Borexino

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Borexino neutrino observatory
Laboratori Nazionali del Gran Sasso, Borexino detector.png
Borexino from the North side of LNGS's underground Hall C in September 2015. It is shown close to being completely covered in thermal insulation (seen as a silvery wrapping), providing a relatively cost-effective way to further improve its unprecedented radiopurity levels.
Detector characteristics
Location Laboratori Nazionali del Gran Sasso
Start of data-taking2007
End of data-taking2021
Detection techniqueElastic scattering on liquid scintillator (PC+PPO)
Height16.9 m
Width18 m
Active mass(volume)278 tonnes (315 m3) ≈100 tonnes fiducial

Borexino is a deep underground particle physics experiment to study low energy (sub-MeV) solar neutrinos. The detector is the world's most radio-pure liquid scintillator calorimeter and is protected by 3,800 meters of water-equivalent depth (a volume of overhead rock equivalent in shielding power to that depth of water). The scintillator is pseudocumene and PPO which is held in place by a thin nylon sphere. It is placed within a stainless steel sphere which holds the photomultiplier tubes (PMTs) used as signal detectors and is shielded by a water tank to protect it against external radiation. Outward pointing PMT's look for any outward facing light flashes to tag incoming cosmic muons [1] that manage to penetrate the overburden of the mountain above. Neutrino energy can be determined through the number of photoelectrons measured in the PMT's. While the position can be determined by extrapolating the difference in arrival times of photons at PMT's throughout the chamber. [2]

Contents

The primary aim of the experiment is to make a precise measurement of the individual neutrino fluxes from the Sun and compare them to the Standard solar model predictions. This will allow scientists to test and to further understand the functioning of the Sun (e.g., nuclear fusion processes taking place at the core of the Sun, solar composition, opacity, matter distribution, etc.) and will also help determine properties of neutrino oscillations, including the MSW effect. Specific goals of the experiment are to detect beryllium-7, boron-8, pp, pep and CNO solar neutrinos as well as anti-neutrinos from the Earth and nuclear power plants. The project may also be able to detect neutrinos from supernovae within our galaxy with a special potential to detect the elastic scattering of neutrinos onto protons, due to neutral current interactions. Borexino is a member of the Supernova Early Warning System. [3] Searches for rare processes and potential unknown particles are also underway.

The name Borexino is the Italian diminutive of BOREX (Boron solar neutrino Experiment), after the original 1 kT-fiducial experimental proposal with a different scintillator (TMB), was discontinued because of a shift in focus in physics goals as well as financial constraints. [4] The experiment is located at the Laboratori Nazionali del Gran Sasso near the town of L'Aquila, Italy, and is supported by an international collaboration with researchers from Italy, the United States, Germany, France, Poland, Russia and Ukraine. [5] The experiment is funded by multiple national agencies; the principal ones are INFN (National Institute for Nuclear Physics, Italy) and NSF (National Science Foundation, USA). In May 2017, Borexino reached 10 years of continuous operation since the start of its data-taking period in 2007.

The SOX experiment was a sub-project designed to study the possible existence of sterile neutrinos or other anomalous effects in neutrino oscillations at short ranges through the use of a neutrino generator based on radioactive cerium-144 placed under the water tank of the Borexino detector. This project was cancelled in early 2018 due to the cancellation in 2017 of the contract for cerium-144 by the Russian Mayak fuel reprocessing plant. The cancellation is thought to be connected to the anomalous airborne radioactivity increase in Europe during the autumn of 2017, whose source was eventually localized to the Mayak reprocessing plant.

