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Journal articles on the topic 'Solar Neutrino Observatory'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Hargrove, C. K., and D. J. Paterson. "Solar-neutrino neutral-current detection methods in the Sudbury neutrino observatory." Canadian Journal of Physics 69, no. 11 (November 1, 1991): 1309–16. http://dx.doi.org/10.1139/p91-196.

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The Sudbury Neutrino Observatory will study the solar-neutrino problem through the detection of charged-current (CC), neutral-current (NC), and elastic-scattering (ES) interactions of solar neutrinos with heavy water. The measurement of the NC rate relative to the CC rate provides a nearly model-independent method of observing neutrino oscillations. The NC interaction breaks up the deuteron producing a neutron and a proton. The interaction rate in the original design is measured by observing Čerenkov light from showers produced by neutron-capture γ rays from the capture of the NC neutrons by a selected additive to the heavy water. These signals overlap the CC and ES signals, so that the measurement of the NC rate requires the subtraction of two signals obtained at different times. This paper describes our investigation of an alternate detection method in which the thermalized neutrons are captured by (n, α) or (n, p) reactions on light nuclei. The resulting charged-particle products are uniquely detected by scintillators or proportional counters, completely separating this NC signal from the CC and ES Čerenkov signals, thus simplifying its measurement, improving its significance, and allowing observation of otherwise unobservable short-term NC fluctuations. Although background rates for the new techniques have not yet been determined, the experimental advantages justify further development work.

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2

KLEIN, JOSHUA R. "SOLAR NEUTRINO RESULTS FROM THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 17, no. 24 (September 30, 2002): 3378–92. http://dx.doi.org/10.1142/s0217751x0201279x.

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We describe here the measurement of the flux of neutrinos created by the decay of solar 8B by the Sudbury Neutrino Observatory (SNO). The neutrinos were detected via the charged current (CC) reaction on deuterium and by the elastic scattering (ES) of electrons. The CC reaction is sensitive exclusively to νe's, while the ES reaction also has a small sensitivity to νμ's and ντ's. The flux of νe's from 8B decay measured by the CC reaction rate is [Formula: see text]. Assuming no flavor transformation, the flux inferred from the ES reaction rate is [Formula: see text]. Comparison of ϕ CC (νe) to the Super-Kamiokande Collaboration's precision value of ϕ ES (νx) yields a 3.3σ difference, assuming the systematic uncertainties are normally distributed, providing evidence that there is non-electron flavor active neutrino component in the solar flux. The total flux of active 8B neutrinos is thus determined to be 5.44 ± 0.99 × 106 cm- 2s- 1, in close agreement with the predictions of solar models.

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3

Miramonti, Lino, Matteo Agostini, Konrad Altenmueller, Simon Appel, Victor Atroshchenko, Zara Bagdasarian, Davide Basilico, et al. "Solar Neutrinos Spectroscopy with Borexino Phase-II." Universe 4, no. 11 (November 7, 2018): 118. http://dx.doi.org/10.3390/universe4110118.

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Solar neutrinos have played a central role in the discovery of the neutrino oscillation mechanism. They still are proving to be a unique tool to help investigate the fusion reactions that power stars and further probe basic neutrino properties. The Borexino neutrino observatory has been operationally acquiring data at Laboratori Nazionali del Gran Sasso in Italy since 2007. Its main goal is the real-time study of low energy neutrinos (solar or originated elsewhere, such as geo-neutrinos). The latest analysis of experimental data, taken during the so-called Borexino Phase-II (2011-present), will be showcased in this talk—yielding new high-precision, simultaneous wide band flux measurements of the four main solar neutrino components belonging to the “pp” fusion chain (pp, pep, 7 Be, 8 B), as well as upper limits on the remaining two solar neutrino fluxes (CNO and hep).

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Gavrin, V. N., A. I. Abazov, D. N. Abdurashitov, O. L. Anosov, O. V. Bychuk, S. N. Danshin, L. A. Eroshkina, et al. "The Baksan Gallium Solar Neutrino Experiment." International Astronomical Union Colloquium 121 (1990): 201–12. http://dx.doi.org/10.1017/s0252921100067956.

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AbstractA radiochemical 71Ga−71 Ge experiment to determine the integral flux of neutrinos from the sun has been constructed at the Baksan Neutrino Observatory in the USSR. Measurements have begun with 30 tonnes of gallium. The experiment is being expanded with the addition of another 30 tonnes. The motivation, experimental procedures, and present status of this experiment are presented.

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5

DUNCAN, F. A. "RESULTS FROM THE PURE D2O PHASE OF THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 18, no. 22 (September 10, 2003): 3789–807. http://dx.doi.org/10.1142/s0217751x0301718x.

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The Sudbury Neutrino Observatory is a 1000 T D2O Cerenkov detector that is sensitive to 8 B and hep solar neutrinos. Both Charged Current and Neutral Current interaction rates on deuterons as well as the Elastic Scattering interaction rate on electrons can be measured simultaneously. Assuming an undistorted 8 B neutrino spectrum, the total flux measured with the NC reaction is [Formula: see text], which is consistent with solar models. The νe component of the 8 B solar flux is [Formula: see text] for a kinetic energy threshold of 5 MeV. The non-νe component is [Formula: see text], which is 5.3σ greater than zero, giving strong evidence for solar νe flavor transformation. The Day-Night Asymmetry for the Charged Current interaction is [Formula: see text]. If the total flux of active neutrinos is additionally constrained to have no asymmetry, the νe asymmetry is found to be [Formula: see text]. Combined with other solar neutrino data, a global MSW oscillation analysis strongly favors the Large Mixing Angle (LMA) solution.

