Zobrazeno 1 - 10
of 34
pro vyhledávání: '"S. W. Hodson"'
Publikováno v:
Journal of Computational Physics. 158:225-238
The need to simulate fully developed turbulence with wide range of scales led us to use the Piecewise Parabolic Method (PPM) to solve the Euler equations of motions. To obtain data for 3-D homogeneous compressible decaying turbulence numerical simula
Publikováno v:
Nonradial and Nonlinear Stellar Pulsation ISBN: 9783540099949
A discussion of the long period R Coronae Borealis stars is presented. The constraints on theoretical models imposed by their age, kinematics and distribution led to difficulties in formulating an evolutionary sequence to the formation of this type o
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::08b44ae04cbd332721c8593892f801cd
https://doi.org/10.1007/3-540-09994-8_14
https://doi.org/10.1007/3-540-09994-8_14
Autor:
A. N. Cox, S. W. Hodson
Publikováno v:
Nonradial and Nonlinear Stellar Pulsation ISBN: 9783540099949
Using results from earlier studies of double-mode dwarf Cepheids by Cox, King and Hodson (1979), hydrodynamic calculations have been undertaken for AI Vel. The evolution theory mass of 1.8 M⊙ previously derived, together with a luminosity of 23 L
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::a5e1fa518e5ad35cc29be609a6411685
https://doi.org/10.1007/3-540-09994-8_4
https://doi.org/10.1007/3-540-09994-8_4
Autor:
A. N. Cox, S. W. Hodson
Publikováno v:
Nonradial and Nonlinear Stellar Pulsation ISBN: 9783540099949
Using the von Sengbusch-Stellingwerf relaxation method, hydrodynamic calculations have been made to find strictly periodic solutions for the fundamental mode pulsations of 7 M⊙ models. These models have a helium enrichment in the surface convection
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::3c1bf5603feb46aac3664f3bffba540e
https://doi.org/10.1007/3-540-09994-8_3
https://doi.org/10.1007/3-540-09994-8_3
Publikováno v:
Nonradial and Nonlinear Stellar Pulsation ISBN: 9783540099949
White dwarf pulsators (ZZ Ceti variables) occur in the extension of the radial pulsation envelope ionization instability strip to the observed luminosities of 3 × 10−3 L⊙ according to van Horn (1979). Investigations have been underway to see if
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::93c46cc831e9bb4b8cabe1332f6be06f
https://doi.org/10.1007/3-540-09994-8_42
https://doi.org/10.1007/3-540-09994-8_42
Autor:
William P. Dannevik, Ronald H. Cohen, David H. Porter, B. C. Curtis, Igor Sytine, S. W. Hodson, Karl-Heinz A. Winkler, Arthur A. Mirin, D. E. Eliason, Paul R. Woodward, Sarah E. Anderson, Andris Dimits
Publikováno v:
Computational Fluid Dynamics.
The steadily increasing power of supercomputing systems is enabling very high resolution simulations of compressible, turbulent flows in the high Reynolds number limit, which is of interest in astrophysics as well as in several other fluid dynamical
Autor:
Arthur N. Cox, S. W. Hodson
Publikováno v:
Symposium - International Astronomical Union. 80:237-240
Mapping of the Cepheid region of the Hertzsprung-Russell diagram has been difficult to do from a theoretical viewpoint because the masses and compositions of the Cepheids have always been very uncertain. It now appears that the various mass anomalies
Autor:
Arthur N. Cox, S. W. Hodson
Publikováno v:
International Astronomical Union Colloquium. 58:323-327
The best known β Cephei variable is a α Virginis (Spica) because it is a binary star (P = 4.01 days) and has a interferometer measurement of its angular diameter. In this study to see if the pulsations can be caused by mixing of hydrogen and helium
Publikováno v:
Physics Today. 40:28-37
In a series of talks in 1946, John von Neumann envisioned the use of high‐speed computers to generate solutions to nonlinear problems, particularly in fluid dynamics. He pointed out that scientists were conducting expensive and difficult experiment
Publikováno v:
International Astronomical Union Colloquium. 58:621-626
A completely new kind of variable star has recently been discovered (McGraw, et. al. 1979). Designated as PG1159-035 (hereafter PG) this star is distinguished not only by the complete lack of hydrogen in its spectrum but also by an effective temperat