The entire Borexino experiment was terminated in October 2021. [6]

History and notable results

The gray bands compare the regions where the three solar neutrino telescopes, that are able to measure the energy of the events, are sensitive. Note that the predictions of solar models are in logarithmic scale: Super-Kamiokande and SNO can observe about 0.02% of the total, while Borexino may observe each type of predicted neutrino. SolarSpectraWithExp.jpg
The gray bands compare the regions where the three solar neutrino telescopes, that are able to measure the energy of the events, are sensitive. Note that the predictions of solar models are in logarithmic scale: Super-Kamiokande and SNO can observe about 0.02% of the total, while Borexino may observe each type of predicted neutrino.
Spectrum of the Borexino data used for the simultaneous determination of the pp, pep and Be solar n fluxes, as well as the best available limit on CNO n flux with weak constraints. Solar n components are shown in red; background components in other colors. The lower plot shows the difference between the spectral shape of the data (black curve), and the expected shape when analytically adding together and fitting the signals corresponding to each species. Spectrum2017.png
Spectrum of the Borexino data used for the simultaneous determination of the pp, pep and Be solar ν fluxes, as well as the best available limit on CNO ν flux with weak constraints. Solar ν components are shown in red; background components in other colors. The lower plot shows the difference between the spectral shape of the data (black curve), and the expected shape when analytically adding together and fitting the signals corresponding to each species.

The initial BOREX proposal was made in 1986. [4] In 1990, the design was fundamentally altered, and the name of the experiment was changed to "Borexino". Research and development began on the detector at that time. [4] By 2004, the structure of the detector had been completed, and by May 2007 the detector chamber had been filled and data taking began. [5] [8]

The first results by the collaboration were published in August 2007 in: “First real time detection of 7Be solar neutrinos by Borexino”. [9] [10] The subject was further extended in 2008. [11] In 2010, "geoneutrinos" from Earth's interior were observed for the first time using Borexino. These are anti-neutrinos produced in radioactive decays of uranium, thorium, potassium, and rubidium, although only the anti-neutrinos emitted in the 238U /232Th chains are visible because of the inverse beta decay reaction channel Borexino is sensitive to. [12] [13] That year, the lowest-threshold (3 MeV) measurement of the 8B solar neutrino flux was also published. [14] Additionally, a multi-source detector calibration campaign took place, [15] where several radioactive sources were inserted in the detector to study its response to known signals which are close to the expected ones to be studied. In 2011, the experiment published a precision measurement of the beryllium-7 neutrino flux, [16] [17] as well as the first evidence for the pep solar neutrinos. [18] [19]

The results of measurements of the speed of CERN Neutrinos to Gran Sasso were published in 2012. These results were consistent with the speed of light, [20] thus providing confirmation that the Faster-than-light neutrino anomaly reported earlier in the year was an erroneous measurement. An extensive scintillator purification campaign was also performed, achieving the successful goal of further reducing the residual background radioactivity levels to unprecedented low amounts (up to 15 orders of magnitude under natural background radioactivity levels).

In 2013, Borexino experiments added new limits on sterile neutrino parameters. [21] They also extracted a signal of geoneutrinos, [22] which gives insight into radioactive element activity in the Earth's crust, [23] a hitherto unclear field. [24]

An analysis of the proton–proton fusion activity in the solar core, published in 2014, found that solar activity has been consistently stable on a 105-year scale. [25] [26] Once the phenomenon of neutrino oscillations, as described by MSW theory, is considered, the measurement of Borexino is consistent with the expectations from the standard solar model. This result provided significant data for understanding the functioning of the Sun. Previous experiments sensitive to low energy neutrinos (SAGE, Gallex, GNO) counted neutrinos above a certain energy, but did not measure individual fluxes.

In 2015, an updated spectral analysis of geoneutrinos was presented. [27] Additionally, a Temperature Management and Monitoring System was installed in several phases throughout 2015, [28] consisting of the multi-sensor Latitudinal Temperature Probe System (LTPS), whose testing and first-phase installation occurred in late 2014; and the Thermal Insulation System (TIS) that minimized the thermal influence of the exterior environment on the interior fluids [29] through the extensive insulation of the experiment's external walls. Later in 2015, Borexino also yielded the best available limit to the lifetime of the electron (via e−→γ+ν decay), providing the most stringent confirmation of charge conservation to date. [30]

