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

### From inside the book

Results 1-3 of 71

Page 48

The

The

**approximation**breaks down when RR 1 . Due to the azimuthal symmetry , the eclipse duration can be calculated as a function of į from the relation cos 0. = cos 0. ( i = 90 ° ) / sin i . We give in fig .Page 49

Furthermore , this

Furthermore , this

**approximation**always yields two equal light minima , and , as explained below , is entirely inadequate in discussions of X - ray heating effects . A somewhat more sophisticated geometrical**approximation**is the ...Page 495

The method employed can be called mean - field

The method employed can be called mean - field

**approximation**, or , alternatively , a relativistic Hartree**approximation**[ 42 ] . It was first employed for a pure vector interaction by ZELDOvich [ 43 ] , who made an extensive study of ...### What people are saying - Write a review

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### Contents

Why are the stars as they are? | 1 |

Krzeminskis StarCen | 5 |

The theory of degenerate configurations the limiting | 7 |

Copyright | |

64 other sections not shown

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### Common terms and phrases

absorption accretion amplitude analysis antenna approximation assumed Astrophys BAHCALL binary black hole calculated colors considered consistent core corresponding cycle Cyg X-1 density dependence detail detected detectors determined dips discussed disk distance eclipse effect electromagnetic electron emission energy equation estimate existence expected field Figure flux frequency function geometry give given gravitational gravitational collapse important increases indicated intensity interesting Journ less Lett light curve limit lines magnetic mass measurements motion Nature neutron star noise observed obtained occur optical orbital parameters particle period phase Phys position possible potential present primary pulsations pulse radiation radio range ratio region relative rotation scale sensitivity shown shows spectrum stellar stellar wind suggested surface temperature transducer values variable variations velocity X-ray sources