Zobrazeno 1 - 10
of 132
pro vyhledávání: '"Arthur N. Cox"'
Autor:
Arthur N. Cox
This new, fourth, edition of Allen's classic Astrophysical Quantities belongs on every astronomer's bookshelf. It has been thoroughly revised and brought up to date by a team of more than ninety internationally renowned astronomers and astrophysicist
Publikováno v:
International Astronomical Union Colloquium. 193:462-465
δ Scuti stars that have been observed intensely by the Delta Scuti Network and other campaigns exhibit fewer modes than predicted in the observed frequency range. In addition, some modes are difficult to match by the most likely observable l = 0, 1,
Autor:
Arthur N. Cox
Publikováno v:
The Astrophysical Journal. 585:975-982
The mechanism that produces pulsations in the hottest pre-white dwarfs has been uncertain since the early work indicated that helium is a poison that smooths opacity bumps in the opacity-temperature plane caused by the ionizations of the large observ
Autor:
Arthur N. Cox
Publikováno v:
International Astronomical Union Colloquium. 185:21-34
Unsolved problems of theoretical stellar pulsations are briefly reviewed for pulsators in six regions of the Hertzsprung-Russell diagram. Only a small selection is included in the discussion of them, and the emphasis is mostly on theoretical problems
Publikováno v:
The Astrophysical Journal. 542:L57-L60
The γ Doradus stars are a newly discovered class of gravity-mode pulsators that lie just at or beyond the red edge of the δ Scuti instability strip. We present the results of calculations that the predict pulsation instability of high-order g-modes
Publikováno v:
International Astronomical Union Colloquium. 169:337-344
Many physical factors, including radial and nonradial pulsation, rotation, radiation pressure, convection, magnetic fields, or dynamical instabilities may play important roles in the hydrodynamics of Luminous Blue Variables. We review the current sta
Autor:
Arthur N. Cox
Publikováno v:
The Astrophysical Journal. 496:246-252
Period changes in RR Lyrae variables and Cepheids, known for more than 60 years, can possibly be explained by small changes in a helium composition gradient below the hydrogen and helium convection zones. The particular cases for the globular cluster