Detecting Solar Neutrinos

The Sun is a large producer of neutrinos from a variety of different fusion mechanisms like pp and CNO being the two most dominant neutrino production mechanisms and have had extensive research done at Borexino. Due to the property of neutrinos to avoid interactions, it allows them to act as messenger particles, giving insight to the inner workings of nuclear fusion in the Sun's core. In order to detect these solar neutrinos, they must first interact with the free electrons within the liquid scintillator via electron-neutrino elastic scattering (). [1] Although the flux of incident neutrinos is high (), the cross section of interactions is significantly smaller which results in an interaction rate of only several dozen counts per day. [2] Through this interaction, the neutrino deposits some of its energy to the electron, potentially exciting it. When the electron drops down to the ground state, it emits a photon and has some recoil with an associated recoil energy. The recoil of the energy of the electron is a spectrum with a maximum energy given by:

[1]

From conservation of energy, it is possible to resolve the energy of the incident neutrino to then distinguish between pp and CNO neutrinos by analyzing the resulting energy spectrum.

The energy and frequency spectrum of pp-chain neutrinos has a sharp drop off while the CNO neutrino spectrum is very broad. Spectra of solar neutrinos.jpg
The energy and frequency spectrum of pp-chain neutrinos has a sharp drop off while the CNO neutrino spectrum is very broad.

pp neutrinos

The pp production process, in which hydrogen is fused into helium, is the primary source of energy production in the Sun (as well as other stars similar to the Sun that tend to be burn cooler and are smaller in size) as well as the dominant source of neutrinos, specifically electron neutrinos (). The first direct detection of pp neutrinos was done by Borexino throughout the second phase of data collection, spanning from early 2012 to May 2013.

CNO neutrinos

Neutrinos originating from the CNO process are identified from the energy spectrum that is observed, characterized by a very broad energy distribution, ranging from 0 to 1740 keV [2] as seen in the figure on the right. The detection of these particles directly gives insight into the metallicity of the Sun's core, as the CNO neutrino flux is dependent on the abundance of heavier elements (anything heavier than 4He). It is also believed that CNO is the dominant fusion process in stars greater than . [2] In order to confidently identify CNO neutrino counts, it is necessary to muffle the counts from 210Bi (whose decay closely resembles the energy spectrum of CNO neutrinos) by imposing a "muon-positron-neutron three-fold coincidence" condition. [2]

In 2017, Borexino provided the first wideband spectroscopic measurement of the solar ν spectrum, [31] featuring the simultaneous and most precise measurements available of the 7Be, pep and pp neutrino fluxes, furthermore extracted from a single extended energy window (190-2930 keV). These measurements reached a precision of up to 2.7% (in the case of the beryllium solar neutrinos) and established a 5σ confirmation of the presence of pep neutrinos. The limit on the long sought-after CNO neutrinos was kept at the same significance level as in previous Borexino results, which hold the best limit so far, but with weaker assumptions, making the result more robust. Much enlarged statistics thanks to the extra years of exposure, as well as renewed analysis techniques and MonteCarlo state-of-the-art simulations of the whole detector and its physical processes were instrumental in this result. [32] Additionally, an updated observation of 8B neutrinos was published [33] with Phase I and II data (2008-2016), improving precision to around twice that of the previous measurement of this solar component, and hinting at a slight favoring of the high-metallicity SSMs with the available solar neutrino data. An improvement in the sensitivity to the seasonal modulation of the solar neutrino signal [34] was also reported in 2017. That same year, the best direct-observation limit available for the neutrino magnetic moment was established by Borexino too. [35] A neutrino signal related to the GW150914, GW151226 and GW170104 gravitational wave observations was rejected to within Borexino's sensitivity, as expected. [36]

In 2020 Borexino detected the first deep solar core CNO Neutrinos. [37]

Detecting geoneutrinos

It is also possible to study the interior composition of the Earth through detection of geoneutrinos produced by beta decays of radioactive elements present in the crust. Some elements of interest include 238U, 232Th and 40K because of their abundance in rocks and their half-life is comparable to the life of a planet on the scale of billions of years, which leads to heating of the Earth's surface via radiogenic heating.