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6

Schever, M. "Status of the Jiangmen Underground Neutrino Observatory." Ukrainian Journal of Physics 64, no. 7 (September 17, 2019): 635. http://dx.doi.org/10.15407/ujpe64.7.635.

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The Jiangmen Underground Neutrino Observatory (JUNO) is a next generation multipurpose antineutrino detector currently under construction in Jiangmen, China. The central detector, containing 20 kton of a liquid scintillator, will be equipped with ∼18 000 20 inch and 25 600 3 inch photomultiplier tubes. Measuring the reactor antineutrinos of two powerplants at a baseline of 53 km with an unprecedented energy resolution of 3%/√︀E(MeV), the main physics goal is to determine the neutrino mass hierarchy within six years of run time with a significance of 3–4q. Additional physics goals are the measurement of solar neutrinos, geoneutrinos, supernova burst neutrinos, the diffuse supernova neutrino background, and the oscillation parameters sin2 O12, Δm212, and |Δm2ee| with a precision <1%, as well as the search for proton decays. The construction is expected to be completed in 2021.

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7

Lawson, I. T. "Solar neutrino results from the sudbury neutrino observatory." Progress in Particle and Nuclear Physics 48, no. 1 (January 2002): 5–20. http://dx.doi.org/10.1016/s0146-6410(02)00103-5.

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8

Lawson, I. "Solar neutrino results from the sudbury neutrino observatory." Nuclear Physics B - Proceedings Supplements 110, no. 2 (July 2002): 308–10. http://dx.doi.org/10.1016/s0920-5632(02)80137-2.

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9

Miramonti, Lino. "Status and the perspectives of the Jiangmen Underground Neutrino Observatory (JUNO)." Modern Physics Letters A 35, no. 09 (March 13, 2020): 2030004. http://dx.doi.org/10.1142/s0217732320300049.

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One of the remaining undetermined fundamental aspects in neutrino physics is the determination of the neutrino mass hierarchy, i.e. discriminating between the two possible orderings of the mass eigenvalues, known as Normal and Inverted Hierarchies. The Jiangmen Underground Neutrino Observatory (JUNO), a 20 kt Liquid Scintillator Detector currently under construction in the South of China, can determine the neutrino mass hierarchy and improve the precision of three oscillation parameters by one order of magnitude. Moreover, thanks to its large liquid scintillator mass, JUNO will also contribute to study neutrinos from non-reactor sources such as solar neutrinos, atmospheric neutrinos, geoneutrinos, supernova burst and diffuse supernova neutrinos. Furthermore, JUNO will also contribute to nucleon decay studies. In this work, I will describe the status and the perspectives of the JUNO experiment.

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10

Rott, Carsten. "Progress in neutrino astronomy." Journal of the Korean Physical Society 78, no. 10 (March 19, 2021): 864–72. http://dx.doi.org/10.1007/s40042-021-00106-1.

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AbstractThe dream of observing our universe through neutrinos is rapidly becoming a reality. More than three decades after the first observation of neutrinos from beyond our solar system associated with Supernova SN1987A, neutrino astronomy is in the midst of a revolution. Extraterrestrial neutrinos are now routinely detected, following the discovery of a high-energy diffuse astrophysical neutrino flux in 2013. The detection of a high-energy neutrino in coincidence with a flaring blazar in 2017 has brought the field rapidly into the multi-messenger science era. The latest developments in the field of neutrino astronomy are reviewed and prospects with current and future detectors discussed. Particular emphasis is put on domestic programs in neutrino astronomy and the possibility to construct a large neutrino observatory in Korea.

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11

Balantekin, A. B., and F. Loreti. "Solar and supernova neutrino physics with Sudbury Neutrino Observatory." Physical Review D 45, no. 4 (February 15, 1992): 1059–65. http://dx.doi.org/10.1103/physrevd.45.1059.

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12

Miramonti, Lino. "Neutrino Physics and Astrophysics with the JUNO Detector." Universe 4, no. 11 (November 16, 2018): 126. http://dx.doi.org/10.3390/universe4110126.

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The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton liquid scintillator multi-purpose underground detector, under construction near the Chinese city of Jiangmen, with data collection expected to start in 2021. The main goal of the experiment is the neutrino mass hierarchy determination, with more than three sigma significance, and the high-precision neutrino oscillation parameter measurements, detecting electron anti-neutrinos emitted from two nearby (baseline of about 53 km) nuclear power plants. Besides, the unprecedented liquid scintillator-type detector performance in target mass, energy resolution, energy calibration precision, and low-energy threshold features a rich physics program for the detection of low-energy astrophysical neutrinos, such as galactic core-collapse supernova neutrinos, solar neutrinos, and geo-neutrinos.

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13

Majumdar, Debasish, and Amitava Raychaudhuri. "Solar neutrino oscillation diagnostics at SuperKamiokande and Sudbury Neutrino Observatory." Pramana 52, no. 5 (May 1999): L529—L536. http://dx.doi.org/10.1007/bf02830099.

