A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae
By using six newly determined mid-eclipse times together with those collected from the literature, we have found that the observed minus calculated (O-C) curve of RR Cae shows a cyclic change with a period of 11.9yr and an amplitude of 14.3 s while it undergoes an upward parabolic variation [reveali...
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| Autores principales: | , , , , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2012
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| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/84385 |
| Aporte de: |
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I19-R120-10915-84385 |
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| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Ciencias Astronómicas Binaries: close Binaries: eclipsing Planetary systems Stars: individual: RR cae White dwarfs |
| spellingShingle |
Ciencias Astronómicas Binaries: close Binaries: eclipsing Planetary systems Stars: individual: RR cae White dwarfs Qian, S. B. Liu, L. Zhu, L. Y. Dai, Z. B. Fernández Lajús, Eduardo Baume, Gustavo A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| topic_facet |
Ciencias Astronómicas Binaries: close Binaries: eclipsing Planetary systems Stars: individual: RR cae White dwarfs |
| description |
By using six newly determined mid-eclipse times together with those collected from the literature, we have found that the observed minus calculated (O-C) curve of RR Cae shows a cyclic change with a period of 11.9yr and an amplitude of 14.3 s while it undergoes an upward parabolic variation [revealing a long-term period increase at a rate of Ṗ = +4.18(±0.20) × 10 -12]. The cyclic change was analysed for the light-travel-time effect that arises from the gravitational influence of a third companion. The mass of the third body was determined to be M 3sin i'= 4.2(± 0.4)M Jup, suggesting that it is a circumbinary giant planet when its orbital inclination is larger than 17°.6. The orbital separation of the circumbinary planet from the central eclipsing binary is about 5.3(± 0.6) au. The period increase is opposite to the changes caused by angular momentum loss via magnetic braking or/and gravitational radiation; and it cannot be explained by the mass transfer between both components because of its detached configuration. These indicate that the observed upward parabolic change is only a part of a long-period (longer than 26.3yr) cyclic variation, which may reveal the presence of another giant circumbinary planet in a wide orbit. |
| format |
Articulo Articulo |
| author |
Qian, S. B. Liu, L. Zhu, L. Y. Dai, Z. B. Fernández Lajús, Eduardo Baume, Gustavo |
| author_facet |
Qian, S. B. Liu, L. Zhu, L. Y. Dai, Z. B. Fernández Lajús, Eduardo Baume, Gustavo |
| author_sort |
Qian, S. B. |
| title |
A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| title_short |
A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| title_full |
A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| title_fullStr |
A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| title_full_unstemmed |
A circumbinary planet in orbit around the short-period white dwarf eclipsing binary RR cae |
| title_sort |
circumbinary planet in orbit around the short-period white dwarf eclipsing binary rr cae |
| publishDate |
2012 |
| url |
http://sedici.unlp.edu.ar/handle/10915/84385 |
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