Neutrino Energy Loss in Stellar Interiors. VII. Pair, Photo-, Plasma, Bremsstrahlung, and Recombination Neutrino Processes

1996 ◽  
Vol 102 ◽  
pp. 411 ◽  
Author(s):  
Naoki Itoh ◽  
Hiroshi Hayashi ◽  
Akinori Nishikawa ◽  
Yasuharu Kohyama
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

Neutrino energy loss in stellar interiors. III - Pair, photo-, plasma, and bremsstrahlung processes

1989 ◽  
Vol 339 ◽  
pp. 354 ◽  
Author(s):  
Naoki Itoh ◽  
Tomoo Adachi ◽  
Masayuki Nakagawa ◽  
Yasuharu Kohyama ◽  
Hiroharu Munakata
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

Neutrino Energy Loss in Stellar Interiors. III. Pair, Photo-, Plasma, and Bremsstrahlung Processes: Erratum

1990 ◽  
Vol 360 ◽  
pp. 741 ◽  
Author(s):  
Itoh Naoki ◽  
Tomoo Adachi ◽  
Masayuki Nakagawa ◽  
Yasuharu Kohyama ◽  
Hiroharu Munakata
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

Neutrino Energy Loss in Stellar Interiors. VIII. Braaten-Segel Approximation for the Plasma Neutrino Process

1996 ◽  
Vol 470 ◽  
pp. 1015 ◽  
Author(s):  
Naoki Itoh ◽  
Akinori Nishikawa ◽  
Yasuharu Kohyama
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

RADIATIVE CORRECTIONS TO NEUTRINO ENERGY LOSS RATE IN STELLAR INTERIORS

2002 ◽  
Vol 17 (08) ◽  
pp. 491-502 ◽  
Author(s):  
S. ESPOSITO ◽  
G. MANGANO ◽  
G. MIELE ◽  
I. PICARDI ◽  
O. PISANTI
Keyword(s):  
Energy Loss ◽  
Loss Rate ◽  
Neutrino Energy ◽  
Tree Level ◽  
Energy Loss Rate ◽  
Star Evolution ◽  
Cooling Mechanism ◽  
Stellar Interiors ◽  
Neutrino Pair ◽  
Late Stages

We consider radiative electromagnetic corrections, at order α, to the process [Formula: see text] at finite density and temperature. This process represents one of the main contributions to the cooling of stellar environments in the late stages of star evolution. We find that these corrections affect the energy loss rate by a factor (-4-1)% with respect to the tree level estimate, in the temperature and density ranges where the neutrino pair production via e+e- annihilation is the most efficient cooling mechanism.

Neutrino energy loss in stellar interiors

1985 ◽  
Vol 296 ◽  
pp. 197 ◽  
Author(s):  
H. Munakata ◽  
Y. Kohyama ◽  
N. Itoh
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

Neutrino energy loss in stellar interiors. IV - Plasma neutrino process for strongly degenerate electrons

1992 ◽  
Vol 395 ◽  
pp. 622 ◽  
Author(s):  
Naoki Itoh ◽  
Haruhiko Mutoh ◽  
Atsushi Hikita ◽  
Yasuharu Kohyama
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors ◽  
Strongly Degenerate

Neutrino Energy Loss in Stellar Interiors: Erratum

1986 ◽  
Vol 304 ◽  
pp. 580 ◽  
Author(s):  
Hiroharu Munakata ◽  
Yasuharu Kohyama ◽  
Naoki Itoh
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors

Neutrino energy loss in stellar interiors. V - Recombination neutrino process

1993 ◽  
Vol 415 ◽  
pp. 267 ◽  
Author(s):  
Yasuharu Kohyama ◽  
Naoki Itoh ◽  
Akihiko Obama ◽  
Haruhiko Mutoh
Keyword(s):  
Energy Loss ◽  
Neutrino Energy ◽  
Stellar Interiors
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