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14

Heeger, Karsten M. "Resolving the solar neutrino problem: Evidence for massive neutrinos in the Sudbury Neutrino Observatory." Europhysics News 32, no. 5 (September 2001): 180–83. http://dx.doi.org/10.1051/epn:2001506.

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15

GOLDMAN, T., G. J. STEPHENSON, and B. H. J. McKELLAR. "IMPLICATIONS OF QUARK–LEPTON SYMMETRY FOR NEUTRINO MASSES AND OSCILLATIONS." Modern Physics Letters A 15, no. 06 (February 28, 2000): 439–43. http://dx.doi.org/10.1142/s0217732300000426.

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We identify a plausible scenario based on quark–lepton symmetry which correlates long baseline oscillations with maximal mixing to sterile neutrinos. The implication for the Sudbury Neutrino Observatory (SNO) is that the neutral current signal will be found to suffer the same suppression from the standard solar model prediction as obtains for the charged current signal. Flavor mixing among active neutrinos is expected to occur on shorter baselines with smaller mixing amplitudes.

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16

Diwan, Milind, Rob Edgecock, Takuya Hasegawa, Thomas Patzak, Masato Shiozawa, and Jim Strait. "Future Long-Baseline Neutrino Facilities and Detectors." Advances in High Energy Physics 2013 (2013): 1–35. http://dx.doi.org/10.1155/2013/460123.

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We review the ongoing effort in the US, Japan, and Europe of the scientific community to study the location and the detector performance of the next-generation long-baseline neutrino facility. For many decades, research on the properties of neutrinos and the use of neutrinos to study the fundamental building blocks of matter has unveiled new, unexpected laws of nature. Results of neutrino experiments have triggered a tremendous amount of development in theory: theories beyond the standard model or at least extensions of it and development of the standard solar model and modeling of supernova explosions as well as the development of theories to explain the matter-antimatter asymmetry in the universe. Neutrino physics is one of the most dynamic and exciting fields of research in fundamental particle physics and astrophysics. The next-generation neutrino detector will address two aspects: fundamental properties of the neutrino like mass hierarchy, mixing angles, and the CP phase, and low-energy neutrino astronomy with solar, atmospheric, and supernova neutrinos. Such a new detector naturally allows for major improvements in the search for nucleon decay. A next-generation neutrino observatory needs a huge, megaton scale detector which in turn has to be installed in a new, international underground laboratory, capable of hosting such a huge detector.

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17

McDonald, Arthur B. "The Sudbury Neutrino Observatory: Observation of Flavor Change for Solar Neutrinos." International Journal of Modern Physics A 31, no. 27 (September 30, 2016): 1630048. http://dx.doi.org/10.1142/s0217751x16300489.

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McDonald, Arthur B. "The Sudbury Neutrino Observatory: Observation of flavor change for solar neutrinos." Annalen der Physik 528, no. 6 (March 17, 2016): 469–80. http://dx.doi.org/10.1002/andp.201600031.

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19

Feder, Toni. "Solar Neutrino Observatory Gets New Lease on Life." Physics Today 50, no. 6 (June 1997): 72–73. http://dx.doi.org/10.1063/1.881794.

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20

MAJUMDAR, DEBASISH, AMITAVA RAYCHAUDHURI, KAMALES KAR, ALAK RAY, and FIROZA K. SUTARIA. "OSCILLATION EFFECTS ON NEUTRINOS FROM THE EARLY PHASE OF A NEARBY SUPERNOVA." International Journal of Modern Physics A 15, no. 14 (June 10, 2000): 2105–20. http://dx.doi.org/10.1142/s0217751x00000872.

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Recent observations of atmospheric and solar neutrinos strongly support the phenomenon of neutrino oscillations — a manifestation of a nonzero and nondegenerate mass spectrum. Neutrinos emitted during stellar core collapse leading to a supernova are of the electron neutrino type at source — as for solar and reactor (anti-)neutrinos — and provide another useful tool in the search for flavor oscillations. Their propagation to an earth-bound detector involves length scales that can uniquely probe very small neutrino mass differences hitherto unobservable. Although the number of neutrinos emitted during the collapse phase is much smaller than that emitted in the post-bounce epoch (in which all flavors of neutrinos are emitted), a nearby supernova event may nevertheless register a substantial number of detections from the collapse phase at SuperKamiokande (SK) and the Sudbury Neutrino Observatory (SNO). The measurement of the fluence of these neutrinos at SNO and the distortion of the spectrum detected at SK can yield valuable information about neutrino mass difference and mixing which are illustrated here in terms of two- and three-flavor oscillation models. In particular, we find that R SNO , the ratio of the calorimetric detection of the neutrino fluence via the neutral current channel to the total energy integrated fluence observed via the charged current channel at SNO, is a sensitive probe for oscillations. We also find that αn, the ratio of the nth central moments of the distributions seen at SK and SNO (charged current), can be a useful tool (especially for n=3) to look for neutrino oscillations.

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21

CHEN, JIUNN-WEI. "EFFECTIVE FIELD THEORY IN NUCLEAR ASTROPHYSICS." Modern Physics Letters A 19, no. 13n16 (May 30, 2004): 1215–22. http://dx.doi.org/10.1142/s0217732304014586.

