## Proceedings of the International School of Physics "Enrico Fermi.", Volume 65N. Zanichelli, 1978 - Nuclear physics |

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Page 3

pressure due to it is given by ( 1 ) Psas = " HOT , where k denotes the Boltzmann

constant , H the mass of the hydrogen atom , u the

density and T the temperature . The pressure due to radiation , in the same ...

pressure due to it is given by ( 1 ) Psas = " HOT , where k denotes the Boltzmann

constant , H the mass of the hydrogen atom , u the

**mean**molecular weight , e thedensity and T the temperature . The pressure due to radiation , in the same ...

Page 429

Figure 31 shows a comparison of 1 ) neutrino

current effects and degeneracy effects , and 2 ) the

WILSON ( 1974 ) , for Q = 1012 g / cm3 and various values of temperature .

Figure 31 shows a comparison of 1 ) neutrino

**mean**free paths including neutral -current effects and degeneracy effects , and 2 ) the

**mean**free paths used byWILSON ( 1974 ) , for Q = 1012 g / cm3 and various values of temperature .

Page 430

5 - o t 26 20 E ( MeV ) Fig . 31 . - Neutrino

energy ( MeV ) . Notice that for low energies the paths calculated including

electron degeneracy effects are much longer than those of Wilson , which did not

include ...

5 - o t 26 20 E ( MeV ) Fig . 31 . - Neutrino

**mean**free path ( cm ) vs . neutrinoenergy ( MeV ) . Notice that for low energies the paths calculated including

electron degeneracy effects are much longer than those of Wilson , which did not

include ...

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### Contents

Gruppo fotografico del partecipanti al Corso | 1 |

Introduction | 17 |

Сen | 37 |

Copyright | |

61 other sections not shown

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### Common terms and phrases

accretion amplitude angular antenna approximation assumed Astrophys binary black hole calculations condition considered cooling core corresponding density depends detailed detectors determined dips discussed disk distance eclipse effect electron emission energy equation estimate existence expected field flux frequency function given gives gravitational heating important increase indicated intensity interesting Journ less Lett light curve limit lines luminosity magnetic field mass matter mean measured momentum motion Nature neutrino neutron star object observed obtained occur optical orbital parameters particle period phase photons Phys physical plasma possible potential present pressure problem pulsations radiation radio radius range region relation relative rotating scale sensitivity shown shows solution spectrum stellar stellar wind suggested surface temperature values variable variations velocity X-ray source