First real time detection of 7Be solar neutrinos by Borexino

Arpesella, C.; Bellini, G.; Benziger, J.; Bonetti, S.; Caccianiga, B.; Calaprice, F.; Dalnoki‐Veress, F.; D’Angelo, D.; Kerret, H. de; Derbin, A.; Deutsch, Martin; Etenko, A.; Fomenko, K.; Ford, R.; Franco, D.; Freudiger, B.; Galbiati, C.; Gazzana, S.; Giammarchi, M.; Goeger-Neff, M.; Goretti, A.; Grieb, C.; Hardy, S.; Heusser, G.; Ianni, Aldo; Ianni, Andrea; Joyce, M.; Korga, G.; Kryn, D.; Laubenstein, M.; Leung, M.; Litvinovich, E.; Lombardi, P.; Ludhová, L.; Machulin, I.; Manuzio, G.; Martemianov, A.; Masetti, F.; McCarty, K.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Montanari, D.; Monzani, M. E.; Muratova, V.; Niedermeier, L.; Oberauer, L.; Obolensky, M.; Ortica, F.; Pallavicini, M.; Papp, L.; Perasso, L.; Pocar, A.; Raghavan, R. S.; Ranucci, G.; Razeto, A.; Sabelnikov, A.; Salvo, C.; Schönert, S.; Simgen, H.; Smirnov, O.; Skorokhvatov, M.; Sonnenschein, A.; Sotnikov, A.; Sukhotin, S.; Suvorov, Y.; Tarasenkov, V. G.; Tartaglia, R.; Testera, G.; Vignaud, D.; Vitale, S.; Vogelaar, R. B.; Feilitzsch, F. von; Wójcik, Marcin; Zaimidoroga, O.; Zavatarelli, S.; Zuzel, G.

doi:10.1016/j.physletb.2007.09.054

Cited by 226 publications

(138 citation statements)

References 21 publications

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“…A detailed description of the detector could be found elsewhere [17][18][19][20][21][22][23][24][25][26][27][28][29].…”

Section: Borexino Detectormentioning

confidence: 99%

“…Borexino first detected and then precisely measured the flux of the 7 Be solar neutrinos [20,21,30], has ruled out any significant day-night asymmetry of their interaction rate [26], has measured the 8 B-neutrino rate with 3 MeV threshold [23], has made the first direct observation of pep neutrinos [27], has made the first spectral measurement of pp-neutrinos [28] and has set the best upper limit on the flux of solar neutrinos produced in the CNO cycle [27]. The uniquely low background level of the Borexino detector made it possible to set new limits on the effective magnetic moment of the neutrino [21], on the stability of the electron for decay into a neutrino and a photon [31], on the heavy sterile neutrino mixing in 8 B decay [32], on the possible violation of the Pauli exclusion principle [33], on the flux of high energy solar axions [34], on antineutrinos from the Sun and other unknown sources [35], on Gamma-Ray bursts neutrino and antineutrino fluences [36] and on some other rare processes.…”

Section: Borexino Detectormentioning

confidence: 99%

See 1 more Smart Citation

A Search for Low-energy Neutrinos Correlated with Gravitational Wave Events GW 150914, GW 151226, and GW 170104 with the Borexino Detector

Agostini¹,

Altenmüller²,

Appel³

et al. 2017

ApJ

Self Cite

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We present the results of a low-energy neutrino search using the Borexino detector in coincidence with the gravitational wave (GW) events GW150914, GW151226 and GW170104. We searched for correlated neutrino events with energies greater than 250 keV within a time window of ±500 s centered around the GW detection time. A total of five candidates were found for all three GW150914, GW151226 and GW170104. This is consistent with the number of expected solar neutrino and

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“…A detailed description of the detector could be found elsewhere [17][18][19][20][21][22][23][24][25][26][27][28][29].…”

Section: Borexino Detectormentioning

confidence: 99%

Section: Borexino Detectormentioning

confidence: 99%

A Search for Low-energy Neutrinos Correlated with Gravitational Wave Events GW 150914, GW 151226, and GW 170104 with the Borexino Detector

Agostini¹,

Altenmüller²,

Appel³

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Here the first error is statistical and the second error is systematic (neutrino flux, particle detection efficiency, cross sections, etc.). Despite the evidence for neutrino oscillations from solar neutrinos [70][71][72][73][74][75][76][77], atmospheric neutrinos [78][79][80], accelerator neutrinos [81,82], and reactor neutrinos [83], the oscillation signal observed at LSND remains a puzzle. Since the neutrino sector is thought as likely to reveal new physics, the LSND anomaly is often explained with new ideas such as sterile neutrino models (see Ref.…”

