## 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 mean molecular weight , e the

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 the

**density**and T the temperature . The pressure due to radiation , in the same ...Page 398

The temperature rises rapidly until the edge of the convective region approaches

burning soon becomes responsible for determining the change in central

.

The temperature rises rapidly until the edge of the convective region approaches

**densities**at which decay of 23Ne ... The change in composition due to carbonburning soon becomes responsible for determining the change in central

**density**.

Page 498

The energy shift increases with

interaction . The effect is of a general nature and is therefore expected to hold for

any ...

The energy shift increases with

**density**and goes from + 140 to + 400 MeV , in the**density**region 0 . 5 ( N , < 5 ( fm - 3 , even in the absence of a two - bodyinteraction . The effect is of a general nature and is therefore expected to hold for

any ...

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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