Solar Neutrinos

Useful Links

References

Useful Links

Solar Neutrino Experiments

Bahcall et al. Standard Solar Models: BU88, BP92, BP95, BP98, BP00, BP04, BS05.

Software and Data by J. Bahcall. New (June 2002): ⁷Be line shape data, from Phys. Rev. D 49 (1994) 3923. Has some effect in the BOREXino predictions for some part of the space of parameters (Carlos Peña Garay). The damping of oscillations due to the ⁷Be line shape is more important than averaging over the radial distribution of neutrino production in the Sun (John Bahcall). See: Fogli, Lisi, Montanino, Palazzo, PRD 62, 113004 (2000), hep-ph/0005261, Sec. VI and Fig. 5, and Lisi, Marrone, Montanino, Palazzo, Petcov, PRD 63, 093002 (2001), hep-ph/0011306, Fig. 8 and related comments.

Super-Kamiokande-I Solar Neutrino Data

Tables and Figures of Neutrino (Anti-Neutrino) Deuteron Reactions Cross Sections

Living Reviews in Solar Physics

Solar Physics (NASA's Marshall Space Flight Center)

Solar Physics Glossary

The Solar and Heliospheric Observatory (SOHO)

APS Neutrino Study: Solar and Atmospheric Neutrino Experiments Working Group

NASA Astronomy Picture of the Day (5 June 1998): Neutrinos in the Sun

References

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[1-5]

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Solar Neutrinos, R.G.H. Robertson, Prog. Part. Nucl. Phys. 57 (2006) 90, arXiv:nucl-ex/0602005. International School on Nuclear Physics; 27th Course: "Neutrinos in Cosmology, in Astro, Particle and Nuclear Physics" in Erice, Sicily, Italy; September 16 - 24, 2005.

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[3-9]

Recent Results of non-accelarator-based neutrino experiments, Yifang Wang, Int. J. Mod. Phys. A20 (2005) 5244, arXiv:hep-ex/0411028. "32nd International Conference on High Energy Physics", Aug. 16-22, 2004, Beijing, P.R. China.

[3-10]

Review of Solar Neutrino Experiments, Alain Bellerive, Int. J. Mod. Phys. A19 (2004) 1167, arXiv:hep-ex/0312045. XXI International Symposium on Lepton and Photon Interactions at High Energies, Fermilab, USA, 11-16 August 2003.

[3-11]

Neutrino Physics: Experimental Status, Kajita, T., 2003. 19th International Workshop on Weak Interactions and Neutrinos, WIN2003, October 6-11, Lake Geneva, Wisconsin, USA. http://conferences.fnal.gov/win03/Talks/Takaaki%20Kajita.pdf.
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[3-12]

Solar Neutrinos, Nishikawa, K., 2002. Topical Seminar on Frontier of Particle Physics 2002: Neutrinos and Cosmology, 20-25 August 2002, Beijing, China. http://bes.ihep.ac.cn/particle/2002/presentation/K.Nishikawa/TALK_1.ZIP.

[4-1]

Radiochemical solar neutrino experiments, successful and otherwise, Richard L. Hahn, 2008. Neutrino 2008, 26-31 May 2008, Christchurch, New Zealand. http://www2.phys.canterbury.ac.nz/~jaa53/presentations/Hahn.pdf.

[5-1]

How the sun shines, Bahcall, John N., SLAC Beam Line 31N1 (2001) 2-12, arXiv:astro-ph/0009259.

[6-1]

Solar neutrinos, helioseismology and the solar internal dynamics, Turck-Chieze, S., Couvidat, S., Rept. Prog. Phys. 74 (2011) 086901, arXiv:1009.0852.

[6-2]

Solar fusion cross sections II: the pp chain and CNO cycles, E. G. Adelberger et al., arXiv:1004.2318, 2010.

[6-3]

Astrophysics in 2005, V. Trimble, M.J. Aschwanden, C.J. Hansen, arXiv:astro-ph/0606663, 2006.

[6-4]

Solar hydrogen burning and neutrinos, Haxton, W. C., Parker, P. D., Rolfs, C. E., Nucl. Phys. A777 (2006) 226-253, arXiv:nucl-th/0501020.

[6-5]

Helioseismology, Antia, H. M., J. Astrophys. Astr. 26 (2005) 161-169.

[6-6]

The Solar Hep Process, Kuniharu Kubodera, Tae-Sun Park, Ann. Rev. Nucl. Part. Sci. 54 (2004) 19, arXiv:nucl-th/0402008.

[6-7]

Fusion cycles in stars and stellar neutrinos, G. Wolschin, arXiv:astro-ph/0210032, 2002.

[6-8]

Solar fusion cross-sections, Adelberger, Eric G. et al., Rev. Mod. Phys. 70 (1998) 1265-1292, arXiv:astro-ph/9805121.

[6-9]

Standard Solar Composition, Grevesse, N., Sauval, A. J., Space Sci. Rev. 85 (1998) 161-174.

[6-10]

The Internal Constitution of the Stars, A. S. Eddington, Observatory 43 (1920) 353.

[7-1]

Solar neutrinos and the sun, Aldo Serenelli, arXiv:1109.2602, 2011. XIV International Workshop on 'Neutrino Telescopes', March 15-18, 2011, Venice, Italy.

[7-2]

Nuclear Astrophysics: CIPANP 2006, Haxton, W. C., AIP Conf. Proc. 870 (2006) 33-43, arXiv:nucl-th/0609006. CIPANP 2006.

[7-3]

Helioseismology, Neutrinos and Radiative Zones, S. Turck-Chieze, S. Couvidat, L. Piau, arXiv:astro-ph/0511008, 2005. Mons 2005: Element Stratifications in Stars: 40 Years of Atomic Diffusion: Meeting in Honor of Georges Michaud, Mons, France, 6-10 June 2005.

[7-4]

The solar chemical composition, Martin Asplund, Nicolas Grevesse, Jacques Sauval, Nucl. Phys. A777 (2006) 1-4, arXiv:astro-ph/0410214. International Symposium on Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis in Honor of Professor David Lambert, Austin, Texas, 17-19 June 2004.

[7-5]

Solar Fusion and The Coulomb Dissociation of 8B; What Have We Learned and Where Do We Go From Here?, Moshe Gai, Heavy Ion Phys. 21 (2004) 335, arXiv:nucl-ex/0303009. 19th Winter Workshop on Nuclear Dynamics, Breckenridge, Colorado, 9-15 Feb 2003.

[7-6]

Review of solar models and helioseismology, Turck-Chieze, S., Nucl. Phys. Proc. Suppl. 91 (2001) 73-79.

[8-1]

Neutrino Physics and The Solar Neutrino Problem, Andrew John Lowe, arXiv:0907.3658, 2009.

[8-2]

The Scientific Life Of John Bahcall, W. C. Haxton, Ann. Rev. Nucl. Part. Sci. 59 (2009) 1-20, arXiv:0904.2865.

[8-3]

Phenomenology with Massive Neutrinos, Gonzalez-Garcia, M. C., Maltoni, Michele, Phys. Rept. 460 (2008) 1-129, arXiv:0704.1800.

[8-4]

Global analysis of three-flavor neutrino masses and mixings, Fogli, G. L., Lisi, E., Marrone, A., Palazzo, A., Prog. Part. Nucl. Phys. 57 (2006) 742-795, arXiv:hep-ph/0506083.

[8-5]

Report of the Solar and Atmospheric Neutrino Experiments Working Group of the APS Multidivisional Neutrino Study, H. Back et al., arXiv:hep-ex/0412016, 2004.

[8-6]

Solar models and solar neutrino oscillations, Bahcall, John N., Pena-Garay, Carlos, New J. Phys. 6 (2004) 63, arXiv:hep-ph/0404061.

[8-7]

Low Energy Neutrino Physics after SNO and KamLAND, Lothar Oberauer, Mod. Phys. Lett. A19 (2004) 337, arXiv:hep-ph/0402162.

[8-8]

Theoretical neutrino physics, Murayama, H., Eur. Phys. J. C33 (2004) s51-s66. http://www.edpsciences.org/articles/epjc/pdf/2004/19/10052S51.pdf?access=ok.

[8-9]

Evidence for the MSW effect, Fogli, Gianluigi, Lisi, Eligio, New J. Phys. 6 (2004) 139.

[8-10]

Neutrino Mixing, Carlo Giunti, Marco Laveder, arXiv:hep-ph/0310238, 2003. In "Developments in Quantum Physics - 2004", p. 197-254, edited by F. Columbus and V. Krasnoholovets, Nova Science, Hauppauge, NY. http://novapublishers.com/catalog/product_info.php?products_id=1633.

