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

### From inside the book

Results 1-3 of 51

Page xxi

A

which the pressure and density of the star ... In both the analysis of the

equilibrium

appeared ...

A

**configuration**of equilibrium then exists , at approximately nuclear densities , inwhich the pressure and density of the star ... In both the analysis of the

equilibrium

**configurations**of white dwarfs , and of neutron stars , a new featureappeared ...

Page 8

Equilibrium

the polytropes of Emden and an equilibrium

26 ) obtains is a polytrope of index 3 . And the theory of polytropes directly leads

...

Equilibrium

**configurations**in which the pressure is a monomial of the density arethe polytropes of Emden and an equilibrium

**configuration**in which the relation (26 ) obtains is a polytrope of index 3 . And the theory of polytropes directly leads

...

Page 10

for M →0 , predicts that the radius tends to zero for M → Milmit ( see fig . 1 ) .

Therefore , finite degenerate equilibrium

and stars more massive than Mlimit « do not have the necessary energy to cool »

.

for M →0 , predicts that the radius tends to zero for M → Milmit ( see fig . 1 ) .

Therefore , finite degenerate equilibrium

**configurations**exist only for M < M limitiand stars more massive than Mlimit « do not have the necessary energy to cool »

.

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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