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In this talk I review some general ideas of effective field theory and give examples of high precision calculations which have astrophysical applications. The examples are np→dγ for big-bang nucleosynthesis and νd inelastic scattering relevant for the solar neutrino detection processes employed by the Sudbury Neutrino Observatory.

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22

BOWLES, THOMAS J. "A NATIONAL UNDERGROUND SCIENCE AND ENGINEERING LABORATORY." International Journal of Modern Physics A 18, no. 22 (September 10, 2003): 4129–33. http://dx.doi.org/10.1142/s0217751x03017415.

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Dramatic progress has been made in the last several years in our understanding of the properties of neutrinos with evidence for neutrino flavor transformation coming from measurements of atmospheric neutrinos by SuperKamiokande, of solar neutrinos by the Sudbury Neutrino Observatory (SNO), and of reactor neutrinos by KamLAND. These results are a step in the ongoing program of science that is carried out in underground laboratories. The potential for additional significant discoveries with new capabilities in underground laboratories exists and should be exploited. Discoveries are likely to be made not only in nuclear and particle physics, but also in astrophysics, geophysics, and geobiology. A concerted effort is now underway in the United States to create a National Underground Science and Engineering Laboratory (NUSEL) that would provide the facilities and infrastructure necessary to capitalize on the opportunities presented by underground science.

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23

Kwong, Waikwok, and S. P. Rosen. "Relations between the Sudbury Neutrino Observatory and the Super Kamiokande solar neutrino rates." Physical Review D 54, no. 3 (August 1, 1996): 2043–47. http://dx.doi.org/10.1103/physrevd.54.2043.

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24

KHONDEKAR, MOFAZZAL H., DIPENDRA N. GHOSH, KOUSHIK GHOSH, and ANUP KUMAR BHATTACHARYA. "NONLINEARITY AND CHAOS IN 8B SOLAR NEUTRINO FLUX SIGNALS FROM SUDBURY NEUTRINO OBSERVATORY." Fractals 20, no. 01 (March 2012): 17–32. http://dx.doi.org/10.1142/s0218348x12500028.

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The Sudbury neutrino observatory (SNO) detects 8 B solar neutrino fluxes from both the D2O and Salt detector. In the present analysis we have taken into consideration the flux data from 2nd November, 1999 to 27th May, 2001 from the D2O detector and that from 26th July, 2001 to 28th August, 2003 from the Salt detector. We have applied Delay Vector Variance analysis, 0-1 test, correlation dimension analysis, largest Lyapunov exponent method, recurrence plot and recurrence quantification analysis to explore the complexity and chaosity in these two time series. Present study reveals deterministic chaotic behaviour of these two signals which in turn suggests that long-term forecasting is not possible for these two signals but short-term forecasting can be made provided the model for the process dynamics is known to us.

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Hossain, K. M., D. N. Ghosh, K. Ghosh, and A. K. Bhattacharya. "Multifractality and singularity of 8B solar neutrino flux signals from Sudbury Neutrino Observatory." IET Signal Processing 5, no. 7 (2011): 690. http://dx.doi.org/10.1049/iet-spr.2010.0168.

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26

Chan, Y. "Solar neutrino flux measurement from the pure D2O-phase of the sudbury neutrino observatory." Nuclear Physics A 718 (May 2003): 75–82. http://dx.doi.org/10.1016/s0375-9474(03)00682-1.

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27

EJIRI, HIROYASU. "MAJORANA NEUTRINO MASSES BY SPECTROSCOPIC STUDIES OF DOUBLE BETA DECAYS AND MOON." Modern Physics Letters A 22, no. 18 (June 14, 2007): 1277–91. http://dx.doi.org/10.1142/s0217732307023778.

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This is a brief review of spectroscopic studies of neutrino-less double beta decays (0νββ) and the MOON (Mo Observatory Of Neutrinos) project. It aims at studying the Majorana nature of neutrinos and the mass spectrum by spectroscopic studies of 0νββ with ν-mass sensitivity of 〈mν〉 ≈ 30 meV . The solid scintillator option of the MOON detector is a super ensemble of multi-layer modules, each being composed by a scintillator plate and two tracking detector planes. Thin ββ source films are interleaved between the detector planes. High localization of the two β tracks enables one to select true signals and reject BG ones by spatial and time correlation analyses. MOON with detector ≠ ββ source is used for studying 0νββ decays from 100 Mo , 82 Se and other ββ isotopes with large nuclear sensitivity (large Qββ). Real-time exclusive measurements of low energy solar neutrinos can also be made by observing inverse β rays from solar-ν captures of 100 Mo in delayed coincidence with the subsequent β decay of 100 Tc .

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Vescovi, D., L. Piersanti, S. Cristallo, M. Busso, F. Vissani, S. Palmerini, S. Simonucci, and S. Taioli. "Effects of a revised 7Be e−-capture rate on solar neutrino fluxes." Astronomy & Astrophysics 623 (March 2019): A126. http://dx.doi.org/10.1051/0004-6361/201834993.

