Sensitivity to neutrinos from the solar CNO cycle in Borexino
Sensitivity to neutrinos from the solar CNO cycle in Borexino
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DOI：
10.1140/epjc/s10052-020-08534-2
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发表时间：
2020-05
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通讯作者：
M. Agostini;K. Altenmüller;S. Appel;V. Atroshchenko;Z. Bagdasarian;Z. Bagdasarian;D. Basilico;G. Bellini;J. Benziger;R. Biondi;D. Bravo;B. Caccianiga;F. Calaprice;A. Caminata;P. Cavalcante;A. Chepurnov;D. D’Angelo;S. Davini;A. Derbin;A. D. Giacinto;V. D. Marcello;X. Ding;A. D. Ludovico;L. Noto;I. Drachnev;A. Formozov;D. Franco;C. Galbiati;C. Ghiano;M. Giammarchi;A. Goretti;A. Göttel;A. Göttel;M. Gromov;M. Gromov;D. Guffanti;A. Ianni;A. Ianni;A. Jany;D. Jeschke;V. Kobychev;G. Korga;S. Kumaran;S. Kumaran;M. Laubenstein;E. Litvinovich;E. Litvinovich;P. Lombardi;I. Lomskaya;L. Ludhova;L. Ludhova;G. Lukyanchenko;L. Lukyanchenko;I. Machulin;I. Machulin;J. Martyn;E. Meroni;M. Meyer;L. Miramonti;M. Misiaszek;V. Muratova;B. Neumair;M. Nieslony;R. Nugmanov;R. Nugmanov;L. Oberauer;V. Orekhov;F. Ortica;M. Pallavicini;L. Papp;Ö. Penek;Ö. Penek;L. Pietrofaccia;N. Pilipenko;A. Pocar;G. Raikov;M. Ranalli;G. Ranucci;A. Razeto;A. Re;M. Redchuk;M. Redchuk;A. Romani;N. Rossi;S. Schönert;D. Semenov;G. Settanta;M. Skorokhvatov;M. Skorokhvatov;O. Smirnov;A. Sotnikov;Y. Suvorov;R. Tartaglia;G. Testera;J. Thurn;E. Unzhakov;F. Villante;A. Vishneva;R. Vogelaar;F. Feilitzsch;M. Wójcik;M. Wurm;S. Zavatarelli;K. Zuber;G. Zuzel
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文献类型：
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作者：
M. Agostini;K. Altenmüller;S. Appel;V. Atroshchenko;Z. Bagdasarian;Z. Bagdasarian;D. Basilico;G. Bellini;J. Benziger;R. Biondi;D. Bravo;B. Caccianiga;F. Calaprice;A. Caminata;P. Cavalcante;A. Chepurnov;D. D’Angelo;S. Davini;A. Derbin;A. D. Giacinto;V. D. Marcello;X. Ding;A. D. Ludovico;L. Noto;I. Drachnev;A. Formozov;D. Franco;C. Galbiati;C. Ghiano;M. Giammarchi;A. Goretti;A. Göttel;A. Göttel;M. Gromov;M. Gromov;D. Guffanti;A. Ianni;A. Ianni;A. Jany;D. Jeschke;V. Kobychev;G. Korga;S. Kumaran;S. Kumaran;M. Laubenstein;E. Litvinovich;E. Litvinovich;P. Lombardi;I. Lomskaya;L. Ludhova;L. Ludhova;G. Lukyanchenko;L. Lukyanchenko;I. Machulin;I. Machulin;J. Martyn;E. Meroni;M. Meyer;L. Miramonti;M. Misiaszek;V. Muratova;B. Neumair;M. Nieslony;R. Nugmanov;R. Nugmanov;L. Oberauer;V. Orekhov;F. Ortica;M. Pallavicini;L. Papp;Ö. Penek;Ö. Penek;L. Pietrofaccia;N. Pilipenko;A. Pocar;G. Raikov;M. Ranalli;G. Ranucci;A. Razeto;A. Re;M. Redchuk;M. Redchuk;A. Romani;N. Rossi;S. Schönert;D. Semenov;G. Settanta;M. Skorokhvatov;M. Skorokhvatov;O. Smirnov;A. Sotnikov;Y. Suvorov;R. Tartaglia;G. Testera;J. Thurn;E. Unzhakov;F. Villante;A. Vishneva;R. Vogelaar;F. Feilitzsch;M. Wójcik;M. Wurm;S. Zavatarelli;K. Zuber;G. Zuzel
在太阳的碳、氮、氧(CNO)聚变循环中发射的中微子是太阳中微子中次要但关键的组成部分，其通量尚未被测量。由于探测器的放射性安全性和对探测器背景的精确了解，意大利国家实验室的Borexino实验有一个直接探测它们的独特机会。我们讨论了Borexino对CNO中微子的敏感性，这是基于我们采取的限制两个最相关背景源的速率的策略，来自Solarpp链的$$pep中微子和$210铋β衰变起源于液体闪烁体的本征污染。210铅。假定高金属丰度标准太阳模型所预测的CNO通量为1000日×71.3t，Borexino对CNO中微子的敏感度中值大于3$$\sigma$σ。在相同的假设下，CNO中微子通量的预期实验不确定度为23%，假设对$$^{210}\Text{Bi}$$210的独立估计的不确定度为1.5$$\HBox{cpd}/100~\Hbox{ton}$$CPD/100吨/吨。最后，我们评估了C和N丰度的预期不确定度和高、低金属丰度标准太阳模型(HZ和LZ)之间的预期区分意义，以期在未来更精确地测量CNO太阳中微子通量。
Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector’s radiopurity and the precise understanding of the detector backgrounds. We discuss the sensitivity of Borexino to CNO neutrinos, which is based on the strategies we adopted to constrain the rates of the two most relevant background sources, $$pep$$ pep neutrinos from the solarpp-chain and $$^{210}$$ 210 Bi beta decays originating in the intrinsic contamination of the liquid scintillator with $$^{210}$$ 210 Pb. Assuming the CNO flux predicted by the high-metallicity Standard Solar Model and an exposure of 1000 days $$\times $$ × 71.3 t, Borexino has a median sensitivity to CNO neutrino higher than 3 $$\sigma $$ σ . With the same hypothesis the expected experimental uncertainty on the CNO neutrino flux is 23%, provided the uncertainty on the independent estimate of the $$^{210}\text {Bi}$$ 210 Bi interaction rate is 1.5 $$\hbox {cpd}/100~\hbox {ton}$$ cpd / 100 ton . Finally, we evaluated the expected uncertainty of the C and N abundances and the expected discrimination significance between the high and low metallicity Standard Solar Models (HZ and LZ) with future more precise measurement of the CNO solar neutrino flux.