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

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Page 48

The

types of

surface , the second related to the local stellar atmospheres . The simplest ...

The

**approximation**breaks down when R / R , ~ 1 . Due to the azimuthal ... Twotypes of

**approximations**are commonly made , the first related to the shape of thesurface , the second related to the local stellar atmospheres . The simplest ...

Page 49

Furthermore , this

explained below , is entirely inadequate in discussions of X - ray heating effects .

A somewhat more sophisticated geometrical

Furthermore , this

**approximation**always yields two equal light minima , and , asexplained below , is entirely inadequate in discussions of X - ray heating effects .

A somewhat more sophisticated geometrical

**approximation**is the expansion in ...Page 495

The method employed can be called mean - field

alternatively , a relativistic Hartree

pure vector interaction by ZELDOVICH [ 43 ] , who made an extensive study of

the high ...

The method employed can be called mean - field

**approximation**, or ,alternatively , a relativistic Hartree

**approximation**[ 42 ] . It was first employed for apure vector interaction by ZELDOVICH [ 43 ] , who made an extensive study of

the high ...

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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