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Context. Electron-capture on 7Be is the main production channel for 7Li in several astrophysical environments. Theoretical evaluations have to account for not only the nuclear interaction, but also the processes in the plasma in which 7Be ions and electrons interact. In recent decades several estimates were presented, pointing out that the theoretical uncertainty in the rate is in general of a few percent. Aims. In the framework of fundamental solar physics, we consider a recent evaluation for the 7Be+e− rate, which has not been used up to now, in the estimate of neutrino fluxes. Methods. We analyzed the effects of the new assumptions on standard solar models (SSMs) and compared the results obtained by adopting the revised 7Be+e− rate to those obtained by that reported in a widely used compilation of reaction rates (ADE11). Results. We found that new SSMs yield a maximum difference in the efficiency of the 7Be channel of about −4% with respect to what is obtained with the previously adopted rate. This fact affects the production of neutrinos from 8B, increasing the relative flux up to a maximum of 2.7%. Negligible variations are found for the physical and chemical properties of the computed solar models. Conclusions. The agreement with the Sudbury Neutrino Observatory measurements of the neutral current component of the 8B neutrino flux is improved.

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Steiger, T. D. "Catching some Zs: The solar neutrino problem, neutral current interactions, and the Sudbury Neutrino Observatory." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 472, no. 3 (October 2001): 348–53. http://dx.doi.org/10.1016/s0168-9002(01)01269-4.

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Aharmim, B., S. N. Ahmed, A. E. Anthony, N. Barros, E. W. Beier, A. Bellerive, B. Beltran, et al. "SEARCHES FOR HIGH-FREQUENCY VARIATIONS IN THE8B SOLAR NEUTRINO FLUX AT THE SUDBURY NEUTRINO OBSERVATORY." Astrophysical Journal 710, no. 1 (January 20, 2010): 540–48. http://dx.doi.org/10.1088/0004-637x/710/1/540.

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31

Andringa, S., E. Arushanova, S. Asahi, M. Askins, D. J. Auty, A. R. Back, Z. Barnard, et al. "Current Status and Future Prospects of the SNO+ Experiment." Advances in High Energy Physics 2016 (2016): 1–21. http://dx.doi.org/10.1155/2016/6194250.

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SNO+ is a large liquid scintillator-based experiment located 2 km underground at SNOLAB, Sudbury, Canada. It reuses the Sudbury Neutrino Observatory detector, consisting of a 12 m diameter acrylic vessel which will be filled with about 780 tonnes of ultra-pure liquid scintillator. Designed as a multipurpose neutrino experiment, the primary goal of SNO+ is a search for the neutrinoless double-beta decay (0νββ) of130Te. In Phase I, the detector will be loaded with 0.3% natural tellurium, corresponding to nearly 800 kg of130Te, with an expected effective Majorana neutrino mass sensitivity in the region of 55–133 meV, just above the inverted mass hierarchy. Recently, the possibility of deploying up to ten times more natural tellurium has been investigated, which would enable SNO+ to achieve sensitivity deep into the parameter space for the inverted neutrino mass hierarchy in the future. Additionally, SNO+ aims to measure reactor antineutrino oscillations, low energy solar neutrinos, and geoneutrinos, to be sensitive to supernova neutrinos, and to search for exotic physics. A first phase with the detector filled with water will begin soon, with the scintillator phase expected to start after a few months of water data taking. The0νββPhase I is foreseen for 2017.

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Fargion, Daniele, Pietro Oliva, Pier Giorgio de Sanctis Lucentini, and Maxim Yu Khlopov. "Signals of HE atmospheric μ decay in flight around the Sun’s albedo versus astrophysical νμ and ντ traces in the Moon shadow." International Journal of Modern Physics D 27, no. 06 (April 2018): 1841002. http://dx.doi.org/10.1142/s021827181841002x.

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The Sun albedo of Cosmic Rays (CRs) at GeVs energy has been discovered recently by the FERMI satellite. They are traces of atmospheric CRs hitting solar atmosphere and reflecting skimming gamma photons. Even if relevant for astrophysics, as being a trace of atmospheric solar CR noises they cannot offer any signal of neutrino astronomy. On the contrary, the Moon with no atmosphere, may become soon a novel filtering calorimeter and an amplifier of energetic muon astronomical neutrinos (at TeV up to hundred TeVs energy); these lepton tracks leave an imprint in their beta decay while in flight to Earth. Their TeV electron air-shower are among the main signals. Also, a more energetic, but more rare, PeV up to EeV tau lunar neutrino events may be escaping as a tau lepton from the Moon: [Formula: see text] PeV secondaries, then, may be shining on Earth’s atmosphere in lunar shadows in a surprising way. One or a few gamma air-shower events inside the Moon shadows may occur each year in near future Cherenkov telescope array (CTA) or large high altitude air shower observatory (LHAASO) TeV gamma array detector, assuming a nonnegligible astrophysical TeV up to hundred TeV neutrino component (with respect to our terrestrial ruling atmospheric ones); these signals will open a new wonderful passe-partout keyhole for neutrino, been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but with the future largest tau radio array as the giant radio array for neutrino detection (GRAND), one might well discover such neutrino imprint.

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Goon, Jason, Blair Jamieson, James Loach, Ryan Martin, Scott Oser, Nikolai Tolich, Alex Wright, and SNO Collaboration. "Signal extraction of the solar neutrino Neutral-Current flux with the Sudbury Neutrino Observatory Neutral Current Detectors." Journal of Physics: Conference Series 136, no. 4 (November 1, 2008): 042010. http://dx.doi.org/10.1088/1742-6596/136/4/042010.

