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 $\bf{<0.064}$ 90 1 APRILE 2022 B XENT 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. • • $<0.16$ 5 CARENZA 2024 A COSM $<0.136$ 90 6 AALBERS 2023 A LZ Solar ${{\mathit \nu}}$ spectrum $<0.11$ 90 7 ATZORI-CORONA 2023 FIT Solar ${{\mathit \nu}}$ spectrum $<0.75$ 90 8 BONET 2022 A CONU Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<2.8$ 90 9 COLOMA 2022 CNTR Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<1.8$ 90 10 ABE 2020 E XMAS Solar ${{\mathit \nu}}$ spectrum $\text{0.14 - 0.29}$ 90 11 APRILE 2020 XE1T Solar ${{\mathit \nu}}$ spectrum $<0.012$ 95 12 CAPOZZI 2020 ASTR Tip of the Red-Giant Branch $\text{0.2 - 0.4}$ 68 13 KHAN 2020 Spectral fit of XENON1T $<0.28$ 90 14 AGOSTINI 2017 A BORX Solar ${{\mathit \nu}}$ spectrum $<0.022$ 90 15 ARCEO-DIAZ 2015 ASTR Red giants $<0.1$ 95 16 CORSICO 2014 ASTR $<0.05$ 95 17 MILLER-BERTOL.. 2014 B ASTR $<0.045$ 95 18 VIAUX 2013 A ASTR Globular cluster M5 $<0.32$ 90 19 BEDA 2010 CNTR Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<2.2$ 90 20 DENIZ 2010 TEXO Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $\text{<0.011 - 0.027}$ 21 KUZNETSOV 2009 ASTR ${{\mathit \nu}_{{{L}}}}$ $\rightarrow$ ${{\mathit \nu}_{{{R}}}}$ in SN1987A $<0.54$ 90 22 ARPESELLA 2008 A BORX Solar ${{\mathit \nu}}$ spectrum $<0.58$ 90 23 BEDA 2007 CNTR Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<0.74$ 90 24 WONG 2007 CNTR Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<0.9$ 90 25 DARAKTCHIEVA 2005 Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<130$ 90 26 XIN 2005 CNTR Reactor ${{\mathit \nu}_{{{e}}}}$ $<37$ 95 27 GRIFOLS 2004 FIT Solar ${}^{8}\mathrm {B}{{\mathit \nu}}$ (SNO NC) $<3.6$ 90 28 LIU 2004 SKAM Solar ${{\mathit \nu}}$ spectrum $<1.1$ 90 29 LIU 2004 SKAM Solar ${{\mathit \nu}}$ spectrum (LMA region) $<5.5$ 90 30 BACK 2003 B CNTR Solar ${{\mathit p}}{{\mathit p}}$ and Be ${{\mathit \nu}}$ $<1.0$ 90 31 DARAKTCHIEVA 2003 Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<1.3$ 90 32 LI 2003 B CNTR Reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ $<2$ 90 33 GRIMUS 2002 FIT solar + reactor (Majorana ${{\mathit \nu}}$) $<80000$ 90 34 TANIMOTO 2000 RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ $\text{<0.01 - 0.04}$ 35 AYALA 1999 ASTR ${{\mathit \nu}_{{{L}}}}$ $\rightarrow$ ${{\mathit \nu}_{{{R}}}}$ in SN$~$1987A $<1.5$ 90 36 BEACOM 1999 SKAM Solar ${{\mathit \nu}}$ spectrum $<0.03$ 37 RAFFELT 1999 ASTR Red giant luminosity $<4$ 38 RAFFELT 1999 ASTR Solar cooling $<44000$ 90 ABREU 1997 J DLPH ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ at LEP $<33000$ 90 39 ACCIARRI 1997 Q L3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ at LEP $<0.62$ 40 ELMFORS 1997 COSM Depolarization in early universe plasma $<27000$ 95 41 ESCRIBANO 1997 RVUE $\Gamma\mathrm {({{\mathit Z}} \rightarrow {{\mathit \nu}} {{\mathit \nu}})}$ at LEP $<30$ 90 VILAIN 1995 B 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 42 DERBIN 1993 CNTR Reactor ${{\overline{\mathit \nu}}}$ ${{\mathit e}}$ $\rightarrow$ ${{\overline{\mathit \nu}}}{{\mathit e}}$ $<5400$ 90 43 COOPER-SARKAR 1992 BEBC ${{\mathit \nu}_{{{\tau}}}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}_{{{\tau}}}}{{\mathit e}^{-}}$ $<2.4$ 90 44 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 45 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 46 KRAKAUER 1990 CNTR LAMPF ${{\mathit \nu}}$ ${{\mathit e}}$ $\rightarrow$ ${{\mathit \nu}}{{\mathit e}}$ $<7.4$ 90 46 KRAKAUER 1990 CNTR LAMPF (${{\mathit \nu}_{{{\mu}}}}$, ${{\overline{\mathit \nu}}_{{{\mu}}}}$ ) ${{\mathit e}}$ elast. $<0.02$ 47 RAFFELT 1990 ASTR Red giant luminosity $<0.1$ 48 RAFFELT 1989 B ASTR Cooling helium stars 49 FUKUGITA 1988 COSM Primordial magn. fields $<40000$ 90 50 GROTCH 1988 RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ $<=.3$ 48 RAFFELT 1988 B ASTR ${}^{}\mathrm {He}$ burning stars $<0.11$ 48 FUKUGITA 1987 ASTR Cooling helium stars $<0.0006$ 51 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 $<0.6$ 52 SUTHERLAND 1976 ASTR Red giants + degenerate dwarfs $<81$ 53 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  APRILE 2022B use data collected with the XENONnT dark matter detector to place a limit on an enhanced magnetic moment of solar neutrinos. Supersedes APRILE 2020. 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  CARENZA 2024A derive the limit from the production of right-handed neutrinos in the early universe. 6  AALBERS 2023A utilize the first 60 days of data collected by the LZ dark matter search to place a limit on the magnetic moment of solar neutrinos. Low energy electron-recoil events are utilized. This LZ-collaboration analysis supersedes that of the external authors in ATZORI-CORONA 2023 because of a more complete treatment of experiment uncertainties. 7  ATZORI-CORONA 2023 use LUX-ZEPLIN dark matter search data published by AALBERS 2023 to place a limit on an enhanced magnetic moment of solar neutrinos. 