Three-Body Treatment of the pep Reaction in the Sun
The experimental result of the neutrino flux produced by the p + p + e → d + ν e reaction ( pep ) in the Sun at 1 AU was announced for the first time in 2012 by the Borexino collaboration. We use the three-body model for the proton–proton–electron system in the initial state for the calculatio...
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| Veröffentlicht in: | Few-body systems 2014-08, Vol.55 (8-10), p.783-786, Article 783 |
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| container_end_page | 786 |
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| container_issue | 8-10 |
| container_start_page | 783 |
| container_title | Few-body systems |
| container_volume | 55 |
| creator | Irgaziev, B. F. Belyaev, V. B. |
| description | The experimental result of the neutrino flux produced by the
p
+
p
+
e
→
d
+
ν
e
reaction (
pep
) in the Sun at 1 AU was announced for the first time in
2012
by the Borexino collaboration. We use the three-body model for the proton–proton–electron system in the initial state for the calculation of the rate of the
pep
reaction with various types of nucleon–nucleon potentials. |
| doi_str_mv | 10.1007/s00601-013-0748-4 |
| format | Article |
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p
+
p
+
e
→
d
+
ν
e
reaction (
pep
) in the Sun at 1 AU was announced for the first time in
2012
by the Borexino collaboration. We use the three-body model for the proton–proton–electron system in the initial state for the calculation of the rate of the
pep
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p
+
p
+
e
→
d
+
ν
e
reaction (
pep
) in the Sun at 1 AU was announced for the first time in
2012
by the Borexino collaboration. We use the three-body model for the proton–proton–electron system in the initial state for the calculation of the rate of the
pep
reaction with various types of nucleon–nucleon potentials.</description><subject>Atomic</subject><subject>Chemical reactions</subject><subject>Flux</subject><subject>Hadrons</subject><subject>Heavy Ions</subject><subject>Mathematical models</subject><subject>Molecular</subject><subject>Neutrinos</subject><subject>Nuclear Physics</subject><subject>Optical and Plasma Physics</subject><subject>Particle and Nuclear Physics</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Sun</subject><issn>0177-7963</issn><issn>1432-5411</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNp9kD1PwzAQhi0EEqXwA9gisbAY7mzHTkao-JIqIUGZLTc901RpEux04N-TEAZUCSZL5-e5j5exc4QrBDDXEUADckDJwaiMqwM2QSUFTxXiIZsAGsNNruUxO4lxA4BpjjBhcrEORPy2WX0mi0Cu21LdJY1PujUlLbXJC7miK5s6Kevv2uuuPmVH3lWRzn7eKXu7v1vMHvn8-eFpdjPnhcxEx5erwmSFzjSR8CScKDQBupX3S6WEAkEZgM-WPs1zI5UnRBq-UIPOnCA5ZZdj3zY0HzuKnd2WsaCqcjU1u2gx1WY4VpoevdhDN80u1P12PaWyFHSayp7CkSpCE2Mgb9tQbl34tAh2iNGOMdo-Rjt0tqp3zJ5TlJ0bEumCK6t_TTGasZ9Sv1P4tdOf0heInoRg</recordid><startdate>20140801</startdate><enddate>20140801</enddate><creator>Irgaziev, B. 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p
+
p
+
e
→
d
+
ν
e
reaction (
pep
) in the Sun at 1 AU was announced for the first time in
2012
by the Borexino collaboration. We use the three-body model for the proton–proton–electron system in the initial state for the calculation of the rate of the
pep
reaction with various types of nucleon–nucleon potentials.</abstract><cop>Vienna</cop><pub>Springer Vienna</pub><doi>10.1007/s00601-013-0748-4</doi><tpages>4</tpages></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0177-7963 |
| ispartof | Few-body systems, 2014-08, Vol.55 (8-10), p.783-786, Article 783 |
| issn | 0177-7963 1432-5411 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_1567074837 |
| source | SpringerLink Journals - AutoHoldings |
| subjects | Atomic Chemical reactions Flux Hadrons Heavy Ions Mathematical models Molecular Neutrinos Nuclear Physics Optical and Plasma Physics Particle and Nuclear Physics Physics Physics and Astronomy Sun |
| title | Three-Body Treatment of the pep Reaction in the Sun |
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