The spectrum of observed geoneutrinos along with accounted for background sources like muons of cosmic origin or neutrinos produced at nuclear power plants. Total neutrino spectrum.png
The spectrum of observed geoneutrinos along with accounted for background sources like muons of cosmic origin or neutrinos produced at nuclear power plants.
Number of neutrino events detected with special attention drawn to the blue peaks corresponding to the neutrinos originating from the beta decay of Thorium and Uranium. Spectrum U Th.png
Number of neutrino events detected with special attention drawn to the blue peaks corresponding to the neutrinos originating from the beta decay of Thorium and Uranium.

When such elements emit antineutrino particles through beta minus decay, it interacts with atomic protons in the scintillator, which then produces a positron and a neutron (
ν
e+p→e++n). [1] [38] The positron eventually decays into two 0.511 MeV photons. The neutron, the other product from the antineutrino-proton reaction, gets captured by a proton via the neutron-capture process which releases a 2.22 MeV photon because of de-excitation. [38] The PMT's are able to detect these flashes of light and in combination, these two signals appear as a coincidence detection (from positron decay and neutron capture) with some delay between them, making it possible to discriminate against many background signals, such as muon interactions, yielding high resolution data. The Borexino collaboration states that the main source of residual background comes from electron neutrinos produced by European nuclear reactors. [38]

As seen from the neutrino spectrum, the blue peaks represent those antineutrinos that come from the Earth's interior. It is seen that only two peaks appear which correspond to 238U (second small peak) and 232Th (first large peak) and there is no presence of antineutrinos that originate from the beta decay of 40K. This is due to the energy threshold of the Borexino detector which is 1.806 MeV, being too high to trigger detection of those antineutrinos produced by the decay of 40K at 1.32 MeV. [1] [38] From this graph, it is also possible to determine the abundances of each element present in the crust by simply extrapolating how many events occur at which energies. Based on the data in this case, it was possible to determine the flux of antineutrinos from 238U and 232Th as and respectively. [38]

Other background discrimination techniques

To get a spectrum of the various sources of background neutrinos several precautions are taken in the experimental design and data analysis, in addition to utilizing coincidence detection techniques. Firstly, to reduce detection of background altogether, the nylon casing is intended to block background signals from the decay of 222Rn and other products in its decay chain that are present in trace amounts within the experiment's materials left over from the production process. [1] The outgassing of these radioactive isotopes, and their subsequent beta decay, would trigger a false detection of a solar neutrino.

It was observed that temperature fluctuations from seasonal variability and human activity created convection inside the scintillator chamber, which ultimately changed the rate of outgassing of 210Po in an unpredictable manner. To alleviate this, thermal insolation was wrapped around the detector in late 2015 to better maintain a steady internal temperature. [2] Furthermore, in early 2016, a temperature control system was installed underneath the main housing in contact with the rock that would remain at cold temperatures. This would act as a heat sink, removing heat energy in and around the detector, further reducing temperature variability. [2]

SOX project

SOX antineutrino generator planned deployment along rail tracks: from its external dropoff point (lower right), through the calorimetry areas (lower right inside clean room), to its operational position (top center) in the small pit under Borexino SOX deployment concept.png
SOX antineutrino generator planned deployment along rail tracks: from its external dropoff point (lower right), through the calorimetry areas (lower right inside clean room), to its operational position (top center) in the small pit under Borexino

The SOX experiment [39] aimed at the complete confirmation or at a clear disproof of the so-called neutrino anomalies, a set of circumstantial evidences of electron neutrino disappearance observed at LSND, MiniBooNE, with nuclear reactors and with solar neutrino Gallium detectors (GALLEX/GNO, SAGE). If successful, SOX would demonstrate the existence of sterile neutrino components and open a brand new era in fundamental particle physics and cosmology. A solid signal would mean the discovery of the first particles beyond the Standard Electroweak Model and would have profound implications in our understanding of the Universe and of fundamental particle physics. In case of a negative result, it would be able to close a long-standing debate about the reality of the neutrino anomalies, would probe the existence of new physics in low energy neutrino interactions, would provide a measurement of neutrino magnetic moment, Weinberg angle and other basic physical parameters; and would yield a superb energy calibration for Borexino which will be very beneficial for future high-precision solar neutrino measurements.