[8-11]

Solar neutrino physics: Historical evolution, present status and perspectives, L. Miramonti, F. Reseghetti, La Rivista del Nuovo Cimento 25 (2002) 1, arXiv:hep-ex/0302035.

[8-12]

Direct observation of neutrino oscillations at the Sudbury Neutrino Observatory, Ananthanarayan, B., Singh, Ritesh K., Curr. Sci. 83 (2002) 553, arXiv:physics/0208096.

[8-13]

Neutrino Masses and Mixing: Evidence and Implications, M.C. Gonzalez-Garcia, Y. Nir, Rev. Mod. Phys. 75 (2003) 345-402, arXiv:hep-ph/0202058.

[8-14]

The solar neutrino problem and its oscillation solution, Smy, M. B., Mod. Phys. Lett. A17 (2002) 2163-2178.

[8-15]

Solar neutrinos, Altmann, M. F., Mossbauer, R. L., Oberauer, L. J. N., Rept. Prog. Phys. 64 (2001) 97-146.

[8-16]

Solar neutrinos, Suzuki, Yoichiro, Int. J. Mod. Phys. A15S1 (2000) 201-228.

[8-17]

Phenomenology of neutrino oscillations, S. M. Bilenky, C. Giunti, W. Grimus, Prog. Part. Nucl. Phys. 43 (1999) 1, arXiv:hep-ph/9812360.

[8-18]

Solar neutrinos: Beyond standard solar models, Castellani, V., Degl'Innocenti, S., Fiorentini, G., Lissia, M., Ricci, B., Phys. Rep. 281 (1997) 309-398, arXiv:astro-ph/9606180.

[8-19]

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[8-20]

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[8-21]

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[8-22]

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[8-23]

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[8-24]

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[9-1]

Neutrinos and the stars, Georg Raffelt, arXiv:1201.1637, 2012. ISAPP School 'Neutrino Physics and Astrophysics', 26 July-5 August 2011, Villa Monastero, Varenna, Italy.

[9-2]

New Results on Solar Neutrinos, Alain Bellerive, PoS ICHEP2010 (2010) 529, arXiv:1012.2493. 35th International Conference of High Energy Physics, Paris, France, July 22-28, 2010.

[9-3]

Lectures on neutrino phenomenology, Walter Winter, Nucl. Phys. B, Proc. Suppl. 203-204 2010 (2010) 45-81, arXiv:1004.4160. Schladming Winter School 2010 'Masses and Constants'.

[9-4]

Significance of neutrino cross-sections for astrophysics, A.B. Balantekin, AIP Conf. Proc. 1189 (2009) 11-15, arXiv:0909.0226. NUINT2009 (6th International Workshop on Neutrino-Nucleus Interactions in the Few-GeV Region), May 18-22, 2009, Sitges, Barcelona, Spain.

[9-5]

Muons and Neutrinos 2007, Thomas K. Gaisser, arXiv:0801.4542, 2008. 30th International Cosmic Ray Conference, Merida, Yucatan, July, 2007.

[9-6]

Solar Neutrinos: Models, Observations, and New Opportunities, W. C. Haxton, Publ. Astron. Soc. Austral. 25 (2008) 44-51, arXiv:0710.2295. Nuclear Astrophysics 1957:2007: Beyond the First 50 Years, Caltech, July, 2007.

[9-7]

Global fits to neutrino oscillation data, Thomas Schwetz, Phys. Scripta T127 (2006) 1-5, arXiv:hep-ph/0606060. SNOW2006 workshop, Stockholm, 2-6 May 2006.

[9-8]

Neutrino oscillations: Current status and prospects, Thomas Schwetz, Acta Phys. Polon. B36 (2005) 3203, arXiv:hep-ph/0510331. XXIX International Conference of Theoretical Physics, "Matter To The Deepest: Recent Developments In Physics of Fundamental Interactions", 8-14 September 2005, Ustron, Poland.

[9-9]

Status of the Standard Solar Model Prediction of Solar Neutrino Fluxes, Moshe Gai, Phys. Atom. Nucl. 69 (2006) 1805-1811, arXiv:nucl-ex/0510081. Fifth International Conferenceon Non-Accelerator New Physics, Dubna, June 20-25, 2005.

[9-10]

Neutrino mass and mixing parameters: A short review, G.L. Fogli et al., arXiv:hep-ph/0506307, 2005. 40th Rencontres de Moriond on Electroweak Interactions and Unified Theories, La Thuile, Aosta Valley, Italy, 5-12 Mar 2005.

[9-11]

Solar Models and Solar Neutrinos: Current Status, John N. Bahcall, Phys. Scripta T121 (2005) 46, arXiv:hep-ph/0412068. Nobel Symposium 2004, Enkoping, Sweden, August 19-24, 2004.

[9-12]

Three-flavour effects and CP- and T-violation in neutrino oscillations, Evgeny Akhmedov, Phys. Scripta T121 (2005) 65, arXiv:hep-ph/0412029. Nobel Symposium 129 - Neutrino Physics, Haga Slott, Enkoping, Sweden, August 19-24, 2004.

[9-13]

Physics of Massive Neutrinos, J. W. F. Valle, Nucl. Phys. Proc. Suppl. 149 (2005) 3, arXiv:hep-ph/0410103. Sixth International Conf. on Neutrino Factories and SuperBeams (NuFact04) Osaka, Japan, July 26-August 1, 2004.

[9-14]

Neutrino 2004: Concluding Talk, Guido Altarelli, Nucl. Phys. Proc. Suppl. 143 (2005) 470, arXiv:hep-ph/0410101. Neutrino 2004, Paris, 14-19 June 2004.

[9-15]

Global Analysis of Neutrino Data, M. C. Gonzalez-Garcia, Phys. Scripta T121 (2005) 72, arXiv:hep-ph/0410030. Nobel Symposium on Neutrino Physics, Haga Slott, Enkoping, Sweden.

[9-16]

Solar Neutrino Oscillation - An Overview, D. P. Roy, arXiv:hep-ph/0409336, 2004. Xth International Symposium on Particles, Strings and Cosmology (PASCOS), Boston, 16-22 August 2004.

[9-17]

Solar Neutrino Oscillation Parameters in Experiments with Reactor Anti-Neutrinos, Sandhya Choubey, arXiv:hep-ph/0402288, 2004. 2nd International Workshop on Neutrino oscillations in Venice (NOVE), December 3-5, 2003, Venice, Italy.

[9-18]

Neutrinos: "...annus mirabilis", A. Yu. Smirnov, arXiv:hep-ph/0402264, 2004. 2nd Int. Workshop on Neutrino oscillations in Venice (NOVE) December 3-5, 2003, Venice, Italy.

[9-19]

Global analysis of neutrino oscillation, S. Goswami, 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/tuesday/goswami.pdf.

[9-20]

Neutrino physics, recent results, Lisi, E., 2004. IFAE-2004, 14-16 April 2004, Torino, Italy. http://agenda.cern.ch/askArchive.php?base=agenda&categ=a041654&id=a041654s3t6/transparencies, http://www.ph.unito.it/ifae/Proceedings/Sessioni/Neutrinos.pdf.

[9-21]

Solar neutrino oscillation phenomenology, Goswami, S., Pramana 62 (2004) 241, arXiv:hep-ph/0307224. 9th International Symposium on Particles, Strings and Cosmology (PASCOS 03), Mumbai, India, 3-8 Jan 2003.

[9-22]

Neutrino masses twenty-five years later, Valle, J. W. F., Aip Conf. Proc. 687 (2003) 16, arXiv:hep-ph/0307192. MRST'03 (Joe-Fest), Syracuse, NY, May 2003.

[9-23]

Neutrino oscillations in the framework of the tree-neutrino mixing, Bilenky, S. M., arXiv:hep-ph/0307186, 2003. Ist Yamada Symposium Om neutrinos and Dark Matter in Nuclear Physics, June 9-14, 2003, Nara, Japan.

[9-24]

Neutrino Physics after KamLAND, Smirnov, A. Yu., arXiv:hep-ph/0306075, 2003. 4th Workshop on "Neutrino Oscillations and their Origin" (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Smirnov.pdf.

[9-25]

Status of Neutrino Fits, C. Giunti, arXiv:hep-ph/0305139, 2003. XXXVIIIth Rencontres de Moriond, ElectroWeak Interactions and Unified Theories, 15-22 March 2003, Les Arcs, France. http://moriond.in2p3.fr/EW/2003/Transparencies/1_Sunday/1_2_afternoon/1_2_6_Giunti/C.Giunti.pdf.

