${{\mathit \nu}}-{{\mathit e}}$ scattering, where the scattered neutrino is not observed. The combinations of matrix elements of $\lambda $ that are constrained by various experiments depend on the initial neutrino flavor and on its propagation between source and detector (e.g., solar ${{\mathit \nu}_{{e}}}$ and reactor ${{\overline{\mathit \nu}}_{{e}}}$ do not constrain the same combinations). The listings below therefore identify the initial neutrino flavor.

Other limits, e.g. from various stellar cooling processes, apply to all neutrino flavors. Analogous flavor independent, but weaker, limits are obtained from the analysis of ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ collider experiments.

VALUE ($ 10^{-10} $ $\mu _{\mathit B}$) CL% DOCUMENT ID TECN  COMMENT
$<0.28$ 90 1
AGOSTINI
2017A
BORX Solar ${{\mathit \nu}}$ spectrum
$\bf{<0.29}$ 90 2
BEDA
2013
CNTR Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$\bf{<6.8}$ 90 3
AUERBACH
2001
LSND ${{\mathit \nu}_{{e}}}{{\mathit e}}$ , ${{\mathit \nu}_{{\mu}}}{{\mathit e}}$ scattering
$\bf{<3900}$ 90 4
SCHWIENHORST
2001
DONU ${{\mathit \nu}_{{\tau}}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}_{{\tau}}}{{\mathit e}^{-}}$
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<0.022$ 90 5
ARCEO-DIAZ
2015
ASTR Red giants
$<0.1$ 95 6
CORSICO
2014
ASTR
$<0.05$ 95 7
MILLER-BERTOL..
2014B
ASTR
$<0.045$ 95 8
VIAUX
2013A
ASTR Globular cluster M5
$<0.32$ 90 9
BEDA
2010
CNTR Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<2.2$ 90 10
DENIZ
2010
TEXO Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$\text{<0.011 - 0.027}$ 11
KUZNETSOV
2009
ASTR ${{\mathit \nu}_{{L}}}$ $\rightarrow$ ${{\mathit \nu}_{{R}}}$ in SN1987A
$<0.54$ 90 12
ARPESELLA
2008A
BORX Solar ${{\mathit \nu}}$ spectrum
$<0.58$ 90 13
BEDA
2007
CNTR Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<0.74$ 90 14
WONG
2007
CNTR Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<0.9$ 90 15
DARAKTCHIEVA
2005
Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<130$ 90 16
XIN
2005
CNTR Reactor ${{\mathit \nu}_{{e}}}$
$<37$ 95 17
GRIFOLS
2004
FIT Solar ${}^{8}\mathrm {B}{{\mathit \nu}}$ (SNO NC)
$<3.6$ 90 18
LIU
2004
SKAM Solar ${{\mathit \nu}}$ spectrum
$<1.1$ 90 19
LIU
2004
SKAM Solar ${{\mathit \nu}}$ spectrum (LMA region)
$<5.5$ 90 20
BACK
2003B
CNTR Solar ${{\mathit p}}{{\mathit p}}$ and Be ${{\mathit \nu}}$
$<1.0$ 90 21
DARAKTCHIEVA
2003
Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<1.3$ 90 22
LI
2003B
CNTR Reactor ${{\overline{\mathit \nu}}_{{e}}}$
$<2$ 90 23
GRIMUS
2002
FIT solar + reactor (Majorana ${{\mathit \nu}}$)
$<80000$ 90 24
TANIMOTO
2000
RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$
$\text{<0.01 - 0.04}$ 25
AYALA
1999
ASTR ${{\mathit \nu}_{{L}}}$ $\rightarrow$ ${{\mathit \nu}_{{R}}}$ in SN$~$1987A
$<1.5$ 90 26
BEACOM
1999
SKAM Solar ${{\mathit \nu}}$ spectrum
$<0.03$ 27
RAFFELT
1999
ASTR Red giant luminosity
$<4$ 28
RAFFELT
1999
ASTR Solar cooling
$<44000$ 90
ABREU
1997J
DLPH ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ at LEP
$<33000$ 90 29
ACCIARRI
1997Q
L3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ at LEP
$<0.62$ 30
ELMFORS
1997
COSM Depolarization in early universe plasma
$<27000$ 95 31
ESCRIBANO
1997
RVUE $\Gamma\mathrm {( {{\mathit Z}} \rightarrow {{\mathit \nu}} {{\mathit \nu}} )}$ at LEP
