dc.creator |
Deupree, Robert G. (Robert Gaston), 1946- |
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dc.creator |
Geroux, Chris M. |
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dc.date.accessioned |
2015-05-06T12:53:25Z |
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dc.date.available |
2015-05-06T12:53:25Z |
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dc.date.issued |
2013-07-10 |
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dc.identifier.issn |
0004-637X |
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dc.identifier.uri |
http://library2.smu.ca/xmlui/handle/01/26097 |
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dc.description |
Publisher's version/PDF |
en_CA |
dc.description.abstract |
We have developed a three-dimensional radiation hydrodynamics code to simulate the interaction of convection and radial pulsation in classical variable stars. One key goal is the ability to carry these simulations to full amplitude in order to compare them with observed light curves. Previous multi-dimensional calculations were prevented from reaching full amplitude because of drift in the radial coordinate system, due to the algorithm defining radial movement of the coordinate system during the pulsation cycle. We have removed this difficulty by defining our radial coordinate flow algorithm to require that the mass in a spherical shell remain constant for every time step throughout the pulsation cycle. We have used our new code to perform two-dimensional (2D) simulations of the interaction of radial pulsation and convection. We have made comparisons between light curves from our 2D convective simulations with observed light curves and find that our 2D simulated light curves are better able to match the observed light curve shape near the red edge of the RR Lyrae instability strip than light curves from previous one-dimensional time-dependent convective models. |
en_CA |
dc.description.provenance |
Submitted by Janine Mills (janine.mills@smu.ca) on 2015-05-06T12:53:25Z
No. of bitstreams: 1
Deupree_Robert_G_article_2013.pdf: 2193512 bytes, checksum: 3058e6182c041125e2c608185dc58f80 (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2015-05-06T12:53:25Z (GMT). No. of bitstreams: 1
Deupree_Robert_G_article_2013.pdf: 2193512 bytes, checksum: 3058e6182c041125e2c608185dc58f80 (MD5)
Previous issue date: 2013-07-10 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
American Astronomical Society |
en_CA |
dc.publisher |
IOP Science |
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dc.relation.uri |
http://dx.doi.org/10.1088/0004-637X/771/2/113 |
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dc.rights |
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user. |
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dc.subject.lcsh |
Convection (Astrophysics) |
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dc.subject.lcsh |
Hydrodynamics |
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dc.subject.lcsh |
Mathematical models |
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dc.subject.lcsh |
Stellar oscillations |
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dc.subject.lcsh |
Variable stars |
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dc.subject.lcsh |
RR Lyrae stars |
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dc.title |
Radial stellar pulsation and three-dimensional convection. II. Two-dimensional convection in full amplitude radial pulsation |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal 771(2), 113. (2013) |
en_CA |
Copyright statement:
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.