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34

Smith, Peter F. "Further studies of the OMNIS supernova neutrino observatory: optimisation of detector configuration and possible extension to solar neutrinos." Astroparticle Physics 16, no. 1 (October 2001): 75–96. http://dx.doi.org/10.1016/s0927-6505(01)00104-9.

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35

CABIBBO, NICOLA. "CONCLUDING REMARKS." International Journal of Modern Physics A 17, no. 24 (September 30, 2002): 3500–3508. http://dx.doi.org/10.1142/s0217751x02012892.

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Important new results have been presented at this conference. The direct violation of CP in K0 → π + π has been firmly established in two independent experiments, NA48 at CERN and KTeV at Fermilab. Both Babar at SLAC and Belle at Kek have determined the CP violation in [Formula: see text] oscillations through the study of the golden KS + Ψ decay mode. The observed CP violation agrees with the expectations of the Standard model, based on the quark-mixing phenomenon. The first results of the Sudbury Neutrino Observatory, SNO, suggest that the long-lasting solar neutrino puzzle has been finally solved in terms of neutrino oscillations. Results appeared after the conference which modify the theoretical prediction of the muon anomaly. This new result, if confirmed, would drastically reduce the significance of the discrepancy between the theoretically expected value for the muon anomaly and the recent results of the Brookhaven experiment.

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36

Farine, J. "Measurement of the rate of ν e+d → p+p+e − interactions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory." Physics of Atomic Nuclei 65, no. 12 (December 2002): 2147–55. http://dx.doi.org/10.1134/1.1530292.

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37

Lawson, Ian T. "Solar neutrino results from the sudbury neutrino observatoryy." Nuclear Physics B - Proceedings Supplements 110 (July 2002): 308–10. http://dx.doi.org/10.1016/s0920-5632(02)01494-9.

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38

Jamieson, B. "The measurement of the solar neutrino flux with the sudbury neutrino observatory's neutron capture detector." Journal of Physics: Conference Series 110, no. 12 (June 1, 2008): 122014. http://dx.doi.org/10.1088/1742-6596/110/12/122014.

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39

CASOLINO, MARCO. "THE PAMELA COSMIC RAY SPACE OBSERVATORY." International Journal of Modern Physics D 22, no. 11 (September 2013): 1360002. http://dx.doi.org/10.1142/s021827181360002x.

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PAMELA is a satellite borne experiment designed to study with great accuracy cosmic rays of galactic, solar, and trapped nature in a wide energy range (protons: 80 MeV–700 GeV, electrons 50 MeV–400 GeV). Main objective is the study of the antimatter component: antiprotons (80 MeV–190 GeV), positrons (50 MeV–270 GeV) and search for antimatter with a precision of the order of 10-8). The experiment, housed on board the Russian Resurs-DK1 satellite, was launched on June, 15 2006 in a 350 × 600 km orbit with an inclination of 70 degrees. The detector is composed of a series of scintillator counters arranged at the extremities of a permanent magnet spectrometer to provide charge, Time-of-Flight and rigidity information. Lepton/hadron identification is performed by a Silicon-Tungsten calorimeter and a Neutron detector placed at the bottom of the device. An Anticounter system is used offline to reject false triggers coming from the satellite. In self-trigger mode the Calorimeter, the neutron detector and a shower tail catcher are capable of an independent measure of the lepton component up to 2 TeV. In this work we present some of its scientific results in its first five years of operation.

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40

Ni, Wei-Tou, Gang Wang, and An-Ming Wu. "Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design." International Journal of Modern Physics D 29, no. 04 (March 2020): 1940007. http://dx.doi.org/10.1142/s0218271819400078.

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AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric Gravitational Wave (GW) Observatory. The scientific goals of AMIGO are to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities: to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescences together with binary neutron star & black hole-neutron star coalescences for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry (TDI) for a nearly triangular formation of three drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2–10 W and telescope diameter 300–500 mm. The design GW sensitivity in the middle frequency band is [Formula: see text] Hz[Formula: see text]. Both geocentric and heliocentric orbit formations are considered. All options have LISA-like formations, that is, the triangular formation is [Formula: see text] inclined to the orbit plane. For all solar orbit options of AMIGO, the first-generation TDI satisfies the laser frequency-noise suppression requirement. We also investigate for each option of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit options, the acceleration to maintain the formation can be designed to be less than 15 nm/s2 with the thruster requirement in the 15 [Formula: see text]N range. AMIGO would be a good place to test the feasibility of the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the mission orbit preference. We study the deployment for this orbit option. After a last-stage launch from 300 km Low Earth Orbit (LEO), each S/C’s maneuver to an appropriate 2-degree-behind-the-Earth AMIGO formation in 95 days requires only a [Formula: see text]v of about 80 m/s.

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41

Tautvaišienė, G., C. Viscasillas Vázquez, Š. Mikolaitis, E. Stonkutė, R. Minkevičiūtė, A. Drazdauskas, and V. Bagdonas. "Abundances of neutron-capture elements in thin- and thick-disc stars in the solar neighbourhood." Astronomy & Astrophysics 649 (May 2021): A126. http://dx.doi.org/10.1051/0004-6361/202039979.