8  BONET 2022A use data collected by four low-threshold ${}^{}\mathrm {Ge}$ detectors, placed 17.1 m from one of the cores of the nuclear reactors at Brokdorf to derive this limit. A spectral analysis is performed on reactor on and off data. 9  COLOMA 2022 present a re-analysis of data taken by the COHERENT and Dresden-II experiments. The combination of both experiments is used to place a limit on the magnetic moment of electron-type neutrinos. The presented value is one-sided limit as recommended by the authors; the two-sided limit is $<3.2 \times 10^{-10}\mu _{B}$ at 90$\%$ C.L. Results based on Fef and YBe quenching models are reported in the paper. The authors are not part of either collaboration. 10  ABE 2020E observed an excess of low-energy events in the XMASS detector, which could be interpreted as a signal produced by a neutrino magnetic moment with this magnitude. 11  APRILE 2020 observed an excess of low-energy events in the XENON1T detector, which could be interpreted as a signal produced by a neutrino magnetic moment with this magnitude. 12  CAPOZZI 2020 obtains a limit on the neutrino dipole moment from the brightness of the tip of the red-giant branch in $\omega $ Centauri. A similar limit of ${{\mathit \mu}_{{{\nu}}}}$ $<$ $1.5 \times 10^{-12}{{\mathit \mu}_{{{B}}}}$ is obtained in NGC 4258. 13  KHAN 2020 performed a constrained spectral fit analysis of the excess observed in the electron recoil energy spectrum by the XENON1T experiment. This range of the ${{\mathit \mu}_{{{B}}}}$ values is one of the possible interpretations of these excess events. For the individual flavor constraints at 90$\%$ C.L. see the original reference. 14  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. 15  ARCEO-DIAZ 2015 constrains the neutrino magnetic moment from observation of the tip of the red giant branch in the globular cluster $\omega $-Centauri. 16  CORSICO 2014 constrains the neutrino magnetic moment from observations of white drarf pulsations. 17  MILLER-BERTOLAMI 2014B constrains the neutrino magnetic moment from observations of the white dwarf luminosity function of the Galactic disk. 18  VIAUX 2013A constrains the neutrino magnetic moment from observations of the globular cluster M5. 19  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. 20  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. 21  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. 22  ARPESELLA 2008A obtained this limit using the shape of the recoil electron energy spectrum from the Borexino 192 live days of solar neutrino data. 23  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. 24  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. 25  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. 26  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 ${{\mathit \nu}_{{{e}}}}$. 27  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 ${{\mathit \mu}}_{{\mathrm {eff}}}$ = (${{\mathit \mu}}{}^{2}_{21}$ + ${{\mathit \mu}}{}^{2}_{22}$ + ${{\mathit \mu}}{}^{2}_{23}){}^{1/2}$. 28  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. 29  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. 30  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). 31  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. 32  LI 2003B used Ge detector in active shield near nuclear reactor to test for nonstandard ${{\overline{\mathit \nu}}_{{{e}}}}-{{\mathit e}}$ scattering. 33  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. 34  TANIMOTO 2000 combined ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}{{\mathit \gamma}}$ data from VENUS, TOPAZ, and AMY. 35  AYALA 1999 improves the limit of BARBIERI 1988. 36  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. 37  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. 38  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. 39  ACCIARRI 1997Q result applies to both direct and transition magnetic moments and for $\mathit q{}^{2}$=0. 40  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. 41  Applies to absolute value of magnetic moment. 42  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. 43  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. 44  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. 45  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 $\mu\mathrm {({{\mathit \nu}})}$ = $\mu\mathrm {({{\overline{\mathit \nu}}})}$. 46  KRAKAUER 1990 experiment fully reported in ALLEN 1993. 47  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 $\delta \mathit M_{\mathit c}$. 48  Significant dependence on details of stellar models. 49  FUKUGITA 1988 find magnetic dipole moments of any two neutrino species are bounded by $\mu $ $<$ $10^{-16}$ $\lbrack{}10^{-9}~\mathit G/{{\mathit B}}_{0}$] where ${{\mathit B}}_{0}$ is the present-day intergalactic field strength. 50  GROTCH 1988 combined data from MAC, ASP, CELLO, and Mark$~$J. 51  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. 52  We obtain above limit from SUTHERLAND 1976 using their limit $\mathit f$ $<$ 1/3. 53  KIM 1974 is a theoretical analysis of ${{\overline{\mathit \nu}}_{{{\mu}}}}$ reaction data.

References