$<30$ 90
VILAIN
1995B
CHM2 ${{\mathit \nu}_{{\mu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\mathit \nu}_{{\mu}}}{{\mathit e}}$
$<55000$ 90
GOULD
1994
RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ at LEP
$<1.9$ 95 32
DERBIN
1993
CNTR Reactor ${{\overline{\mathit \nu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\overline{\mathit \nu}}}{{\mathit e}}$
$<5400$ 90 33
COOPER-SARKAR
1992
BEBC ${{\mathit \nu}_{{\tau}}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}_{{\tau}}}{{\mathit e}^{-}}$
$<2.4$ 90 34
VIDYAKIN
1992
CNTR Reactor ${{\overline{\mathit \nu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\overline{\mathit \nu}}}{{\mathit e}}$
$<56000$ 90
DESHPANDE
1991
RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$
$<100$ 95 35
DORENBOSCH
1991
CHRM ${{\mathit \nu}_{{\mu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\mathit \nu}_{{\mu}}}{{\mathit e}}$
$<8.5$ 90
AHRENS
1990
CNTR ${{\mathit \nu}_{{\mu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\mathit \nu}_{{\mu}}}{{\mathit e}}$
$<10.8$ 90 36
KRAKAUER
1990
CNTR LAMPF ${{\mathit \nu}}$ ${{\mathit e}}$ $\rightarrow$ ${{\mathit \nu}}{{\mathit e}}$
$<7.4$ 90 36
KRAKAUER
1990
CNTR LAMPF (${{\mathit \nu}_{{\mu}}}$, ${{\overline{\mathit \nu}}_{{\mu}}}$ ) ${{\mathit e}}$ elast.
$<0.02$ 37
RAFFELT
1990
ASTR Red giant luminosity
$<0.1$ 38
RAFFELT
1989B
ASTR Cooling helium stars
39
FUKUGITA
1988
COSM Primordial magn. fields
$<40000$ 90 40
GROTCH
1988
RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$
$<=.3$ 38
RAFFELT
1988B
ASTR ${}^{}\mathrm {He}$ burning stars
$<0.11$ 38
FUKUGITA
1987
ASTR Cooling helium stars
$<0.0006$ 41
NUSSINOV
1987
ASTR Cosmic EM backgrounds
$\text{<0.1 - 0.2}$
MORGAN
1981
COSM ${}^{4}\mathrm {He}$ abundance
$<0.85$
BEG
1978
ASTR Stellar plasmons
$<0.6$ 42
SUTHERLAND
1976
ASTR Red giants + degenerate dwarfs
$<81$ 43
KIM
1974
RVUE ${{\overline{\mathit \nu}}_{{\mu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\overline{\mathit \nu}}_{{\mu}}}{{\mathit e}}$
$<1$
BERNSTEIN
1963
ASTR Solar cooling
$<14$
COWAN
1957
CNTR Reactor ${{\overline{\mathit \nu}}}$
1  AGOSTINI 2017A obtained this limit using the shape of the recoil electron energy spectrum from the Borexino Phase-II 1291.5 live days of solar neutrino data and the constraints on the sum of the solar neutrino fluxes from the radiochemical gallium experiments SAGE, Gallex, and GNO. Without radiochemical constraints, the 90$\%$ C.L. limit of $<4.0 \times 10^{-11}\mu _{B}$ is obtained.
2  BEDA 2013 report ${{\overline{\mathit \nu}}_{{e}}}{{\mathit e}^{-}}$ scattering results, using the Kalinin Nuclear Power Plant and a shielded ${}^{}\mathrm {Ge}$ detector. The recoil electron spectrum is analyzed between 2.5 and 55 keV. Supersedes BEDA 2007 . Supersedes BEDA 2010 . This is the most stringent limit on the magnetic moment of reactor ${{\overline{\mathit \nu}}_{{e}}}$.
3  AUERBACH 2001 limit is based on the LSND ${{\mathit \nu}_{{e}}}$ and ${{\mathit \nu}_{{\mu}}}$ electron scattering measurements. The limit is slightly more stringent than KRAKAUER 1990 .
4  SCHWIENHORST 2001 quote an experimental sensitivity of $4.9 \times 10^{-7}$.
5  ARCEO-DIAZ 2015 constrains the neutrino magnetic moment from observation of the tip of the red giant branch in the globular cluster $\omega $-Centauri.