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Aims. The aim of this work is to determine abundances of neutron-capture elements for thin- and thick-disc F, G, and K stars in several selected sky fields near the north ecliptic pole and to compare the results with the Galactic chemical evolution models, to explore elemental gradients according to stellar ages, mean galactocentric distances, and maximum heights above the Galactic plane. Methods. The observational data were obtained with the 1.65 m telescope at the Molėtai Astronomical Observatory and a fibre-fed high-resolution spectrograph covering a full visible wavelength range (4000−8500 Å). Elemental abundances were determined using a differential line-by-line spectrum synthesis using the TURBOSPECTRUM code with the MARCS stellar model atmospheres and accounting for the hyperfine-structure effects. Results. We determined abundances of Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, and Eu for 424 thin- and 82 thick-disc stars. The sample of thick-disc stars shows a clearly visible decrease in [Eu/Mg] with increasing metallicity compared to the thin-disc stars, bringing more evidence of a different chemical evolution in these two Galactic components. Abundance correlation with age slopes for the investigated thin-disc stars are slightly negative for the majority of s-process dominated elements, while r-process dominated elements have positive correlations. Our sample of thin-disc stars with ages spanning from 0.1 to 9 Gyr gives the [Y/Mg] = 0.022 (±0.015)−0.027 (±0.003)⋅age [Gyr] relation. However, for the thick-disc stars, when we also took data from other studies into account, we found that [Y/Mg] cannot serve as an age indicator. The radial abundance-to-iron gradients in the thin disc are negligible for the s-process dominated elements and become positive for the r-process dominated elements. The vertical gradients are negative for the light s-process dominated elements and become positive for the r-process dominated elements. In the thick disc, the radial abundance-to-iron slopes are negligible, and the vertical slopes are predominantly negative.

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Chen, Xuelei, Jingye Yan, Li Deng, Fengquan Wu, Lin Wu, Yidong Xu, and Li Zhou. "Discovering the sky at the longest wavelengths with a lunar orbit array." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 379, no. 2188 (November 23, 2020): 20190566. http://dx.doi.org/10.1098/rsta.2019.0566.

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Due to ionosphere absorption and the interference of natural and artificial radio emissions, astronomical observation from the ground becomes very difficult at the wavelengths of decametre or longer, which we shall refer to as the ultralong wavelengths. This unexplored part of the electromagnetic spectrum has the potential for great discoveries, notably in the study of cosmic dark ages and dawn, but also in heliophysics and space weather, planets and exoplanets, cosmic ray and neutrinos, pulsar and interstellar medium (ISM), extragalactic radio sources, and so on. The difficulty of the ionosphere can be overcome by space observation, and the Moon can shield the radio frequency interferences (RFIs) from the Earth. A lunar orbit array can be a practical first step to opening up the ultralong wave band. Compared with a lunar surface observatory on the far side, the lunar orbit array is simpler and more economical, as it does not need to make the risky and expensive landing, can be easily powered with solar energy, and the data can be transmitted back to the Earth when it is on the near-side part of the orbit. Here, I describe the discovering sky at the longest wavelength (DSL) project, which will consist of a mother satellite and 6–9 daughter satellites, flying on the same circular orbit around the Moon, and forming a linear interferometer array. The data are collected by the mother satellite which computes the interferometric cross-correlations (visibilities) and transmits the data back to the Earth. The whole array can be deployed on the lunar orbit with a single rocket launch. The project is under intensive study in China. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades’.

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Hawkins, Keith, Madeline Lucey, and Jason Curtis. "The chemical nature of the young 120-Myr-old nearby Pisces–Eridanus stellar stream flowing through the Galactic disc." Monthly Notices of the Royal Astronomical Society 496, no. 2 (June 12, 2020): 2422–35. http://dx.doi.org/10.1093/mnras/staa1673.

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ABSTRACT Recently, a new cylindrical-shaped stream of stars up to 700 pc long was discovered hiding in the Galactic disc using kinematic data enabled by the Gaia mission. This stream of stars, dubbed Pisces–Eridanus (Psc–Eri), was initially thought to be as old as 1 Gyr, yet its stars shared a rotation period distribution consistent with a population that was 120 Myr old. Here, we explore the detailed chemical nature of this stellar stream. We carried out high-resolution spectroscopic follow-up of 42 Psc–Eri stars using McDonald Observatory and combined these data with information for 40 members observed with the low-resolution LAMOST spectroscopic survey. Together, these data enabled us to measure the abundance distribution of light/odd-Z (Li, Na, Al, Sc, V), α (Mg, Si, Ca, Ti), Fe-peak (Cr, Mn, Fe, Co, Ni, Zn), and neutron capture (Sr, Y, Zr, Ba, La, Nd, Eu) elements along the Psc–Eri stream. We find that the stream is (1) near-solar metallicity with [Fe/H] = –0.03 dex and (2) has a metallicity spread of 0.07 dex (or 0.04 dex when outliers are excluded). We also find that (3) the abundance of Li indicates that Psc–Eri is ∼120 Myr old, consistent with its gyrochronology age. Additionally, Psc–Eri has (4) [X/Fe] abundance spreads that are just larger than the typical uncertainty in most elements, (5) it is a cylindrical-like system whose outer edges rotate about the centre, and (6) no significant abundance gradients along its major axis except a potentially weak gradient in [Si/Fe]. These results show that Psc–Eri is a uniquely close young chemically interesting laboratory for testing our understanding of star and planet formation.