[9-26]

The MSW effect and Solar Neutrinos, A. Yu. Smirnov, arXiv:hep-ph/0305106, 2003. 11th workshop on Neutrino Telescopes, Venice, March 11- 14, 2003.

[9-27]

Neutrino Masses and Mixing: Where We Stand and Where We are Going, M. C. Gonzalez-Garcia, arXiv:hep-ph/0211054, 2002. 10th International Conference on Supersymmetry and Unification of Fundamental Interactions, SUSY02 (June 17-23, 2002, DESY, Hamburg).

[9-28]

Theory of Neutrino Masses and Mixing, M. C. Gonzalez-Garcia, Nucl. Phys. Proc. Suppl. 117 (2003) 186, arXiv:hep-ph/0210359. 31st international conference on high energy physics (ICHEP 2002), Amsterdam, 24-31 July 2002.

[9-29]

Current Status of Neutrino Masses and Mixings, Giunti, C., arXiv:hep-ph/0209103, 2002. 31st International Conference on High Energy Physics "ICHEP02", 24-31 July 2002, Amsterdam. http://www.ichep02.nl/Transparencies/NEU/NEU-2/NEU-2-1.giunti.ps.

[9-30]

Global analysis of solar neutrinos, Choubey, S., 2002. Fourth NuFact '02 Workshop on Neutrino Factories based on Muon Storage Rings, Imperial College, London, 1-6 July 2002. http://www.hep.ph.ic.ac.uk/NuFact02/Scientific-programme/files/Wednesday/wg2/A01_choubey.ps.

[9-31]

Actuality and potentiality of neutrino mixing, Giunti, C., 2002. IIIrd International Workshop on Low Energy Solar Neutrinos - LowNu 2002, 22-24 May 2002, Heidelberg, Germany. http://www.mpi-hd.mpg.de/nubis/www_lownu2002/transparency/giunti_lownu_2002.pdf.

[10-1]

First evidence of pep solar neutrinos by direct detection in Borexino, G. Bellini et al. (Borexino), arXiv:1110.3230, 2011.

[10-2]

Combined Analysis of all Three Phases of Solar Neutrino Data from the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), arXiv:1109.0763, 2011.

[10-3]

Measurement of the and Total B Solar Neutrino Fluxes with the Sudbury Neutrino Observatory Phase-III Data Set, B. Aharmim et al. (SNO), arXiv:1107.2901, 2011.

[10-4]

Measurement of the 8B Solar Neutrino Flux with KamLAND, S. Abe et al. (KamLAND), Phys. Rev. C84 (2011) 035804, arXiv:1106.0861.

[10-5]

Absence of day-night asymmetry of 862 keV solar neutrino rate in Borexino and MSW oscillation parameters, G. Bellini et al. (Borexino), Phys. Lett. B707 (2012) 22-26, arXiv:1104.2150.

[10-6]

Precision measurement of the solar neutrino interaction rate in Borexino, G. Bellini et al. (Borexino), (2011), arXiv:1104.1816.

[10-7]

Solar neutrino results in Super-Kamiokande-III, K. Abe et al. (Super-Kamiokande), Phys. Rev. D83 (2011) 052010, arXiv:1010.0118.

[10-8]

Study of solar and other unknown anti-neutrino fluxes with Borexino at LNGS, G.Bellini (Borexino), Phys. Lett. B696 (2011) 191-196, arXiv:1010.0029.

[10-9]

Reanalysis of the GALLEX solar neutrino flux and source experiments, F. Kaether, W. Hampel, G. Heusser, J. Kiko, T. Kirsten, Phys. Lett. B685 (2010) 47-54, arXiv:1001.2731.

[10-10]

Low Energy Threshold Analysis of the Phase I and Phase II Data Sets of the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Phys. Rev. C81 (2010) 055504, arXiv:0910.2984.

[10-11]

Searches for High Frequency Variations in the Solar Neutrino Flux at the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Astrophys. J. 710 (2010) 540-548, arXiv:0910.2433.

[10-12]

Measurement of the solar neutrino capture rate with Gallium metal, Part III, Abdurashitov, J. N. et al. (SAGE), Phys. Rev. C80 (2009) 015807, arXiv:0901.2200.

[10-13]

Measurement of the solar neutrino flux with 246 live days of Borexino and observation of the MSW vacuum-matter transition, G. Bellini et al. (BOREXino), Phys. Rev. D82 (2010) 033006, arXiv:0808.2868.

[10-14]

The Borexino detector at the Laboratori Nazionali del Gran Sasso, G. Alimonti et al. (Borexino), Nucl. Instrum. Meth. A600 (2009) 568-593, arXiv:0806.2400.

[10-15]

An Independent Measurement of the Total Active 8B Solar Neutrino Flux Using an Array of 3He Proportional Counters at the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Phys. Rev. Lett. 101 (2008) 111301, arXiv:0806.0989.

[10-16]

New results on solar neutrino fluxes from 192 days of Borexino data, C. Arpesella et al. (BOREXino), Phys. Rev. Lett. 101 (2008) 091302, arXiv:0805.3843.

[10-17]

Solar neutrino measurements in Super-Kamiokande-II, J.P. Cravens et al. (Super-Kamiokande), Phys. Rev. D78 (2008) 032002, arXiv:0803.4312.
From the abstract: The results of the second phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first phase. The solar neutrino flux spectrum and time-variation as well as oscillation results are statistically consistent with the first phase and do not show spectral distortion. The time-dependent flux measurement of the combined first and second phases coincides with the full period of solar cycle 23 and shows no correlation with solar activity.

[10-18]

First real time detection of solar neutrinos by BOREXino, C. Arpesella et al. (BOREXino), Phys. Lett. B658 (2008) 101-108, arXiv:0708.2251.

[10-19]

Measurement of the and Total Solar Neutrino Fluxes with the Sudbury Neutrino Observatory Phase I Data Set, B. Aharmim et al. (SNO), Phys. Rev. C75 (2007) 045502, arXiv:nucl-ex/0610020.

[10-20]

A Search for Neutrinos from the Solar hep Reaction and the Diffuse Supernova Neutrino Background with the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Astrophys. J. 653 (2006) 1545-1551, arXiv:hep-ex/0607010.

[10-21]

Search for electron antineutrino interactions with the BOREXino Counting Test Facility at Gran Sasso, M. Balata et al. (BOREXino), Eur. Phys. J. C47 (2006) 21-30, arXiv:hep-ex/0602027.

[10-22]

The SAGE@LNGS experiment: Measurement of solar neutrinos at LNGS using gallium from SAGE, Abdurashitov, J. N. et al., Astropart. Phys. 25 (2006) 349-354, arXiv:nucl-ex/0509031.

[10-23]

Solar neutrino measurements in Super-Kamiokande-I, Hosaka, J. et al. (Super-Kamkiokande), Phys. Rev. D73 (2006) 112001, arXiv:hep-ex/0508053.

[10-24]

A Search for Periodicities in the Solar Neutrino Flux Measured by the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Phys. Rev. D72 (2005) 052010, arXiv:hep-ex/0507079.
From the abstract: The variation at a period of one year is consistent with modulation of the neutrino flux by the Earth's orbital eccentricity. No significant sinusoidal periodicities are found with periods between 1 day and 10 years.

[10-25]

Complete results for five years of GNO solar neutrino observations, M. Altmann et al. (GNO), Phys. Lett. B616 (2005) 174, arXiv:hep-ex/0504037.

[10-26]

Electron Energy Spectra, Fluxes, and Day-Night Asymmetries of Solar Neutrinos from the 391-Day Salt Phase SNO Data Set, B. Aharmim et al. (SNO), Phys. Rev. C72 (2005) 055502, arXiv:nucl-ex/0502021.

[10-27]

Electron Antineutrino Search at the Sudbury Neutrino Observatory, B. Aharmim et al. (SNO), Phys. Rev. D70 (2004) 093014, arXiv:hep-ex/0407029.

[10-28]

Limit On the Neutrino Magnetic Moment Using 1496 Days of Super-Kamiokande-i Solar Neutrino Data, D. W. Liu et al. (Super-Kamiokande), Phys. Rev. Lett. 93 (2004) 021802, arXiv:hep-ex/0402015.

[10-29]

Precise Measurement of the Solar Neutrino Day/Night and Seasonal Variation in Super-Kamiokande-I, M. B. Smy et al. (Super-Kamiokande), Phys. Rev. D69 (2004) 011104, arXiv:hep-ex/0309011.