SOX was envisioned to use a powerful (≈150 kCi) and innovative antineutrino generator made of Ce-144/Pr-144 and possibly a later Cr-51 neutrino generator, which would require a much shorter data-taking campaign. These generators would be located at short distance (8.5 m) from the Borexino detector -under it, in fact: in a pit built ex-profeso before the detector was erected, with the idea it could be used for the insertion of such radioactive sources- and would yield tens of thousands of clean neutrino interactions in the internal volume of the Borexino detector. A high precision (<1% uncertainty) twin-calorimetry campaign would be carried out before deployment in the pit, at the end of data-taking and possibly at some point during the experimental run, in order to provide an independent precise measurement of the source's activity, in order to accomplish a low-uncertainty rate analysis. Shape analyses for the source's antineutrino signal have also been developed in order to increase the experiment's sensitivity, covering the whole high-significance "anomaly" phase space that is still left where light sterile neutrinos could lie in.

SOX cancelled

The experiment was expected to start in the first half of 2018 and take data for about two years. In October 2017, an end-to-end "blank" (without radioactive material) transport test was carried out successfully at the Borexino site in LNGS, [40] in order to clear out final regulatory permissions for the start of the experiment, ahead of the arrival of the source. The cerium oxide (ceria, or CeO2) source for CeSOX's antineutrino generator had to be manufactured by Mayak PA, but technical problems during the fabrication were disclosed in late 2017. These problems meant the generator would not be able to provide the necessary amount of antineutrinos, [41] by a factor of 3, and prompted a review of the project and its eventual starting date. By early February 2018, the CeSOX project was officially cancelled by CEA and INFN due to the radioactive source production problem, [42] and Borexino's 2018-19 goals were reoriented toward achieving higher detector stability and, with it, increased radiopurity, in order to push for higher precision solar neutrino results, with special emphasis on CNO neutrinos.

