dc.creator |
Gruberbauer, Michael |
|
dc.creator |
Balona, L. A. |
|
dc.creator |
Cunha, M. S. |
|
dc.creator |
Kurtz, D. W. |
|
dc.creator |
Saio, H. |
|
dc.creator |
White, T. R. |
|
dc.creator |
Christensen-Dalsgaard, J. |
|
dc.creator |
Kjeldsen, H. |
|
dc.creator |
Christiansen, J. L. |
|
dc.creator |
Hall, J. R. |
|
dc.date.accessioned |
2014-11-18T18:53:53Z |
|
dc.date.available |
2014-11-18T18:53:53Z |
|
dc.date.issued |
2011 |
|
dc.identifier.issn |
0035-8711 |
|
dc.identifier.issn |
1365-2966 |
|
dc.identifier.uri |
http://library2.smu.ca/xmlui/handle/01/25914 |
|
dc.description |
Publisher's version/PDF |
en_CA |
dc.description.abstract |
Photometry of KIC 10483436 was obtained continuously with 1-min exposures over a 27-d period from the Kepler satellite. The light curve shows rotational variations from surface spots with a period of 4.303 [plus or minus] 0.002 d, an amplitude of about 6 mmag and eight pulsation frequencies typical of roAp stars. The high-frequency pattern consists of a quintuplet of equally spaced peaks where the frequency of the dominant central peak (68 [micro]mag amplitude) is 1353.00 [micro]Hz (P = 12.32 min). A second set of three peaks of lower amplitude are also visible. These appear to form part of a quintuplet centred on 1511.6 [micro]Hz with the central peak and one side peak missing. The equidistant frequency spacing is 2.69 [micro]Hz, which corresponds to the 4.303 d rotation period. However, the amplitudes (12 [micro]mag) of these peaks are too close to the detection level to allow definite identification of the multiplets. Although no spectrum is available, the character of the pulsations shows that this is a roAp star with two high-frequency modes modulated in amplitude in accordance with the oblique pulsator model. The 4.303-d variation in the light curve, which is interpreted as rotational modulation, shows harmonics as high as the 26th. These harmonics are probably a result of many patches of varying surface brightness associated with surface abundance variations characteristic of Ap stars. |
en_CA |
dc.description.provenance |
Submitted by Janine Mills (janine.mills@smu.ca) on 2014-11-18T18:53:53Z
No. of bitstreams: 1
Gruberbauer_Michael_article_2011_a.pdf: 6280164 bytes, checksum: c233d1e000fd07ea117c31866a290eba (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2014-11-18T18:53:53Z (GMT). No. of bitstreams: 1
Gruberbauer_Michael_article_2011_a.pdf: 6280164 bytes, checksum: c233d1e000fd07ea117c31866a290eba (MD5)
Previous issue date: 2011 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
Oxford University Press |
en_CA |
dc.relation.uri |
http://dx.doi.org/10.1111/j.1365-2966.2011.18334.x |
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dc.subject.lcsh |
Ap stars |
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dc.subject.lcsh |
Peculiar stars |
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dc.subject.lcsh |
Pulsating stars |
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dc.title |
Rotation and oblique pulsation in Kepler observations of the roAp star KIC 10483436 |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Monthly Notices of the Royal Astronomical Society 413, 2651-2657. (2011) |
en_CA |