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Universe, Helical. "The Solar Neutrino Problem Has Not Been Solved." JOURNAL OF ADVANCES IN PHYSICS, December 30, 2017, 4821–29. http://dx.doi.org/10.24297/jap.v13i4.5950.

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A closer look at the data collected from different detectors, reveal that the so-called solar neutrino problem is far from being solved. And contrary to the assessment of the Nobel Committee, the experimental results from the Sudbury Neutrino Observatory cannot be a confirmation of the Standard Solar Model. In fact, the obsoleteness of the current model has been recently exposed by the crisis of solar abundance. Furthermore, using images obtained by the Solar Dynamics Observatory, researchers found the convective motions (the plasma motions at the Sun's interior) to be nearly 100 times smaller than current theoretical expectations.

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45

Aalbers, J., F. Agostini, S. E. M. Ahmed Maouloud, M. Alfonsi, L. Althueser, F. D. Amaro, J. Angevaare, et al. "Solar neutrino detection sensitivity in DARWIN via electron scattering." European Physical Journal C 80, no. 12 (December 2020). http://dx.doi.org/10.1140/epjc/s10052-020-08602-7.

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AbstractWe detail the sensitivity of the proposed liquid xenon DARWIN observatory to solar neutrinos via elastic electron scattering. We find that DARWIN will have the potential to measure the fluxes of five solar neutrino components: pp, $$^7$$ 7 Be, $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep. The precision of the $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep components is hindered by the double-beta decay of $$^{136}$$ 136 Xe and, thus, would benefit from a depleted target. A high-statistics observation of pp neutrinos would allow us to infer the values of the electroweak mixing angle, $$\sin ^2\theta _w$$ sin 2 θ w , and the electron-type neutrino survival probability, $$P_{ee}$$ P ee , in the electron recoil energy region from a few keV up to 200 keV for the first time, with relative precision of 5% and 4%, respectively, with 10 live years of data and a 30 tonne fiducial volume. An observation of pp and $$^7$$ 7 Be neutrinos would constrain the neutrino-inferred solar luminosity down to 0.2%. A combination of all flux measurements would distinguish between the high- (GS98) and low-metallicity (AGS09) solar models with 2.1–2.5$$\sigma $$ σ significance, independent of external measurements from other experiments or a measurement of $$^8$$ 8 B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, we demonstrate that with a depleted target DARWIN may be sensitive to the neutrino capture process of $$^{131}$$ 131 Xe.

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46

"Status of the Soviet-American gallium experiment." Philosophical Transactions of the Royal Society of London. Series A: Physical and Engineering Sciences 346, no. 1678 (January 15, 1994): 15–21. http://dx.doi.org/10.1098/rsta.1994.0003.

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A radiochemical 71 Ga- 71 Ge experiment to determine the primary flux of neutrinos from the Sun began measurements of the solar neutrino flux at the Baksan Neutrino Observatory in 1990. The number of 71 Ge atoms extracted from 30 tons of gallium in 1990 and from 57 tons of gallium in 1991 was measured in 12 runs during the period of January 1990 to December 1991. The combined 1990 and 1991 data-sets give a value of 58 + 17/ —24 (stat) ± 14 (syst) SNU. This is to be compared with 132 + 7/ —5 SNU predicted by the Standard Solar Model.

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47

Wallenius, Maria, Klaus Mayer, Sylvain Millet, Adrian Nicholl, Edmund Henrich, Marco Balata, Stefano Nisi, and Klaus Lützenkirchen. "Precise isotope ratio measurements by MC-ICP-MS and application of the isotope dilution technique for the determination of germanium in the Gallium Neutrino Observatory." Radiochimica Acta 96, no. 8 (January 1, 2008). http://dx.doi.org/10.1524/ract.2008.1513.

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SummaryIn the Gallium Neutrino Observatory (GNO) experiment solar neutrinos are studied. Low energy neutrinos interact withGe-removal from the GaClIn this paper we describe the evaluation of the results using the two-isotopes and two-components approach, as well as the multi-isotope and three-components approaches. We could demonstrate that the measured isotopic composition of the carrier after extraction can be fully modelled by a mixture of the initially used Ge carrier, of the Ge carrier from the previous run and of a small, but non-negligible contribution of a natural Ge contamination.

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48

McDonald, Arthur B. "Nobel Lecture: The Sudbury Neutrino Observatory: Observation of flavor change for solar neutrinos." Reviews of Modern Physics 88, no. 3 (July 6, 2016). http://dx.doi.org/10.1103/revmodphys.88.030502.

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49

Bhusal, Aagaman, Nick Houston, and Tianjun Li. "Searching for Solar Axions Using Data from the Sudbury Neutrino Observatory." Physical Review Letters 126, no. 9 (March 2, 2021). http://dx.doi.org/10.1103/physrevlett.126.091601.

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50

Aharmim, B., S. N. Ahmed, A. E. Anthony, N. Barros, E. W. Beier, A. Bellerive, B. Beltran, et al. "Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory." Physical Review C 88, no. 2 (August 1, 2013). http://dx.doi.org/10.1103/physrevc.88.025501.

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