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References

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  6. ↑ "About".
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  12. ↑ "A first look at the Earth interior from the Gran Sasso underground laboratory". INFN press release. 11 March 2010.
  13. ↑ Borexino Collaboration (2010). "Observation of geo-neutrinos". Physics Letters B. 687 (4–5): 299–304. arXiv: 1003.0284 . Bibcode:2010PhLB..687..299B. doi:10.1016/j.physletb.2010.03.051.
  14. ↑ Borexino Collaboration; Bellini, G.; Benziger, J.; Bonetti, S.; Buizza Avanzini, M.; CaccianigBa, B.; Cadonati, L.; Calaprice, F.; Carraro, C. (2010-08-05). "Measurement of the solar 8B neutrino rate with a liquid scintillator target and 3 MeV energy threshold in the Borexino detector". Physical Review D. 82 (3): 033006. arXiv: 0808.2868 . Bibcode:2010PhRvD..82c3006B. doi:10.1103/PhysRevD.82.033006. S2CID   119258273.
  15. ↑ Back, H.; Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G.; Bravo, D.; Avanzini, M. Buizza; Caccianiga, B.; Cadonati, L. (2012-01-01). "Borexino calibrations: hardware, methods, and results". Journal of Instrumentation. 7 (10): P10018. arXiv: 1207.4816 . doi:10.1088/1748-0221/7/10/P10018. ISSN   1748-0221. S2CID   8924046.
  16. ↑ "Precision measurement of the beryllium solar neutrino flux and its day/night asymmetry, and independent validation of the LMA-MSW oscillation solution using Borexino-only data". Borexino Collaboration press release. 11 April 2011.
  17. ↑ Borexino Collaboration (2011). "Precision Measurement of the 7Be Solar Neutrino Interaction Rate in Borexino". Physical Review Letters. 107 (14): 141302. arXiv: 1104.1816 . Bibcode:2011PhRvL.107n1302B. doi:10.1103/PhysRevLett.107.141302. PMID   22107184. S2CID   34522767.
  18. ↑ "Borexino Collaboration succeeds in spotting pep neutrinos emitted from the sun". PhysOrg.com. 9 February 2012.
  19. ↑ Borexino Collaboration (2012). "First Evidence of pep Solar Neutrinos by Direct Detection in Borexino". Physical Review Letters. 108 (5): 051302. arXiv: 1110.3230 . Bibcode:2012PhRvL.108e1302B. doi:10.1103/PhysRevLett.108.051302. PMID   22400925. S2CID   118444784.
  20. ↑ Borexino collaboration (2012). "Measurement of CNGS muon neutrino speed with Borexino". Physics Letters B. 716 (3–5): 401–405. arXiv: 1207.6860 . Bibcode:2012PhLB..716..401A. doi:10.1016/j.physletb.2012.08.052. hdl:11696/50952.
  21. ↑ Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G.; Bravo, D.; Buizza Avanzini, M.; Caccianiga, B.; Cadonati, L.; Calaprice, F. (2013-10-29). "New limits on heavy sterile neutrino mixing in B 8 decay obtained with the Borexino detector". Physical Review D. 88 (7): 072010. arXiv: 1311.5347 . Bibcode:2013PhRvD..88g2010B. doi:10.1103/physrevd.88.072010. ISSN   1550-7998. S2CID   27175903.
  22. ↑ Borexino Collaboration (15 April 2013). "Measurement of geo-neutrinos from 1353 days of Borexino". Physics Letters B. 722 (4–5): 295–300. arXiv: 1303.2571 . Bibcode:2013PhLB..722..295B. doi:10.1016/j.physletb.2013.04.030. S2CID   55822151.
  23. ↑ "Borexino has new results on geoneutrinos". CERN COURIER. 26 April 2013. Retrieved 20 October 2014.
  24. ↑ Šrámek, Ondřej; Roskovec, Bedřich; Wipperfurth, Scott A.; Xi, Yufei; McDonough, William F. (2016). "Revealing the Earth's mantle from the tallest mountains using the Jinping Neutrino Experiment". Scientific Reports. 6: 33034. Bibcode:2016NatSR...633034S. doi:10.1038/srep33034. PMC   5017162 . PMID   27611737.
  25. ↑ Borexino Collaboration (27 August 2014). "Neutrinos from the primary proton–proton fusion process in the Sun". Nature. 512 (7515): 383–386. Bibcode:2014Natur.512..383B. doi:10.1038/nature13702. PMID   25164748. S2CID   205240340.
  26. ↑ "Borexino measures the Sun's energy in real time". CERN COURIER. 23 September 2014. Retrieved 20 October 2014.
  27. ↑ Borexino Collaboration (7 August 2015). "Spectroscopy of geoneutrinos from 2056 days of Borexino data". Physical Review D. 92 (3): 031101. arXiv: 1506.04610 . Bibcode:2015PhRvD..92c1101A. doi:10.1103/PhysRevD.92.031101. S2CID   55041121.
