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http://hdl.handle.net/20.500.12386/24462
Titolo: | Physical parameters and long-term photometric variability of V1481 Ori, an SB2 member of Orion nebula Cluster with an accreting component | Autori: | MESSINA, Sergio Parihar, P. BIAZZO, Katia LANZA, Antonino Francesco DISTEFANO, Elisa Maria Carmela Melo, C. H. F. Bradstreet, D. H. Herbst, W. |
Data pubblicazione: | 2016 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 457 | Fascicolo: | 3 | Da pagina:: | 3372 | Abstract: | We present the results of our analysis on V1481 Ori (JW 239), a young SB2 in the Orion nebula Cluster with a circumbinary disc accreting on the lower mass component. The analysis is based on high-resolution spectroscopic data and high-quality photometric time series about 20-yr long. Thanks to the spectroscopy, we confirm the binary nature of this system consisting of M3 + M4 components and derive the mass ratio M<SUB>B</SUB>/M<SUB>A</SUB> = 0.54, a variable luminosity ratio L<SUB>B</SUB>/L<SUB>A</SUB> = 0.68-0.94, and an orbital period P<SUB>orb</SUB> = 4.433 d. The photometric data allowed us to measure the rotation periods of the two components P<SUB>phot</SUB> = 4.4351 d and they are found to be synchronized with the orbital period. The simultaneous modelling of V-, I-band, and radial velocity curves in the 2005 season suggests that the variability is dominated by one hotspot on the secondary component covering at least ∼3.5 per cent of the stellar surface and about 420 K hotter than the unperturbed photosphere. Such a spot may originate from the material of the circumbinary disc accreting on to the secondary component. We also detect an apparent 6-yr periodic variation in the position of this hotspot, which is inferred from the phase migration of the light-curve maximum, which we interpret as due to either the presence of surface differential rotation as large as 0.065 per cent, a value compatible with the fully convective components, or to a periodic exchange of angular momentum between the disc and the star, which implies a minimum magnetic field strength of 650 G at the stellar surface. | URI: | http://hdl.handle.net/20.500.12386/24462 | URL: | https://academic.oup.com/mnras/article/457/3/3372/2588884 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stv3000 | Bibcode ADS: | 2016MNRAS.457.3372M | Fulltext: | open |
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