Double-mode Cepheids in M31
Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was claimed to show two pulsation modes. We conducted a systematic search for double mode Cepheids in the archival data and discovered four such o...
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| Published in | arXiv.org |
|---|---|
| Main Author | |
| Format | Paper Journal Article |
| Language | English |
| Published |
Ithaca
Cornell University Library, arXiv.org
14.08.2013
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| Subjects | |
| Online Access | Get full text |
| ISSN | 2331-8422 |
| DOI | 10.48550/arxiv.1308.3227 |
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| Abstract | Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was claimed to show two pulsation modes. We conducted a systematic search for double mode Cepheids in the archival data and discovered four such objects. We identify one of the stars as a first and second overtone pulsator even though its secondary period is subject to strong aliasing. Two stars turn out to pulsate in the fundamental mode and the first overtone. Their fundamental periods are 9.392 d and 9.163 d. This makes them the first candidates for the fundamental mode and the first overtone Cepheids, which double mode pulsations are caused by the 1:2 resonance of the fundamental mode and the second overtone. |
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| AbstractList | Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was claimed to show two pulsation modes. We conducted a systematic search for double mode Cepheids in the archival data and discovered four such objects. We identify one of the stars as a first and second overtone pulsator even though its secondary period is subject to strong aliasing. Two stars turn out to pulsate in the fundamental mode and the first overtone. Their fundamental periods are 9.392 d and 9.163 d. This makes them the first candidates for the fundamental mode and the first overtone Cepheids, which double mode pulsations are caused by the 1:2 resonance of the fundamental mode and the second overtone. Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was claimed to show two pulsation modes. We conducted a systematic search for double mode Cepheids in the archival data and discovered four such objects. We identify one of the stars as a first and second overtone pulsator even though its secondary period is subject to strong aliasing. Two stars turn out to pulsate in the fundamental mode and the first overtone. Their fundamental periods are 9.392 d and 9.163 d. This makes them the first candidates for the fundamental mode and the first overtone Cepheids, which double mode pulsations are caused by the 1:2 resonance of the fundamental mode and the second overtone. |
| Author | Poleski, Radosław |
| Author_xml | – sequence: 1 givenname: Radosław surname: Poleski fullname: Poleski, Radosław |
| BackLink | https://doi.org/10.48550/arXiv.1308.3227$$DView paper in arXiv https://doi.org/10.1088/0004-637X/778/2/147$$DView published paper (Access to full text may be restricted) |
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| DOI | 10.48550/arxiv.1308.3227 |
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| Snippet | Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was... Until now, double mode Cepheids (or beat Cepheids) were known in the Galaxy, Magellanic Clouds and M33. Curiously, none of more than 2000 Cepheids in M31 was... |
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| SubjectTerms | Aliasing Cepheid variables Galaxies Magellanic clouds Physics - Solar and Stellar Astrophysics Spiral galaxies |
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| Title | Double-mode Cepheids in M31 |
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