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http://hdl.handle.net/2445/134583
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DC Field | Value | Language |
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dc.contributor.author | Tokovinin, Andrei | - |
dc.contributor.author | Corbett, Hank | - |
dc.contributor.author | Fors Aldrich, Octavi | - |
dc.contributor.author | Howard, Ward | - |
dc.contributor.author | Law, Nicholas M. | - |
dc.contributor.author | Moe, Maxwell | - |
dc.contributor.author | Ratzloff, Jeffrey | - |
dc.contributor.author | Walter, Frederick M. | - |
dc.date.accessioned | 2019-06-06T11:27:11Z | - |
dc.date.available | 2019-06-06T11:27:11Z | - |
dc.date.issued | 2018-08-24 | - |
dc.identifier.issn | 0004-6256 | - |
dc.identifier.uri | http://hdl.handle.net/2445/134583 | - |
dc.description.abstract | High-resolution spectroscopy and speckle interferometry reveal the young star HD 86588 as a quadruple system with a three-tier hierarchy. The 0 3 resolved binary A,B with an estimated period around 300 years contains the 8-yr pair Aa,Abc (also potentially resolvable), where Ab,Ac is a double-lined binary with equal components, for which we compute the spectroscopic orbit. Despite the short period of 2.4058 days, the orbit of Ab,Ac is eccentric (e=0.086±0.003)). It has a large inclination, but there are no eclipses; only a 4.4 mmag light modulation apparently caused by star spots on the components of this binary is detected with Evryscope. Assuming a moderate extinction of AV=0.5 mag and a parallax of 5.2 mas, we find that the stars are on or close to the main sequence (age >10 Myr) and their masses are from 1 to 1.3 solar. We measure the strength of the lithium line in the visual secondary B which, together with rotation, suggests that the system is younger than 150 Myr. This object is located behind the extension of the Chamaeleon I dark cloud (which explains extinction and interstellar sodium absorption), but apparently does not belong to it. We propose a scenario where the inner orbit has recently acquired its high eccentricity through dynamical interaction with the outer two components; it is now undergoing rapid tidal circularization on a timescale of ∼1 Myr. Alternatively, the eccentricity could be excited quasi-stationary by the outer component Aa. | - |
dc.format.extent | 9 p. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | Institute of Physics (IOP) | - |
dc.relation.isformatof | Reproducció del document publicat a: https://doi.org/10.3847/1538-3881/aad694 | - |
dc.relation.ispartof | Astronomical Journal, 2018, vol. 156, num. 3, p. 120-128 | - |
dc.relation.uri | https://doi.org/10.3847/1538-3881/aad694 | - |
dc.rights | (c) American Astronomical Society, 2018 | - |
dc.source | Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB)) | - |
dc.subject.classification | Espectroscòpia astronòmica | - |
dc.subject.classification | Interferometria | - |
dc.subject.classification | Estels | - |
dc.subject.other | Astronomical spectroscopy | - |
dc.subject.other | Interferometry | - |
dc.subject.other | Stars | - |
dc.title | Young and Eccentric: The Quadruple System HD 86588 | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 689252 | - |
dc.date.updated | 2019-06-06T11:24:41Z | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB)) |
Files in This Item:
File | Description | Size | Format | |
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689252.pdf | 857.06 kB | Adobe PDF | View/Open |
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