Secular changes in the orbits of the quadruple system VW LMi
VW LMi is the tightest known quadruple system with 2 + 2 hierarchy. It consists of a W UMa-type eclipsing binary (P12 = 0.477 55 d) and another detached non-eclipsing binary (P34 = 7.93 d) orbiting around a common centre of mass in about P1234 = 355 d. We present new observations of the system exten...
Elmentve itt :
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| Dokumentumtípus: | Cikk |
| Megjelent: |
2020
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| Sorozat: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
494 No. 1 |
| Tárgyszavak: | |
| doi: | 10.1093/mnras/staa699 |
| mtmt: | 31277704 |
| Online Access: | http://publicatio.bibl.u-szeged.hu/39112 |
| Tartalmi kivonat: | VW LMi is the tightest known quadruple system with 2 + 2 hierarchy. It consists of a W UMa-type eclipsing binary (P12 = 0.477 55 d) and another detached non-eclipsing binary (P34 = 7.93 d) orbiting around a common centre of mass in about P1234 = 355 d. We present new observations of the system extending the time baseline to study long-term perturbations in the system and to improve orbital elements. The multidataset modelling of the system (four radial-velocity curves for the components and the timing data) clearly showed an apsidal motion in the non-eclipsing binary at a rate of 4.6 deg yr−1, but no other perturbations. This is consistent with the nearly co-planarity of the outer, 355-d orbit, and the 7.93-d orbit of the non-eclipsing binary. Extensive N-body simulations enabled us to constrain the mutual inclination of the non-eclipsing binary and the outer orbits to j34–1234 < 10 deg. |
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| Terjedelem/Fizikai jellemzők: | 178-189 |
| ISSN: | 0035-8711 |