6  CORSICO 2014 constrains the neutrino magnetic moment from observations of white drarf pulsations.
7  MILLER-BERTOLAMI 2014B constrains the neutrino magnetic moment from observations of the white dwarf luminosity function of the Galactic disk.
8  VIAUX 2013A constrains the neutrino magnetic moment from observations of the globular cluster M5.
9  BEDA 2010 report ${{\overline{\mathit \nu}}_{{e}}}{{\mathit e}^{-}}$ scattering results, using the Kalinin Nuclear Power Plant and a shielded ${}^{}\mathrm {Ge}$ detector. The recoil electron spectrum is analyzed between 2.9 and 45 keV. Supersedes BEDA 2007 . Superseded by BEDA 2013 .
10  DENIZ 2010 observe reactor ${{\overline{\mathit \nu}}_{{e}}}{{\mathit e}}$ scattering with recoil kinetic energies $3 - 8$ MeV using CsI(Tl) detectors. The observed rate and spectral shape are consistent with the Standard Model prediction, leading to the reported constraint on ${{\overline{\mathit \nu}}_{{e}}}$ magnetic moment.
11  KUZNETSOV 2009 obtain a limit on the flavor averaged magnetic moment of Dirac neutrinos from the time averaged neutrino signal of SN1987A. Improves and supersedes the analysis of BARBIERI 1988 and AYALA 1999 .
12  ARPESELLA 2008A obtained this limit using the shape of the recoil electron energy spectrum from the Borexino 192 live days of solar neutrino data.
13  BEDA 2007 performed search for electromagnetic ${{\overline{\mathit \nu}}_{{e}}}-{{\mathit e}}$ scattering at Kalininskaya nuclear reactor. A ${}^{}\mathrm {Ge}$ detector with active and passive shield was used and the electron recoil spectrum between 3.0 and 61.3 keV analyzed. Superseded by BEDA 2010 .
14  WONG 2007 performed search for non-standard ${{\overline{\mathit \nu}}_{{e}}}-{{\mathit e}}$ scattering at the Kuo-Sheng nuclear reactor. Ge detector equipped with active anti-Compton shield is used. Most stringent laboratory limit on magnetic moment of reactor ${{\overline{\mathit \nu}}_{{e}}}$. Supersedes LI 2003B.
15  DARAKTCHIEVA 2005 present the final analysis of the search for non-standard ${{\overline{\mathit \nu}}_{{e}}}-{{\mathit e}}$ scattering component at Bugey nuclear reactor. Full kinematical event reconstruction of both the kinetic energy above 700 keV and scattering angle of the recoil electron, by use of TPC. Most stringent laboratory limit on magnetic moment. Supersedes DARAKTCHIEVA 2003 .
16  XIN 2005 evaluated the ${{\mathit \nu}_{{e}}}$ flux at the Kuo-Sheng nuclear reactor and searched for non-standard ${{\mathit \nu}_{{e}}}-{{\mathit e}}$ scattering. Ge detector equipped with active anti-Compton shield was used. This laboratory limit on magnetic moment is considerably less stringent than the limits for reactor ${{\overline{\mathit \nu}}_{{e}}}$, but is specific to ${{\mathit \nu}_{{e}}}$.
17  GRIFOLS 2004 obtained this bound using the SNO data of the solar ${}^{8}\mathrm {B}$ neutrino flux measured with deuteron breakup. This bound applies to ${{\mathit \mu}}_{{\mathrm {eff}}}$ = (${{\mathit \mu}}{}^{2}_{21}$ + ${{\mathit \mu}}{}^{2}_{22}$ + ${{\mathit \mu}}{}^{2}_{23}){}^{1/2}$.
18  LIU 2004 obtained this limit using the shape of the recoil electron energy spectrum from the Super-Kamiokande-I 1496 days of solar neutrino data. Neutrinos are assumed to have only diagonal magnetic moments, ${{\mathit \mu}_{{\nu1}}}$ = ${{\mathit \mu}_{{\nu2}}}$. This limit corresponds to the oscillation parameters in the vacuum oscillation region.