[10-30]

Measurement of the Total Active 8B Solar Neutrino Flux at the Sudbury Neutrino Observatory with Enhanced Neutral Current Sensitivity, S. N. Ahmed et al. (SNO), Phys. Rev. Lett. 92 (2004) 181301, arXiv:nucl-ex/0309004.

[10-31]

A search for periodic modulations of the solar neutrino flux in Super-Kamiokande-I, J. Yoo et al. (Super-Kamiokande), Phys. Rev. D68 (2003) 092002, arXiv:hep-ex/0307070.

[10-32]

Search for from the sun at Super-Kamiokande-I, Y. Gando et al. (Super-Kamiokande), Phys. Rev. Lett. 90 (2003) 171302, arXiv:hep-ex/0212067.
From the article: For the spectrum the upper limit to the solar flux is of the SSM flux prediction for total energy = 8 Mev - 20 MeV.

[10-33]

Determination of solar neutrino oscillation parameters using 1496 days of Super-Kamiokande-I data, S. Fukuda et al. (Super-Kamiokande), Phys. Lett. B539 (2002) 179-187, arXiv:hep-ex/0205075.

[10-34]

Measurement of the Solar Neutrino Capture Rate by the Russian-American Gallium Solar Neutrino Experiment During One Half of the 22-Year Cycle of Solar Activity, Abdurashitov, J. N. et al. (SAGE), J. Exp. Theor. Phys. 95 (2002) 181-193, arXiv:astro-ph/0204245.
From the abstract: Combined analysis of the data of 92 runs during the 12-year period January 1990 through December 2001 gives a capture rate of solar neutrinos with energy more than 233 keV of 70.8 +5.3/-5.2 (stat.) +3.7/-3.2 (syst.) SNU. This represents only slightly more than half of the predicted standard solar model rate of 130 SNU.... Using a simple analysis of the SAGE results combined with those from all other solar neutrino experiments, we estimate the electron neutrino pp flux that reaches the Earth to be (4.6 ± 1.1) × 10¹⁰ cm^-2 s^-1. Assuming that neutrinos oscillate to active flavors the pp neutrino flux emitted in the solar fusion reaction is approximately (7.7 ± 1.8) × 10¹⁰ cm^-2 s^-1, in agreement with the standard solar model calculation of (5.95 ± 0.06) × 10¹⁰ cm^-2 s^-1.

[10-35]

Measurement of Day and Night Neutrino Energy Spectra at SNO and Constraints on Neutrino Mixing Parameters, Ahmad, Q. R. et al. (SNO), Phys. Rev. Lett. 89 (2002) 011302, arXiv:nucl-ex/0204009. http://www.sno.phy.queensu.ca/sno/results_04_02/DayNight.

[10-36]

Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in the Sudbury Neutrino Observatory, Ahmad, Q. R. et al. (SNO), Phys. Rev. Lett. 89 (2002) 011301, arXiv:nucl-ex/0204008. http://www.sno.phy.queensu.ca/sno/results_04_02/NC.

[10-37]

Search for radiative decays of solar neutrinos during a solar eclipse, Giacomelli, G., Popa, V., arXiv:hep-ex/0110013, 2001.

[10-38]

Measurement of the Rate of Interactions Produced by B Solar Neutrinos at the Sudbury Neutrino Observatory, Ahmad, Q. R. et al. (SNO), Phys. Rev. Lett. 87 (2001) 071301, arXiv:nucl-ex/0106015.

[10-39]

Solar and neutrino measurements from 1258 days of Super-Kamiokande data, Fukuda, S. et al. (Super-Kamiokande), Phys. Rev. Lett. 86 (2001) 5651-5655, arXiv:hep-ex/0103032.

[10-40]

Measurement of the solar neutrino capture rate by SAGE and implications for neutrino oscillations in vacuum, J. N. Abdurashitov et al. (SAGE), Phys. Rev. Lett. 83 (1999) 4686-4689, arXiv:astro-ph/9907131.

[10-41]

Measurement of the solar neutrino capture rate with gallium metal, J. N. Abdurashitov et al. (SAGE), Phys. Rev. C60 (1999) 055801, arXiv:astro-ph/9907113.

[10-42]

GALLEX solar neutrino observations: Results for GALLEX IV, W. Hampel et al. (GALLEX), Phys. Lett. B447 (1999) 127.

[10-43]

Measurement of the solar neutrino energy spectrum using neutrino electron scattering, Fukuda, Y. et al. (Super-Kamiokande), Phys. Rev. Lett. 82 (1999) 2430-2434, arXiv:hep-ex/9812011.

[10-44]

Constraints on neutrino oscillation parameters from the measurement of day-night solar neutrino fluxes at Super- Kamiokande, Fukuda, Y. et al. (Super-Kamiokande), Phys. Rev. Lett. 82 (1999) 1810-1814, arXiv:hep-ex/9812009.

[10-45]

Measurements of the solar neutrino flux from Super- Kamiokande's first 300 days, Fukuda, Y. et al. (Super-Kamiokande), Phys. Rev. Lett. 81 (1998) 1158-1162, arXiv:hep-ex/9805021.

[10-46]

Measurement of the solar electron neutrino flux with the Homestake chlorine detector, B. T. Cleveland et al. (Homestake), Astrophys. J. 496 (1998) 505.

[11-1]

Low Energy Neutrino Astronomy in Super-Kamiokande, Michael Smy, arXiv:1110.0012, 2011. DPF 2011.

[11-2]

The Recent Results of the Solar Neutrino Measurement in Borexino, Yusuke Koshio (Borexino), arXiv:1106.3055, 2011. Recontres de Moriond EW session 2011.

[11-3]

Solar neutrino results from Borexino and main future perspectives, M. Pallavicini (Borexino), Nucl. Instrum. Meth. A630 (2011) 210-213, arXiv:0910.3367. RICAP 2009.

[11-4]

Solar Neutrino Measurement at SK-III, B.S. Yang (Super-Kamiokande), arXiv:0909.5469, 2009. DPF-2009, Detroit, MI, July 2009.

[11-5]

Searching for hep Neutrinos using the Sudbury Neutrino Observatory, Howard, Chris (SNO), arXiv:0906.0040, 2009.

[11-6]

Results from the Neutral Current Detector phase of the Sudbury Neutrino Observatory, Martin, Ryan (SNO), arXiv:0905.4907, 2009. Lake Louise Winter Institute 2009.

[11-7]

Results from the Borexino Experiment, Timo Lewke (Borexino), arXiv:0905.2526, 2009. Moriond 2009 EW session.

[11-8]

The first year of Borexino, (Borexino), arXiv:0905.1044, 2009. Heavy Quarks and Leptons, Melbourne, 2008.

[11-9]

Measurement of the Solar Neutrino Flux with an Array of Neutron Detectors in the Sudbury Neutrino Observatory, Jamieson, Blair, Collaboration, for the SNO (SNO), arXiv:0810.3760, 2008. ICHEP08.

[11-10]

Recent Results from Super-Kamiokande, Sekiya, H. et al. (Super-Kamiokande), arXiv:0810.0595, 2008. ICHEP08, Philadelphia, USA, July 2008.

[11-11]

Results and perspectives of the solar neutrino experiment Borexino, G. Ranucci (Borexino), arXiv:0810.0176, 2008. ICHEP08, Philadelphia, USA, July 2008.

[11-12]

Results from the solar neutrino experiment BOREXINO, Oberauer, Lothar (Borexino), J. Phys. Conf. Ser. 203 (2010) 012081.

[11-13]

Search for possible solar neutrino radiative decays during total solar eclipses, S. Cecchini et al., arXiv:hep-ex/0606037, 2006. SPSE2006, Waw an Namos, Libya, 27-29 March 2006.

[11-14]

Integral Fluxes, Day-Night, and Spectrum Results from SNO's 391-Day Salt Phase, Juergen Wendland et al. (SNO), arXiv:hep-ex/0507058, 2005. Lake Louise Winter Institute: Fundamental Interactions, Lake Louise, Alberta, Canada, Feb 20-26 2005.

[11-15]

Results from the Salt Phase of SNO, Miknaitis, K. (SNO), arXiv:hep-ex/0505071, 2005. XXXXth Rencontres de Moriond: Electroweak Interactions and Unified Theories, La Thuile, Italy, March 5-12, 2005.

[11-16]

Measurement of the SAGE Response to Neutrinos from Ar37 Source, Gavrin, V.N. (SAGE), 2005. XI International Workshop on Neutrino Telescopes, February 22-25, 2005, Venice, Italy. http://www.pd.infn.it/~laveder/unbound/talks/exp/sage/VE05-Gavrin.pdf.
Comment: The ratio of the production rate (measured/predicted) is .