  28. ↑ Bravo-Berguño, David; Mereu, Riccardo; Cavalcante, Paolo; Carlini, Marco; Ianni, Andrea; Goretti, Augusto; Gabriele, Federico; Wright, Tristan; Yokley, Zachary (2017-05-25). "The Borexino Thermal Monitoring and Management System". arXiv: 1705.09078 [physics.ins-det].
  29. ↑ Bravo-Berguño, David; Mereu, Riccardo; Vogelaar, Robert Bruce; Inzoli, Fabio (2017-05-26). "Fluid-dynamics in the Borexino Neutrino Detector: behavior of a pseudo-stably-stratified, near-equilibrium closed system under asymmetrical, changing boundary conditions". arXiv: 1705.09658 [physics.ins-det].
  30. ↑ Agostini, M.; et al. (Borexino Collaboration) (2015). "Test of Electric Charge Conservation with Borexino". Physical Review Letters . 115 (23): 231802. arXiv: 1509.01223 . Bibcode:2015PhRvL.115w1802A. doi:10.1103/PhysRevLett.115.231802. PMID   26684111. S2CID   206265225.
  31. ↑ Borexino Collaboration; Agostini, M.; Altenmüller, K.; Appel, S.; Atroshchenko, V.; Bagdasarian, Z.; Basilico, D.; Bellini, G.; Benziger, J.; Bonfini, G.; Bravo, D. (2019-10-28). "Simultaneous precision spectroscopy of pp, 7Be, and pep solar neutrinos with Borexino Phase-II". Physical Review D. 100 (8): 082004. arXiv: 1707.09279 . Bibcode:2019PhRvD.100h2004A. doi: 10.1103/PhysRevD.100.082004 .
  32. ↑ Agostini, M.; et al. (2018). "The Monte Carlo simulation of the Borexino detector". Astroparticle Physics. 97: 136–159. arXiv: 1704.02291 . Bibcode:2018APh....97..136A. doi:10.1016/j.astropartphys.2017.10.003.
  33. ↑ The Borexino Collaboration; Agostini, M.; Altenmueller, K.; Appel, S.; Atroshchenko, V.; Bagdasarian, Z.; Basilico, D.; Bellini, G.; Benziger, J. (2020). "Improved measurement of 8B solar neutrinos with 1.5 kt y of Borexino exposure". Physical Review D. 101 (6): 062001. arXiv: 1709.00756 . Bibcode:2020PhRvD.101f2001A. doi:10.1103/PhysRevD.101.062001. S2CID   119348649.
  34. ↑ Agostini, M.; Altenmüller, K.; Appel, S.; Atroshchenko, V.; Basilico, D.; Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G. (2017-06-01). "Seasonal modulation of the 7Be solar neutrino rate in Borexino". Astroparticle Physics. 92 (Supplement C): 21–29. arXiv: 1701.07970 . Bibcode:2017APh....92...21A. doi:10.1016/j.astropartphys.2017.04.004. S2CID   119355273.
  35. ↑ Agostini, M.; et al. (2017). "Limiting neutrino magnetic moments with Borexino Phase-II solar neutrino data". Physical Review D. 96 (9): 091103. arXiv: 1707.09355 . Bibcode:2017PhRvD..96i1103A. doi:10.1103/PhysRevD.96.091103. S2CID   118955967.
  36. ↑ Agostini, M.; et al. (2017). "A Search for Low-energy Neutrinos Correlated with Gravitational Wave Events GW 150914, GW 151226, and GW 170104 with the Borexino Detector". The Astrophysical Journal. 850 (1): 21. arXiv: 1706.10176 . Bibcode:2017ApJ...850...21A. doi: 10.3847/1538-4357/aa9521 . S2CID   119485742.
  37. ↑ Agostini, M.; Altenmüller, K.; Appel, S.; Atroshchenko, V.; Bagdasarian, Z.; Basilico, D.; Bellini, G.; Benziger, J.; Biondi, R.; Bravo, D.; Caccianiga, B. (November 2020). "Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun". Nature. 587 (7835): 577–582. arXiv: 2006.15115 . Bibcode:2020Natur.587..577B. doi:10.1038/s41586-020-2934-0. ISSN   1476-4687. PMID   33239797. S2CID   227174644.
  38. 1 2 3 4 5 Giammarchi, Marco G. (2014-04-01). "Solar and geoneutrino physics with Borexino". Nuclear Instruments and Methods in Physics Research Section A. 742: 250–253. Bibcode:2014NIMPA.742..250G. doi:10.1016/j.nima.2013.11.088. ISSN   0168-9002.
  39. ↑ Caminata, Alessio. "The SOX project". web.ge.infn.it. Archived from the original on 2017-10-19. Retrieved 2016-04-22.
  40. ↑ Galeota, Marco. "Il test di trasporto per l'esperimento SOX". Laboratori Nazionali del Gran Sasso (in Italian). Retrieved 2017-10-25.
  41. ↑ Galeota, Marco. "Nota stampa 12-12-2017". Laboratori Nazionali del Gran Sasso (in Italian). Retrieved 2017-12-13.
  42. ↑ varaschin. "THE SOX PROJECT IS CANCELLED DUE TO THE IMPOSSIBILITY OF REALIZING THE SOURCE WITH THE REQUIRED CHARACTERISTICS". home.infn.it. Archived from the original on 2018-03-09. Retrieved 2018-03-16.

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