19  LIU 2004 obtained this limit using the shape of the recoil electron energy spectrum from the Super-Kamiokande-I 1496 live-day solar neutrino data, by limiting the oscillation parameter region in the LMA region allowed by solar neutrino experiments plus KamLAND. ${{\mathit \mu}_{{\nu1}}}$ = ${{\mathit \mu}_{{\nu2}}}$ is assumed. In the LMA region, the same limit would be obtained even if neutrinos have off-diagonal magnetic moments.
20  BACK 2003B obtained this bound from the results of background measurements with Counting Test Facility (the prototype of the Borexino detector). Standard Solar Model flux was assumed. This ${{\mathit \mu}_{{\nu}}}$ can be different from the reactor ${{\mathit \mu}_{{\nu}}}$ in certain oscillation scenarios (see BEACOM 1999 ).
21  DARAKTCHIEVA 2003 searched for non-standard ${{\overline{\mathit \nu}}_{{e}}}$-e scattering component at Bugey nuclear reactor. Full kinematical event reconstruction by use of TPC. Superseded by DARAKTCHIEVA 2005 .
22  LI 2003B used Ge detector in active shield near nuclear reactor to test for nonstandard ${{\overline{\mathit \nu}}_{{e}}}-{{\mathit e}}$ scattering.
23  GRIMUS 2002 obtain stringent bounds on all Majorana neutrino transition moments from a simultaneous fit of LMA-MSW oscillation parameters and transition moments to global solar neutrino data + reactor data. Using only solar neutrino data, a 90$\%$ CL bound of $6.3 \times 10^{-10}\mu _{{{\mathit B}}}$ is obtained.
24  TANIMOTO 2000 combined ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ data from VENUS, TOPAZ, and AMY.
25  AYALA 1999 improves the limit of BARBIERI 1988 .
26  BEACOM 1999 obtain the limit using the shape, but not the absolute magnitude which is affected by oscillations, of the solar neutrino spectrum obtained by Superkamiokande (825 days). This $\mu _{{{\mathit \nu}}}$ can be different from the reactor $\mu _{{{\mathit \nu}}}$ in certain oscillation scenarios.
27  RAFFELT 1999 is an update of RAFFELT 1990 . This limit applies to all neutrino flavors which are light enough ($<5~$keV) to be emitted from globular-cluster red giants. This limit pertains equally to electric dipole moments and magnetic transition moments, and it applies to both Dirac and Majorana neutrinos.
28  RAFFELT 1999 is essentially an update of BERNSTEIN 1963 , but is derived from the helioseismological limit on a new energy-loss channel of the Sun. This limit applies to all neutrino flavors which are light enough ($<1~$keV) to be emitted from the Sun. This limit pertains equally to electric dipole and magnetic transition moments, and it applies to both Dirac and Majorana neutrinos.
29  ACCIARRI 1997Q result applies to both direct and transition magnetic moments and for $\mathit q{}^{2}$=0.
30  ELMFORS 1997 calculate the rate of depolarization in a plasma for neutrinos with a magnetic moment and use the constraints from a big-bang nucleosynthesis on additional degrees of freedom.
31  Applies to absolute value of magnetic moment.
32  DERBIN 1993 determine the cross section for $0.6 - 2.0$ MeV electron energy as ($1.28$ $\pm0.63){\times }\sigma _{{\mathrm {weak}}}$. However, the (reactor on -- reactor off)/(reactor off) is only $\sim{}$1/100.
33  COOPER-SARKAR 1992 assume $\mathit f_{{{\mathit D}_{{s}}}}/\mathit f_{{{\mathit \pi}}}$ = 2 and ${{\mathit D}_{{s}}}$, ${{\overline{\mathit D}}_{{s}}}$ production cross section = $2.6$ $\mu $b to calculate ${{\mathit \nu}}$ flux.
34  VIDYAKIN 1992 limit is from a ${{\mathit e}}{{\overline{\mathit \nu}}_{{e}}}$ elastic scattering experiment. No experimental details are given except for the cross section from which this limit is derived. Signal/noise was 1/10. The limit uses sin$^2\theta _{\mathit W}$ = $0.23$ as input.
35  DORENBOSCH 1991 corrects an incorrect statement in DORENBOSCH 1989 that the ${{\mathit \nu}}$ magnetic moment is $<~1 \times 10^{-9}$ at the 95$\%$CL. DORENBOSCH 1989 measures both ${{\mathit \nu}_{{\mu}}}{{\mathit e}}$ and ${{\overline{\mathit \nu}}}{{\mathit e}}$ elastic scattering and assume $\mu\mathrm {({{\mathit \nu}})}$ = $\mu\mathrm {({{\overline{\mathit \nu}}})}$.