[11-17]

Sudbury Neutrino Observatory Results, A.B. McDonald et al. (SNO), Phys. Scripta T121 (2005) 29, arXiv:hep-ex/0412060. Nobel Symposium 129, August 19-24, 2004, Enkoping, Sweden.

[11-18]

Super Kamiokande results: atmospheric and solar neutrinos, M.Ishitsuka (Super-Kamiokande), arXiv:hep-ex/0406076, 2004. XXXIX Rencontres de Moriond, Electroweak Interactions and Unified Theories, La Thuile, March 21-28-2004. http://moriond.in2p3.fr/EW/2004/transparencies/3_Wednesday/3_2_afternoon/3_2_3_Ishitsuka/Ishitsuka.pdf.

[11-19]

High Sensitivity Anti-Neutrino Detection by KamLAND, S. Hatakeyama et al. (KamLAND), arXiv:hep-ex/0405001, 2004. Moriond EW04.

[11-20]

Search for neutrino radiative decays during a total solar eclipse, V. Popa, arXiv:hep-ex/0402014, 2004. AHEP2003, Valencia.

[15-2]

KamLAND: updated results, Inoue, K., 2004. Neutrino Oscillation Workshop NOW 2004, September 11-17, 2004, Conca Specchiulla (Otranto, Italy). http://www.ba.infn.it/~now2004/talks/12_09_04/plen/KamLAND.pdf.

[11-22]

SuperKamiokande's solar neutrino results, M. Nakahata (Super-Kamiokande), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/nakahata.pdf.

[11-23]

Results from radiochemical solar neutrino experiments, C. Cattadori, 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/cattadori.ppt.

[11-24]

The Sudbury Neutrino Observatory, J. Wilkerson (SNO), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/wilkerson.pdf.

[11-25]

Recent Results from the Sudbury Neutrino Observatory, A. W. P. Poon (SNO), Eur. Phys. J. C33 (2004) S823, arXiv:hep-ex/0312002. International Europhysics Conference on High Energy Physics (EPS2003).

[11-26]

Recent Results from KamLAND, J. Detwiler (KamLAND), eConf C0307282 (2003) TW04, arXiv:hep-ex/0311007. SLAC Summer Institute, July 2003.

[11-27]

The Solar Neutrino Day/Night Effect in Super-Kamiokande, M. B. Smy (Super-Kamiokande), Nucl. Phys. Proc. Suppl. 138 (2005) 91, arXiv:hep-ex/0310064. TAUP 2003.

[11-28]

Latest News from SNO, K. Graham (SNO), eConf C030626 (2003) THAT02, arXiv:hep-ex/0310039. XXIII Physics in Collisions Conference (PIC03), Zeuthen, Germany, June 2003.

[11-29]

A study of short-time periodic variation of the B8 solar neutrino flux at Super-Kamiokande, J. Yoo (Super-Kamiokande), eConf C030626 (2003) FRAP01, arXiv:hep-ex/0309048. XXIII Physics in Collisions Conference (PIC03), Zeuthen, Germany, June 2003.

[11-30]

KamLAND results, Inoue, K. (Kamland), arXiv:hep-ex/0307030, 2003. XXXVIIIth Recontres de Moriond Electroweak Interactions and Unified Theories.

[11-31]

The recent results of solar neutrino measurements in Super-Kamiokande, Y. Koshio (Super-Kamiokande), arXiv:hep-ex/0306002, 2003. XXXVIIIth Recontres de Moriond Electroweak Interactions and Unified Theories.

[11-32]

Results from SNO and Other Solar Neutrino Experiments, Robertson, R., 2003. TAUP 2003, September 5-9, 2003 University of Washington, Seattle, Washington. http://mocha.phys.washington.edu/~int_talk/WorkShops/TAUP03/Plenary/People/Robertson_H/SNO_and_Others-Robertson.pdf.

[11-33]

The Gallium Neutrino Observatory (GNO), Bellotti, E. (GNO), 2003. TAUP 2003, September 5-9, 2003 University of Washington, Seattle, Washington. http://mocha.phys.washington.edu/~int_talk/WorkShops/TAUP03/Parallel/People/Bellotti_E/GNO-Bellotti.pdf.

[15-4]

KamLAND Results, Inoue, K. (Kamland), 2003. The 4th Workshop on Neutrino Oscillations and their Origin (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Inoue-KamLAND.pdf.

[11-35]

Solar Neutrino Observations at the Sudbury Neutrino Observatory, Poon, A. W. P. (SNO), eConf C020805 (2002) TTH01, arXiv:hep-ex/0211013. SLAC Summer Institute Topical Conference (SSI02-TTh01), 2002.

[11-36]

Solar Neutrinos, McDonald, A. B., eConf C020620 (2002) SAAT02, arXiv:hep-ex/0209056. Physics in Collision Conference, Stanford, California, June, 2002.

[11-37]

Solar Neutrino Precision Measurements using all 1496 Days of Super-Kamiokande-I Data, Smy, M. B. (Super-Kamiokande), Nucl. Phys. Proc. Suppl. 118 (2003) 25, arXiv:hep-ex/0208004. XXth International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/smy.

[11-38]

Five Years of Neutrino Physics with Super-Kamiokande, M. B. Smy (Super-Kamiokande), arXiv:hep-ex/0206016, 2002. XXXVII Rencontres de Moriond: Electroweak Interactions and Unified Theories.

[11-39]

An update on progress at KamLAND, Dazeley, S. A. (KamLAND), arXiv:hep-ex/0205041, 2002.

[15-5]

First Results from KamLAND: Evidence for disappearance, Gratta, G. (Kamland), 2002. SLAC Colloquium, December 2002. http://hep.stanford.edu/neutrino/KamLAND/TalksAndPublications/KamLAND_FirstResults_SLAC_Colloq.pdf.

[15-6]

KamLAND: Examination of the LMA solution with reactor neutrinos, Suzuki, A. (Kamland), 2002. XVI International Conference on Particles and Nuclei, Osaka, Japan, September 30 - October 4, 2002. http://www.rcnp.osaka-u.ac.jp/Divisions/np2/PaNic02/Suzuki.pdf.

[11-42]

The Sudbury Neutrino Observatory, Hallin, A. (SNO), 2002. XXth International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/hailin.

[12-1]

SNO : Low Energy Treshold Analysis (LETA), Orebi Gann, A., 2009. 5th International Workshop on Low energy neutrino physics, 19-21 October 2009, Reims, France. http://neutrino-champagne.in2p3.fr/Talks/LowNu_OrebiGann_noanim.pdf.

[13-1]

Precision Measurement of Neutrino Oscillation Parameters with KamLAND, Abe, S. et al. (KamLAND), Phys. Rev. Lett. 100 (2008) 221803, arXiv:0801.4589.
From the abstract: Combining with solar neutrino data, we obtain and .
From the article: The spectrum indicates almost two cycles of the periodic feature expected from neutrino oscillation.

[13-2]

Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion, T. Araki et al. (KamLAND), Phys. Rev. Lett. 94 (2005) 081801, arXiv:hep-ex/0406035.
From the article: See this summary.

[13-3]

A High Sensitivity Search for 's from the Sun and Other Sources at KamLAND, K. Eguchi et al. (KamLAND), Phys. Rev. Lett. 92 (2004) 071301, arXiv:hep-ex/0310047.
From the abstract: Data corresponding to a KamLAND detector exposure of 0.28 kton-year has been used to search for 's in the energy range . No candidates were found for an expected background of events. This result can be used to obtain a limit on fluxes of any origin. Assuming that all flux has its origin in the Sun and has the characteristic solar energy spectrum, we obtain an upper limit of (90% C.L.) on the flux. We interpret this limit, corresponding to of the Standard Solar Model flux, in the framework of spin-flavor precession and neutrino decay models.

[15-3]

Results from the KamLAND experiment, G. Gratta (KamLAND), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/gratta.pdf.
Comment: See Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion.

[15-1]

KamLAND (Anti-Neutrino Status), I. Shimizu (KamLAND), 2007. TAUP 2007, 11-15 September 2007, Sendai, Japan. http://www.awa.tohoku.ac.jp/taup2007/slides/workshop14/roomA/02-KamLAND-AntiNeutrino-Status-Shimizu.pdf.

[15-2]

KamLAND: updated results, Inoue, K. (KamLAND), 2004. Neutrino Oscillation Workshop NOW 2004, September 11-17, 2004, Conca Specchiulla (Otranto, Italy). http://www.ba.infn.it/~now2004/talks/12_09_04/plen/KamLAND.pdf.

[15-3]

Results from the KamLAND experiment, G. Gratta (KamLAND), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/gratta.pdf.
Comment: See Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion.