Section: Lsnd Experimentsmentioning

confidence: 99%

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

Katori

2008

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school was successful since I relied 100% on your support. For FINeSSE, you taught me everything step by step because I didn't know anything. For Lorentz violation, even though it was a spin-off subject for me and you, but you were so generous, supportive, and patient.And for MiniBooNE, the CCQE work couldn't have been done without your ideas. I am really proud of the amount of work I present in this thesis; it is the evidence of what a good work relationship we have. Finally I want to apologize for my bad English and for how you always had to correct it, including in this thesis. This acknowledgments section is the only one place in all my writings for which you didn't correct my English! Thank you Rex.My first three years were supported by the people in Indiana.I wish to give sincere appreciation to Chris Cox and Nikodem Pop lawski, I think it was my fate to see you from the very first day in US. I had a hard time (as you know), but because of your help, I not only survived, but also changed my style to be more suitable in this country. No one ever was so influential for me as Chris, I think. And Niko, before Thank you for sharing good times with me. I also want to thank Hans-Otto Mayer, Jack Doskow, and Gerard Visser for your help and inspiration for the work on FINeSSE. Thank you everyone.My friends from the classroom, it is a very strange feeling that now all we are going somewhere to do something, but we have known each other more than six years! Liliana Cabellero, you changed shy Teppei...to an emotional salsa dancer! If the dancing is my mother of energy, then Lily is founding mother of energetic Teppei. Muchas gracias. Leah Welty and Jason Rieger are the first real American students I met. When you described Chicago, I didn't understand very much, but now, yeah, I love this city and want to stay here more. Heechang Na, thank you for talking with me every time I stopped by your office, v because you are so kind and welcome and easy to talk with! Haiyang "Ocean" Yan, I am proud that I nicknamed you. I think you are a very good physicist. Thank you for teaching me a lot about Chinese history and physics. I always enjoyed it. Masaki (& Shizuka) Ishitsuka is the first Japanese fellow I met at Indiana even though I left Bloomington before you came. I always enjoyed talking about neutrinos with you, your view of physics is very unique and interesting to me. Thank you. Yun-Chan, Tony, George, Jay, Helber, Jorge, Shinya... I had so much fun in Indiana because of you. Thank you very much.One of the reasons I wanted to be a physicist is that physicists make friends all over the world so easily. I met many friends at conferences, summer schools, etc. Thank you to everyone who called me a crazy Japanese, even uploading my stupidities on YouTube.

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“…The precision measurement of 7 Be was obtained during the first stage of the experiment [27][28]. Real time detection of the events and detector stability allowed to study the day-night effect of the 7 Be solar neutrino signal, which yielded the exclusion of the LOW solution of the neutrino oscillation based on solar data alone [29].…”

Section: Sub-mev Solar Neutrino Detection With Borexinomentioning

confidence: 99%

Short review on solar neutrinos experiments and search for sterile neutrinos with solar neutrino detectors

Pallavicini

2015

EPJ Web of Conferences

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Abstract. The spectroscopy of solar neutrinos is now entering the precision era, after a golden age which has led to the discovery of neutrino oscillations and the MSW effect. In this paper we summarise the current experimental knowledge in the field and its future perspectives, showing that solar neutrino detectors are and will remain a crucial tool for a deeper understanding of stars, neutrinos, and fundamental physics. We also show that solar neutrinos may become pivotal for the search of sterile neutrinos. Historical introductionThe development of solar neutrino physics in recent years may be divided into two periods. The first, which lasted from the early 70s until 2001, began with the pioneering work of the radiochemical 37 Cl experiment at Homestake (1970-1994, [1]), grew with the study of high energy (E>6 MeV) solar neutrinos by means of the water Cherenkov detectors at Kamioka mine in Japan (KamiokaNDE 1983(KamiokaNDE -1995[3] and Super-KamiokaNDE 1996-present [4]), continued with the detection of low energy neutrinos with gallium radiochemical experiments (Gallex [5], SAGE [6]), and was concluded by the discovery of solar neutrino oscillations by SNO [7][8].The second period started after the convincing discovery of neutrino oscillations and the beginning of the high precision era of solar physics, which has been initiated mainly by the SNO, KamLAND and Borexino experiments and which continues to develop thanks to upgrades and improvements of existing experiments and the design of future detectors.The first period, certainly a golden age for neutrino physics, has witness the first detection of solar neutrinos at different energies, which have proved unambiguously that the Sun's energy has a nuclear origin, the development of a very refined Standard Solar Model (SSM), the recognition of a sharp discrepancy between the model itself and the observed neutrino rates (the so called Solar Neutrino Problem, SNP), and the triumphal discovery of neutrino flavour oscillations as the sole possible explanation of that discrepancy.Although solar neutrino oscillations were, since the very beginning, a possible explanation of the SNP, the favour increased only when a clear evidence of oscillations was found in 1998 by means of atmospheric neutrinos [9].The observed deficit is explained by the fact that most solar neutrino experiments are either insensitive to muon or tau neutrinos, or have a suppressed cross section. The fact that the deficit is energy dependent requires the so called MSW effect [10] the SNO experiment that closed the story. The use of heavy water made the experiment able to measure separately the electron neutrino and the total neutrino flux at Earth, proving without ambiguities that the total neutrino flux at is the same as predicted by the SSM and that the electron neutrino flux is reduced by oscillations. Later measurements with enhanced neutron detection capability, first by dissolving salt in water and later with 3 He detectors, have confirmed the result. The oscillation picture was confirmed s...

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First real time detection of 7Be solar neutrinos by Borexino

Cited by 226 publications

References 21 publications

A Search for Low-energy Neutrinos Correlated with Gravitational Wave Events GW 150914, GW 151226, and GW 170104 with the Borexino Detector

A Search for Low-energy Neutrinos Correlated with Gravitational Wave Events GW 150914, GW 151226, and GW 170104 with the Borexino Detector

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

Short review on solar neutrinos experiments and search for sterile neutrinos with solar neutrino detectors

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