36  KRAKAUER 1990 experiment fully reported in ALLEN 1993 .
37  RAFFELT 1990 limit applies for a diagonal magnetic moment of a Dirac neutrino, or for a transition magnetic moment of a Majorana neutrino. In the latter case, the same analysis gives $<1.4 \times 10^{-12}$. Limit at 95$\%$CL obtained from $\delta \mathit M_{\mathit c}$.
38  Significant dependence on details of stellar models.
39  FUKUGITA 1988 find magnetic dipole moments of any two neutrino species are bounded by $\mu $ $<$ $10^{-16}$ [$10^{-9}~\mathit G/{{\mathit B}}_{0}$] where ${{\mathit B}}_{0}$ is the present-day intergalactic field strength.
40  GROTCH 1988 combined data from MAC, ASP, CELLO, and Mark$~$J.
41  For ${\mathit m}_{{{\mathit \nu}}}$ = 8$-$200 eV. NUSSINOV 1987 examines transition magnetic moments for ${{\mathit \nu}_{{\mu}}}$ $\rightarrow$ ${{\mathit \nu}_{{e}}}$ and obtain $<$ $3 \times 10^{-15}$ for ${\mathit m}_{{{\mathit \nu}}}$ $>$ 16 eV and $<$ $6 \times 10^{-14}$ for ${\mathit m}_{{{\mathit \nu}}}$ $>$ 4 eV.
42  We obtain above limit from SUTHERLAND 1976 using their limit $\mathit f$ $<$ 1/3.
43  KIM 1974 is a theoretical analysis of ${{\overline{\mathit \nu}}_{{\mu}}}$ reaction data.
  References:
AGOSTINI 2017A
PR D96 091103 Limiting Neutrino Magnetic Moments with Borexino Phase-II Solar Neutrino Data
ARCEO-DIAZ 2015
ASP 70 1 Constraint on the Magnetic Dipole Moment of Neutrinos by the tip-RGB Luminosity in $\omega $-Centauri
CORSICO 2014
JCAP 1408 054 Constraining the Neutrino Magnetic Dipole Moment from White Dwarf Pulsations
MILLER-BERTOLAMI 2014B
AA 562 A123 Limits on the Neutrino Magnetic Dipole Moment from the Luminosity Function of hot White Dwarfs
BEDA 2013
PPNL 10 139 Gemma Experiment: The Results of Neutrino Magnetic Moment Search
VIAUX 2013A
PRL 111 231301 Neutrino and Axion Bounds from the Globular Cluster M5 (NGC 5904)
BEDA 2010
PPNL 7 406 Gemma Experiment: Three Years of the Search for the Neutrino Magnetic Moment
DENIZ 2010
PR D81 072001 Measurement of ${{\overline{\mathit \nu}}_{{e}}}{{\mathit e}}$ Scattering Cross Section with a CsI(Ti) Scintillating Crystal Array at the Kuo-Sheng Nuclear Power Reactor
KUZNETSOV 2009
IJMP A24 5977 Reexamination Oof a Bound on the Dirac Neutrino Magnetic Moment from the Supernova Neutrino Luminosity
ARPESELLA 2008A
PRL 101 091302 Direct Measurement of the ${}^{7}\mathrm {Be}$ Solar Neutrino Flux with 192 Days of Borexino Data
BEDA 2007
PAN 70 1873 First Result for Neutrino Magnetic Moment from Measurements with the GEMMA Spectrometer
WONG 2007
PR D75 012001 Search of Neutrino Magnetic Moments with a High-Purity Germanium Detector at the Kuo-Sheng Nuclear Power Station
DARAKTCHIEVA 2005
PL B615 153 Final Results on the Neutrino Magnetic Moment from the MUNU Experiment
XIN 2005
PR D72 012006 Production of Electron Neutrinos at Nuclear Power Reactors and the Prospects for Neutrino Physics
GRIFOLS 2004
PL B587 184 Neutrino Magnetic Moments and Photodisintegration of Deuterium
LIU 2004
PRL 93 021802 Limits on the Neutrino Magnetic Moment using 1495 Days of Super-Kamiokande-I Solar Neutrino Data
BACK 2003B
PL B563 35 Study of the Neutrino Electromagnetic Properties with Prototype of BOREXINO Detector
DARAKTCHIEVA 2003
PL B564 190 Limits on the Neutrino Magnetic Moment from the MUNU Experiment
LI 2003B
PRL 90 131802 Limit on the Electron Neutrino Magnetic Moments from the Kuo-Sheng Reactor Neutrino Experiment
