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

### From inside the book

Results 1-3 of 85

Page 318

14 and Yo = ( 1 - 2 M / r ) dt / dt

particle at infinite distance from the black hole . The boundary conditions and the

formulae to compute the energy fluxes are the same as the ones given in fig . 14 .

14 and Yo = ( 1 - 2 M / r ) dt / dt

**gives**a measure of the kinetic energy of theparticle at infinite distance from the black hole . The boundary conditions and the

formulae to compute the energy fluxes are the same as the ones given in fig . 14 .

Page 383

The first equation ensures mass conservation , the second equation is for charge

conservation , and the third

relation to the abundances of the free protons and neutrons . The quantity Y .

The first equation ensures mass conservation , the second equation is for charge

conservation , and the third

**gives**the equilibrium abundance of each nucleus inrelation to the abundances of the free protons and neutrons . The quantity Y .

Page 594

Above po , a variational procedure is employed to determine which equation of

state

causality ( dp / do < 1 ) and local stability of matter ( dp / do > 0 ) . The variational

...

Above po , a variational procedure is employed to determine which equation of

state

**gives**the biggest contribution to the mass with the only constraints ofcausality ( dp / do < 1 ) and local stability of matter ( dp / do > 0 ) . The variational

...

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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