[15-4]

KamLAND Results, Inoue, K. (KamLAND), 2003. The 4th Workshop on Neutrino Oscillations and their Origin (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Inoue-KamLAND.pdf.

[15-5]

First Results from KamLAND: Evidence for disappearance, Gratta, G. (Kamland), 2002. SLAC Colloquium, December 2002. http://hep.stanford.edu/neutrino/KamLAND/TalksAndPublications/KamLAND_FirstResults_SLAC_Colloq.pdf.

[15-6]

KamLAND: Examination of the LMA solution with reactor neutrinos, Suzuki, A. (Kamland), 2002. XVI International Conference on Particles and Nuclei, Osaka, Japan, September 30 - October 4, 2002. http://www.rcnp.osaka-u.ac.jp/Divisions/np2/PaNic02/Suzuki.pdf.

[16-1]

LUNA: Nuclear Astrophysics Deep Underground, Carlo Broggini, Daniel Bemmerer, Alessandra Guglielmetti, Roberto Menegazzo, Ann. Rev. Nucl. Part. Sci. 60 (2010) 53-73, arXiv:1010.4165.

[16-2]

The 3He(alpha,gamma)7Be S-factor at solar energies: the prompt gamma experiment at LUNA, Costantini, H. et al., Nucl. Phys. A814 (2008) 144-158, arXiv:0809.5269.

[16-3]

The 3He + 4He -> 7Be Astrophysical S-factor, T. A. D. Brown et al., Phys. Rev. C76 (2007) 055801, arXiv:0710.1279.

[16-4]

3He(alpha,gamma)7Be cross section at low energies, Gy. Gyurky et al., Phys. Rev. C75 (2007) 035805, arXiv:nucl-ex/0702003.

[16-5]

S-factor of 14N(p,gamma)15O at astrophysical energies, Imbriani, G. et al. (LUNA), Eur. Phys. J. A25 (2005) 455, arXiv:nucl-ex/0509005.

[16-6]

Astrophysical S-factor of 14N(p,g)15O, A. Formicola et al. (LUNA), Phys. Lett. B591 (2004) 61, arXiv:nucl-ex/0312015.

[16-7]

Precise measurement of the S-factor, Junghans, A. R. et al., Phys. Rev. C68 (2003) 065803, arXiv:nucl-ex/0308003.

[22-49]

Precise measurement of cross section of 3He(3He,2p)4He by using He-3 doubly charged beam, Nobuyuki Kudomi et al., Phys. Rev. C69 (2004) 015802, arXiv:astro-ph/0306454.

[22-62]

Indirect measurements of the solar neutrino production reaction , Motobayashi, T., Nucl. Phys. A693 (2001) 258-268.

[22-63]

The solar neutrino problem: Low energy measurements of the cross section, Hammache, F. et al., Nucl. Phys. A688 (2001) 273-276.

[22-64]

Precision measurements of the reaction with radioactive beams and the solar neutrino flux, Gai, Moshe, Prog. Part. Nucl. Phys. 46 (2001) 89-96, arXiv:nucl-ex/0010014.

[22-69]

First Measurement of the He3+He3->He4+2p Cross Section down to the Lower Edge of the Solar Gamow Peak, Bonetti, R. et al. (LUNA), Phys. Rev. Lett. 82 (1999) 5205-5208, arXiv:nucl-ex/9902004.

[17-1]

Study of the Production of Radioactive Isotopes through Cosmic Muon Spallation in KamLAND, Abe, S. et al. (KamLAND), Phys. Rev. C81 (2010) 025807, arXiv:0907.0066.

[18-1]

Solar Neutron Events of October-November 2003, K. Watanabe et al., Astrophys. J. 636 (2006) 1135, arXiv:astro-ph/0509527.

[19-1]

Solar models with accretion. I. Application to the solar abundance problem, Aldo M. Serenelli, Wick C. Haxton, Carlos Pena-Garay, Astrophys. J. 743 (2011) 24, arXiv:1104.1639.

[19-2]

Seismic and dynamical solar models i-the impact of the solar rotation history on neutrinos and seismic indicators, Sylvaine Turck-Chieze, Ana Palacios, Joao Marques, P. Nghiem, Astrophys. J. 715 (2010) 1539-1555, arXiv:1004.1657.

[19-3]

New Solar Composition: The Problem With Solar Models Revisited, Aldo Serenelli, Sarbani Basu, Jason W. Ferguson, Martin Asplund, Astrophys. J. 705 (2009) L123-L127, arXiv:0909.2668.

[19-4]

Solar neutrinos and the solar composition problem, Pena-Garay, Carlos, Serenelli, Aldo, arXiv:0811.2424, 2008.

[19-5]

10,000 Standard Solar Models: a Monte Carlo Simulation, John N. Bahcall, Aldo M. Serenelli, Sarbani Basu, Astrophys. J. Supp. Ser. 165 (2006) 400-431, arXiv:astro-ph/0511337.

[19-6]

What Is The Neon Abundance Of The Sun?, Bahcall, John N., Basu, Sarbani, Serenelli, Aldo M., Astrophys. J. 631 (2005) 1281, arXiv:astro-ph/0502563.
From the abstract: We have evolved a series of thirteen complete solar models that utilize different assumed heavy element compositions.... The predicted solar neutrino fluxes are affected by the uncertainties in the composition by less than their theoretical uncertainties.

[19-7]

New solar opacities, abundances, helioseismology, and neutrino fluxes, Bahcall, John N., Serenelli, Aldo M., Basu, Sarbani, Astrophys. J. 621 (2005) L85-L88, arXiv:astro-ph/0412440.
From the abstract: We construct solar models with the newly calculated radiative opacities from the Opacity Project (OP) and recently determined (lower) heavy element abundances. ... For all the variations we consider, solar models that are constructed with the newer and lower heavy element abundances advocated by Asplund and others (2005) disagree by much more than the estimated measuring errors with helioseismological determinations of the depth of the solar convective zone, the surface helium composition, the internal sound speeds, and the density profile. Using the new OP radiative opacities, the ratio of the B neutrino flux calculated with the older and larger heavy element abundances (or with the newer and lower heavy element abundances) to the total neutrino flux measured by the Sudbury Neutrino Observatory is 1.09 (0.87) with a 9% experimental uncertainty and a 16% theoretical uncertainty, errors.
Comment: BS05.

[19-8]

How do Uncertainties in the Surface Chemical Abundances of the Sun Affect the Predicted Solar Neutrino Fluxes?, John N. Bahcall, Aldo M. Serenelli, Astrophys. J. 626 (2005) 530, arXiv:astro-ph/0412096.

[19-9]

Surprising Sun, S. Turck-Chieze et al., Phys. Rev. Lett. 93 (2004) 211102, arXiv:astro-ph/0407176.

[19-10]

What do we (not) know theoretically about solar neutrino fluxes?, Bahcall, John N., Pinsonneault, M. H., Phys. Rev. Lett. 92 (2004) 121301, arXiv:astro-ph/0402114.
From the abstract: Solar model predictions of and neutrinos agree with the experimentally-determined fluxes (including oscillations): , and , experimental and theoretical uncertainties, respectively.
From the article: The 15% increase in the calculated neutrino flux is the only significant change in the best-estimate fluxes.
Comment: BP04.

[19-11]

Solar seismic models and the neutrino predictions, Couvidat, S., Turck-Chieze, Sylvaine, Kosovichev, A.G., Astrophys.J. 599 (2003) 1434-1448.

[19-12]

Our Sun. IV. The Standard Model and Helioseismology: Consequences of Uncertainties in Input Physics and in Observed Solar Parameters, Arnold I. Boothroyd, I.-Juliana Sackmann, Astrophys. J. 583 (2003) 1004, arXiv:astro-ph/0210127.

[19-13]

New solar seismic models and the neutrino puzzle, Couvidat, S., Turck-Chieze, S., Kosovichev, A. G., arXiv:astro-ph/0203107, 2002.

[19-14]

Solar models: Current epoch and time dependences, neutrinos, and helioseismological properties, Bahcall, J. N., Pinsonneault, M. H., Basu, S., Astrophys. J. 555 (2001) 990-1012, arXiv:astro-ph/0010346.
Comment: BP00.

[19-15]

How uncertain are solar neutrino predictions?, Bahcall, J. N., Basu, S., Pinsonneault, M. H., Phys. Lett. B433 (1998) 1-8, arXiv:astro-ph/9805135.
Comment: BP98.

[26-13]

Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates, Bahcall, John N., Phys. Rev. C56 (1997) 3391, arXiv:hep-ph/9710491.