GRIMUS 2002
NP B648 376 Constraining Majorana Neutrino Electromagnetic Properties from the LMA-MSW Solution of the Solar Neutrino Problem
AUERBACH 2001
PR D63 112001 Measurement of ${{\mathit \nu}_{{e}}}{{\mathit e}^{-}}$ Elastic Scattering
SCHWIENHORST 2001
PL B513 23 A New Upper Limit for the ${{\mathit \nu}_{{\tau}}}$ Magnetic Moment
TANIMOTO 2000
PL B478 1 Bound on the ${{\mathit \nu}_{{\tau}}}$ Magnetic Moment from the TRISTAN Experiments
AYALA 1999
PR D59 111901 Bound on the Neutrino Magnetic Moment from Chirality Flip in Supernovae
BEACOM 1999
PRL 83 5222 Neutrino Magnetic Moments, Flavor Mixing, and the Super-Kamiokande Solar Data
RAFFELT 1999
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ABREU 1997J
ZPHY C74 577 Search for New Phenomena using Single Photon Events in the DELPHI Detector at LEP
ACCIARRI 1997Q
PL B412 201 Search for New Physics in Energetic Single Photon Production in ${{\mathit e}^{+}}{{\mathit e}^{-}}$ Annihilation at the ${{\mathit Z}}$ Resonance
ELMFORS 1997
NP B503 3 Neutrinos with Magnetic Moment: Depolarization Rate in Plasma
ESCRIBANO 1997
PL B395 369 Improved Bounds on the Electromagnetic Dipole Moments of the ${{\mathit \tau}}$ Lepton
VILAIN 1995B
PL B345 115 Experimental Study of Electromagnetic Properties of the Muon Neutrino in Neutrino Electron Scattering
GOULD 1994
PL B333 545 Bounding the ${{\mathit \nu}_{{\tau}}}$ Magnetic Moment from Single Photon Searches at LEP
DERBIN 1993
JETPL 57 768 Experiment on Antineutrino Scattering by Electrons at a Reactor of the Rovno Nuclear Power Plant
COOPER-SARKAR 1992
PL B280 153 Bound on the ${{\mathit \nu}_{{\tau}}}$ Magnetic Moment from the BEBC Beam Dump Experiment
VIDYAKIN 1992
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PR D43 943 Limit on ${{\mathit \nu}_{{\tau}}}$ Magnetic Moment from Neutrino Counting
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AHRENS 1990
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PL B252 177 Limits on the Neutrino Magnetic Moment from a Measurement of Neutrino-Electron Elastic Scattering
RAFFELT 1990
PRL 64 2856 New Bound on Neutrino Dipole Moments from Globular Cluster Stars
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FUKUGITA 1988
PRL 60 879 Magnetically Induced Neutrino Oscillations and Neutrino Refractive Effects in the Early Universe
GROTCH 1988
ZPHY C39 553 Limits on the ${{\mathit \nu}_{{\tau}}}$ Electromagnetic Properties from Single Photon Searches at ${{\mathit e}^{+}}{{\mathit e}^{-}}$ Colliders
RAFFELT 1988B
PR D37 549 Bounds on Weakly Interacting Particles from Observational Lifetimes of Helium Burning Stars
FUKUGITA 1987
PR D36 3817 Reexamination of Astrophysical and Cosmological Constraints on the Magnetic Moment of Neutrinos
NUSSINOV 1987
PR D36 2278 Magnetic Moments of Neutrinos: Particle and Astrophysical Aspects
MORGAN 1981
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BEG 1978
PR D17 1395 Properties of Neutrinos in a Class of Gauge Theories
SUTHERLAND 1976
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BERNSTEIN 1963
PR 132 1227 Electromagnetic Properties of the Neutrino
COWAN 1957
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PRL 61 27 Limit on the Magnetic Moment of the Neutrino from Supernova SN1987a Observations
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FUJIKAWA 1980
PRL 45 963 The Magnetic Moment of a Massive Neutrino and Neutrino Spin Rotation