Cosmic Neutrino Radiation

Marx, G.; Menyhárd, Nora

doi:10.1126/science.131.3396.299

Cited by 17 publications

(11 citation statements)

References 7 publications

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“…where H CC rad is the radiogenic heat produced in the continental crust. The secular cooling of the core is expected in the range of [5][6][7][8][9][10][11] TW [38], while no radiogenic heat is expected to be produced in the core.…”

Section: Why Study Geoneutrinos?mentioning

confidence: 99%

“…Every ID PMT is ACcoupled to an electronic chain made by an analogue front end (so-called FE boards, FEBs) followed by a digital circuit (so-called Laben boards). 6 While the main DAQ treats every PMT individually, the FADC sub-system receives as input the sums of up to 24 analogue FEB outputs. More details about the Borexino data structure are given in Sec.…”

Section: The Borexino Detectormentioning

confidence: 99%

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Comprehensive geoneutrino analysis with Borexino

Agostini¹,

Altenmüller²,

Appel³

et al. 2020

Phys. Rev. D

104

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This paper presents a comprehensive geoneutrino measurement using the Borexino detector, located at Laboratori Nazionali del Gran Sasso (LNGS) in Italy. The analysis is the result of 3262.74 days of data between December 2007 and April 2019. The paper describes improved analysis techniques and optimized data selection, which includes enlarged fiducial volume and sophisticated cosmogenic veto. The reported exposure of ð1.29 AE 0.05Þ × 10 32 protons × year represents an increase by a factor of two over a previous Borexino analysis reported in 2015. By observing 52.6 þ9.4 −8.6 ðstatÞ þ2.7 −2.1 ðsysÞ geoneutrinos (68% interval) from 238 U and 232 Th, a geoneutrino signal of 47.0 þ8.4 −7.7 ðstatÞ þ2.4 −1.9 ðsysÞ TNU with þ18.3 −17.2 % total precision was obtained. This result assumes the same Th/U mass ratio as found in chondritic CI meteorites but compatible results were found when contributions from 238 U and 232 Th were both fit as free parameters. Antineutrino background from reactors is fit unconstrained and found compatible with the expectations. The null-hypothesis of observing a geoneutrino signal from the mantle is excluded at a 99.0% C.L. when exploiting detailed knowledge of the local crust near the experimental site. Measured mantle signal of 21.2 þ9.5 −9.0 ðstatÞ þ1.1 −0.9 ðsysÞ TNU corresponds to the production of a radiogenic heat of 24.6 þ11.1 −10.4 TW (68% interval) from 238 U and 232 Th in the mantle. Assuming 18% contribution of 40 K in the mantle and 8.1 þ1.9 −1.4 TW of total radiogenic heat of the lithosphere, the Borexino estimate of the total radiogenic heat of the Earth is 38.2 þ13.6 −12.7 TW, which corresponds to the convective Urey ratio of 0.78 þ0.41 −0.28. These values are compatible with different geological predictions, however there is a ∼2.4σ tension with those Earth models which predict the lowest concentration of heat-producing elements in the mantle. In addition, by constraining the number of expected reactor antineutrino events, the existence of a hypothetical georeactor at the center of the Earth having power greater than 2.4 TW is excluded at 95% C.L. Particular attention is given to the description of all analysis details which should be of interest for the next generation of geoneutrino measurements using liquid scintillator detectors.

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Section: Why Study Geoneutrinos?mentioning

confidence: 99%

Section: The Borexino Detectormentioning

confidence: 99%

Comprehensive geoneutrino analysis with Borexino

Agostini¹,

Altenmüller²,

Appel³

et al. 2020

Phys. Rev. D

104

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“…10 Proposed experimental arrangement.-Consider a thin, large-area slab of target material (Li or B) surrounded on both sides by a detector. We assume here that the detector is an organic scintillator.…”

Section: (3)mentioning

confidence: 99%

New Approach to the Detection of Solar Neutrinos Via inverse Beta Decay

Reines¹,

Woods²

1965

Phys. Rev. Lett.

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nucleus. The cross section for the production of such a coherent state should be enhanced by a factor of the order of the number of contributing states. The extreme assumption of perfect unitary symmetry implies an equivalence of nucleons and hyperons such that it costs the same energy to change a neutron to a A in any orbit. The SU(3) multiplets contain coherent linear combinations of all these states and also include states in which a nucleon is transformed into a Z as well. Because of symmetry breaking, the 2 component of the SU(3) analog state must clearly be rejected in view of the large Z-A mass difference, while the A component of the SU(3) state must be split by the difference between A-nucleon and nucleon-nucleon interactions. However, some coherence and enhancement may still remain if there are groups of states which are approximately degenerate. One should then expect to see some kind of a peak, possibly with some structure, in the pion spectrum at low momentum transfer in Reaction (1). The observed cross section should be smaller and the observed width greater than that predicted from pure SU(3) symmetry.Another reaction which might be of interest is This reaction has two outgoing charged particles which can be measured. This is analogous to the (p, 2p) experiments for probing nuclear structure. 5 The advantage of this type of reaction is that the angles and energies of the outgoing pions can be set at values corresponding to zero momentum transfer to the residual nucleus.Theoretical calculations for the energy generation processes in the sun predict 1 the production of B 8 in such quantities that a neutrino flux at earth of (2.5± 1)10 7 ^/cm 2 sec and end point of 14.06 MeV results from beta decay of this nuclide. It is of great interest to check this prediction since it relates to the entire theoretical picture of the sun's deep interior condition. To date, two methods of detection have been suggested, that of Davis 2 which employs a radiochemical technique to observe inverse beta decay of CI 37 , and the direct counting approach of Reines and Kropp 3 in which it is proposed to detect the recoil electron from elastically scattered solar neutrinos. The point of this communication is to discuss yet another approach to the problem, using inverse beta decay.It is desirable to measure the neutrino spectrum and the direction from which the signals emanate in order to label separately the source and the responsible reaction. The radiochemical approach is limited in that it gives the response averaged over a spectrum and with a time constant determined by the half-life of the product nucleus. Also in the radiochemical approach the direct association with the sun can only be made by use of the 7% annual inverse-square variation of intensity. The elastic-scattering experiment, although capable of fairly precise 4 (~15°) directional and energy determination (e.g., by using a multiplate spark 20

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“…zNA--~ -z_q A --}-e + -{--r, (1) thus the total number of r's, radiated by the star, is nearly equal to the number of neutrons in the star; the ~-radiation can be neglected. In such a case the neutrinos take away no more than a few per cent of the total radiation energy [1].…”

Section: W 1 Thermal Neutrino Radiation Of a Hot Plasmamentioning

confidence: 99%

“…In such a case the neutrinos take away no more than a few per cent of the total radiation energy [1]. However, as the star temperature approaches 109 ~ processes begin which produce r --~ pairs at the expense of the inner thermal energy of the stellar matter.…”

Section: W 1 Thermal Neutrino Radiation Of a Hot Plasmamentioning

confidence: 99%