[19-17]

Are standard solar models reliable?, Bahcall, J. N., Pinsonneault, M. H., Basu, S., Christensen-Dalsgaard, J., Phys. Rev. Lett. 78 (1997) 171-174, arXiv:astro-ph/9610250.

[19-18]

Neutrino Energy Loss in Stellar Interiors. VII. Pair, Photo-, Plasma, Bremsstrahlung, and Recombination Neutrino Processes, Itoh, N., Hayashi, H., Nishikawa, A., Kohyama, Y., Astrophysical Journal Supplement 102 (1996) 411-424.

[19-19]

Solar models with helium and heavy element diffusion, Bahcall, J. N., Pinsonneault, M. H., Rev. Mod. Phys. 67 (1995) 781-808, arXiv:hep-ph/9505425.
Comment: BP95.

[19-20]

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[19-21]

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From the abstract: ... we take a weighted average of the results of four direct and three indirect measurements to obtain a recommended value for of (95% confidence level).
From the article: If this value were adopted in solar models, the reaction rate would no longer represent the dominant uncertainty in the theoretical prediction of the high-energy solar neutrino flux.
Comment: In the BP2000 SSM [19-14] (see [41-1]), taken from [6-8].

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Solar Neutrino Constraints on the BBN Production of Li, Cyburt, Richard H., Fields, Brian D., Olive, Keith A., Phys. Rev. D69 (2004) 123519, arXiv:astro-ph/0312629.

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Neutrino flux variations and solar activity, R.N. Ikhsanov, E.V. Miletsky, arXiv:astro-ph/0312581, 2003.

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Neutrino oscillations, fluctuations and solar magneto- gravity waves, Dzhalilov, C. P. Burgess N. S. et al., arXiv:hep-ph/0312345, 2003.

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Detecting Solar Neutrino Flares and Flavors, D. Fargion, JHEP 0406 (2004) 045, arXiv:hep-ph/0312011.

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The effect of very low energy solar neutrinos on the MSW mechanism, S. Esposito, Mod. Phys. Lett. A19 (2004) 2611, arXiv:hep-ph/0311093.

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Three-neutrino model analysis of the world's oscillation data, D. C. Latimer, D. J. Ernst, arXiv:nucl-th/0310083, 2003.
Comment: Another junk paper in which it is claimed that solar, atmospheric and LSND data can be fitted in a three-neutrino model.
Important data (energy spectra) are omitted and the analysis is very approximate.
The claimed best-fit values of the largest are either or .
The smaller value give in LSND. Therefore, this case is equivalent to neglect LSND.
The larger values obviously cannot fit the energy spectra of atmospheric neutrinos, which have been omitted in the analysis.
[C.G.].

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Solar neutrinos: the SNO salt phase results and physics of conversion, P. C. de Holanda, A. Yu. Smirnov, Astropart. Phys. 21 (2004) 287, arXiv:hep-ph/0309299.

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On the Measurement of Solar Neutrino Oscillation Parameters with KamLAND, Abhijit Bandyopadhyay, Sandhya Choubey, Srubabati Goswami, S.T. Petcov, Phys. Lett. B581 (2004) 62, arXiv:hep-ph/0309236.

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Three-Neutrino Mixing after the First Results from K2K and KamLAND, M. C. Gonzalez-Garcia, Carlos Pena-Garay, Phys. Rev. D68 (2003) 093003, arXiv:hep-ph/0306001.

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Further Evidence for Neutrino Flux Variability from Super- Kamiokande Data, Caldwell, D. O., Sturrock, P. A., arXiv:hep-ph/0305303, 2003.

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Global analyses as a road map to solar neutrino fluxes and oscillation parameters, Bahcall, John N., Pena-Garay, Carlos, JHEP 0311 (2003) 004, arXiv:hep-ph/0305159.
From the abstract: Existing experiments show that the solar neutrino flux is times the flux predicted by the BP00 standard solar model; the Be neutrino flux is the predicted flux; and the B flux is the predicted flux. The oscillation parameters are: and .
...
A future Be scattering experiment accurate to % can reduce the uncertainty in the experimentally determined Be neutrino flux by a factor of four and the uncertainty in the neutrino flux by a factor of 2.5 (to %). A future experiment must be accurate to better than % to shrink the uncertainty in by more than 15%.
Comment: Figure 4 shows the allowed regions for oscillation of solar neutrinos before and after the presentation of new data at TAUP03 conference [M.L.].

[29-169]

A new model of solar neutrinos in manifest violation of CPT invariance, Raghavan, R. S., JCAP 0308 (2003) 002, arXiv:astro-ph/0304331.

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KamLAND, solar antineutrinos and the solar magnetic field, Chauhan, Bhag C., Pulido, Joao, Torrente-Lujan, E., Phys. Rev. D68 (2003) 033015, arXiv:hep-ph/0304297.

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Joint Time-Series Analysis of Homestake and GALLEX-GNO Solar Neutrino Data: Evidence for Rieger-Type Periodicities and their Interpretation as R-Mode Oscillations, P. A. Sturrock, arXiv:hep-ph/0304106, 2003.

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Time-Series Analysis of Super-Kamiokande Measurements of the Solar Neutrino Flux, P.A. Sturrock, Astrophys. J. 594 (2003) 1102, arXiv:hep-ph/0304073.

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Do the KamLAND and Solar Neutrino Data Rule out Solar Density Fluctuations?, Balantekin, A. B., Yuksel, H., Phys. Rev. D68 (2003) 013006, arXiv:hep-ph/0303169.

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A Search for Periodicity in the Super-Kamiokande Solar Neutrino Flux Data, A. Milsztajn, arXiv:hep-ph/0301252, 2003.

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Does the Sun Shine by pp or CNO Fusion Reactions?, J. N. Bahcall, M. C. Gonzalez-Garcia, C. Penya-Garay, Phys. Rev. Lett. 90 (2003) 131301, arXiv:astro-ph/0212331.

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Determining the oscillation parameters by Solar neutrinos and KamLAND, H. Nunokawa, W. J. C. Teves, R. Zukanovich Funchal, Phys. Lett. B562 (2003) 28, arXiv:hep-ph/0212202.

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Implications on neutrino oscillation plus decay from recent solar neutrino data, Indumathi, D., arXiv:hep-ph/0212038, 2002.

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Critical review of the results of the Homestake solar neutrino experiment, Cattaneo, Paolo Walter, arXiv:astro-ph/0211534, 2002.
Comment: The data are reanalyzed and a new ratio has been found. (M.L.).

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Solar neutrino oscillations and indications of matter effects in the Sun, G.L. Fogli, E. Lisi, A. Palazzo, A.M. Rotunno, Phys. Rev. D67 (2003) 073001, arXiv:hep-ph/0211414.

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Analysis of solar neutrino problem by means of Notzold and Nakagawa's approach including the interference term- Hyperbolic-tangent profile for electron density in the sun and exact solution -, Masahiro Kaneyama, Minoru Biyajima, arXiv:hep-ph/0211273, 2002.

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Testing the solar LMA region with KamLAND data, Abhijit Bandyopadhyay et al., J. Phys. G29 (2003) 2465, arXiv:hep-ph/0211266.

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Searches for sterile component with solar neutrinos and KamLAND, P. C. de Holanda, A. Yu. Smirnov, arXiv:hep-ph/0211264, 2002.

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Active neutrino Oscillations and the SNO neutral Current measurement, A. Aguilar-Arevalo, J.C. Dolivo, Phys. Rev. D66 (2002) 113009, arXiv:hep-ph/0211091.

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Constraining Majorana neutrino electromagnetic properties from the LMA-MSW solution of the solar neutrino problem, Grimus, W., Maltoni, M., Schwetz, T., Tortola, M. A., Valle, J. W. F., Nucl. Phys. B648 (2003) 376-396, arXiv:hep-ph/0208132.

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KamLAND, solar antineutrinos and their magnetic moment, Aliani, P., Antonelli, V., Picariello, M., Torrente-Lujan, E., JHEP 02 (2003) 025, arXiv:hep-ph/0208089.

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KamLAND potentiality on the determination of Neutrino mixing parameters in the post SNO-NC era, Aliani, P., Antonelli, V., Picariello, M., Torrente-Lujan, E., New J. Phys. 5 (2003) 2, arXiv:hep-ph/0207348.

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Confronting Spin Flavor Solutions of the Solar Neutrino Problem with current and future solar neutrino data, Barranco, J., Miranda, O. G., Rashba, T. I., Semikoz, V. B., Valle, J. W. F., Phys. Rev. D66 (2002) 093009, arXiv:hep-ph/0207326.

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Ruling out four-neutrino oscillation interpretations of the LSND anomaly?, Maltoni, M., Schwetz, T., Tortola, M. A., Valle, J. W. F., Nucl. Phys. B643 (2002) 321-338, arXiv:hep-ph/0207157.
From the abstract: ... all four-neutrino descriptions of the LSND anomaly, both in (2+2) as well as (3+1) realizations, are highly disfavoured. Our analysis brings the LSND hint to a more puzzling status.
From the article: The exclusion of four-neutrino oscillation schemes of the (2+2)-type is based on the improved sensitivity of solar and atmospheric neutrino experiments to oscillations into a sterile neutrino, thanks to recent experimental data. This is a very robust result, independent of whether the LSND experiment is confirmed or disproved. The exclusion of (3+1) schemes depends somehow on the used LSND data. Furthermore, it heavily relies on the results of negative SBL experiments, especially on the Bugey and CDHS disappearance experiments.

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Does Solar Physics Provide Constraints to Weakly Interacting Massive Particles?, Bottino, A. et al., Phys. Rev. D66 (2002) 053005, arXiv:hep-ph/0206211.

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Resonance spin flavour precession of solar neutrinos after SNO NC data, Chauhan, Bhag C., Pulido, Joao, Phys. Rev. D66 (2002) 053006, arXiv:hep-ph/0206193.

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Getting the most from the statistical analysis of solar neutrino oscillations, Fogli, G. L., Lisi, E., Marrone, A., Montanino, D., Palazzo, A., Phys. Rev. D66 (2002) 053010, arXiv:hep-ph/0206162.

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Constraints on two-body axial currents from reactor antineutrino deuteron breakup reactions, Butler, Malcolm, Chen, Jiunn-Wei, Vogel, Petr, Phys. Lett. B549 (2002) 26-31, arXiv:nucl-th/0206026.

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Which solar neutrino data favour the LMA solution?, Strumia, Alessandro, Cattadori, Carla, Ferrari, Nicola, Vissani, Francesco, Phys. Lett. B541 (2002) 327-331, arXiv:hep-ph/0205261.

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Solar neutrinos: Global analysis with day and night spectra from SNO, de Holanda, P. C., Smirnov, A. Yu., Phys. Rev. D66 (2002) 113005, arXiv:hep-ph/0205241.

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Determination of neutrino mixing parameters after SNO oscillation evidence, Aliani, P., Antonelli, V., Ferrari, R., Picariello, M., Torrente-Lujan, E., Phys. Rev. D67 (2003) 013006, arXiv:hep-ph/0205053.

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The SNO solar neutrino data, neutrinoless double-beta decay and neutrino mass spectrum, Pascoli, S., Petcov, S. T., Phys. Lett. B544 (2002) 239-250, arXiv:hep-ph/0205022.

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Before and after: How has the SNO neutral current measurement changed things?, Bahcall, J. N., Gonzalez-Garcia, M. C., Pena-Garay, Carlos, JHEP 07 (2002) 054, arXiv:hep-ph/0204314.

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Bounds on neutrino magnetic moment tensor from solar neutrinos, Joshipura, Anjan S., Mohanty, Subhendra, Phys. Rev. D66 (2002) 012003, arXiv:hep-ph/0204305.

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Implications of the first neutral current data from SNO for solar neutrino oscillation, Bandyopadhyay, Abhijit, Choubey, Sandhya, Goswami, Srubabati, Roy, D. P., Phys. Lett. B540 (2002) 14-19, arXiv:hep-ph/0204286.

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Imprint of SNO neutral current data on the solar neutrino problem, Barger, V., Marfatia, D., Whisnant, K., Wood, B. P., Phys. Lett. B537 (2002) 179-186, arXiv:hep-ph/0204253.
From the article: Since in SNO the measured NC flux is consistent with the Solar Standard Model Prediction one obtains .

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If sterile neutrinos exist, how can one determine the total B-8 and Be-7 solar neutrino fluxes?, Bahcall, J. N., Gonzalez-Garcia, M. C., Pena-Garay, C., Phys. Rev. C66 (2002) 035802, arXiv:hep-ph/0204194.

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Neutrino decay confronts the SNO data, Abhijit Bandyopadhyay, Sandhya Choubey, Srubabati Goswami, Phys. Lett. B555 (2003) 33, arXiv:hep-ph/0204173.

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Solar Magnetic Fields Profile: A Natural Consequence of RSFP Scenario, B. C. Chauhan, arXiv:hep-ph/0204160, 2002.

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Do solar neutrinos decay?, Beacom, J. F., Bell, N. F., Phys. Rev. D65 (2002) 113009, arXiv:hep-ph/0204111.

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What can the SNO neutral current rate teach us about the solar neutrino anomaly, Bandyopadhyay, Abhijit, Choubey, Sandhya, Goswami, Srubabati, Roy, D. P., Mod. Phys. Lett. A17 (2002) 1455-1464, arXiv:hep-ph/0203169.

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Addendum to: Model-dependent and -independent implications of the first Sudbury Neutrino Observatory results, Fogli, Gian Luigi, Lisi, E., Montanino, D., Palazzo, A., Phys. Rev. D65 (2002) 117301, arXiv:hep-ph/0203138.

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Has Super-Kamiokande observed antineutrinos from the Sun?, Alexander Friedland, Andrei Gruzinov, Astropart. Phys. 19 (2003) 575, arXiv:hep-ph/0202095.

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Distinguishing magnetic moment from oscillation solutions of the solar neutrino problem with Borexino, Akhmedov, E. K., Pulido, Joao, Phys. Lett. B529 (2002) 193-198, arXiv:hep-ph/0201089.

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On the Day-Night Effect and CC to NC Event Rate Ratio Predictions for the SNO Detector, Maris, M., Petcov, S. T., Phys. Lett. B534 (2002) 17-27, arXiv:hep-ph/0201087.

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Seasonal Variations of the Effect from Solar Neutrinos in Lithium Detector, Kopylov, Anatoli, Petukhov, Valeri, Phys. Lett. B544 (2002) 11-15, arXiv:hep-ph/0201042.

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Implications of recent solar neutrino observations: an analysis of charged current data, Baba, C. V. K., Indumathi, D., Murthy, M. V. N., Phys. Rev. D65 (2002) 073033, arXiv:hep-ph/0201031.

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Matter Effects of Thin Layers: Detecting Oil by Oscillations of Solar Neutrinos, Ioannisian, Ara N., Smirnov, Alexei Yu., arXiv:hep-ph/0201012, 2002.

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Solar neutrino zenith angle distribution and uncertainty in earth matter density, Shan, Lian-You, arXiv:hep-ph/0112319, 2001.

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Status of a hybrid three-neutrino interpretation of neutrino data, Guzzo, M. et al., Nucl. Phys. B629 (2002) 479-490, arXiv:hep-ph/0112310.

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Solar Neutrinos with Magnetic Moment: Rates and Global Analysis, Pulido, Joao, Astropart. Phys. 18 (2002) 173-181, arXiv:hep-ph/0112104.

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The LMA MSW solution of the solar neutrino problem, inverted neutrino mass hierarchy and reactor neutrino experiments, Petcov, S. T., Piai, M., Phys. Lett. B533 (2002) 94-106, arXiv:hep-ph/0112074.

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Global analysis of the post-SNO solar neutrino data for standard and non-standard oscillation mechanisms, Gago, A. M. et al., Phys. Rev. D65 (2002) 073012, arXiv:hep-ph/0112060.

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The solar neutrino spectrum derived from electron scattering and charged current interactions, Fiorentini, G., Villante, F. L., arXiv:hep-ph/0111330, 2001.

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Global analysis with SNO: Toward the solution of the solar neutrino problem, Krastev, P. I., Smirnov, A. Yu., Phys. Rev. D65 (2002) 073022, arXiv:hep-ph/0108177.

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Obtaining the large angle MSW solution to the solar neutrino problem in models, Dorsner, Ilja, Barr, Stephen M., Nucl. Phys. B617 (2001) 493-513, arXiv:hep-ph/0108168.

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Exact analysis of the combined data of SNO and Super-Kamiokande, Berezinsky, V., Astropart. Phys. 17 (2002) 509-514, arXiv:hep-ph/0108166.

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How many sigma's is the solar neutrino effect?, Bahcall, J. N., Phys. Rev. C65 (2002) 015802, arXiv:hep-ph/0108147.

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SN1987A and the status of oscillation solutions to the solar neutrino problem, Kachelriess, M., Strumia, A., Tomas, R., Valle, J. W. F., Phys. Rev. D65 (2002) 073016, arXiv:hep-ph/0108100.

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