Journal
ASTROPHYSICAL JOURNAL
Volume 785, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/785/2/83
Keywords
binaries: eclipsing; stars: early-type; stars: formation; stars: individual (CV Velorum, DI Herculis, EP Crucis); stars: kinematics and dynamics; stars: rotation; techniques: spectroscopic
Categories
Funding
- Rubicon fellowship from the Netherlands Organisation for Scientific Research (NWO)
- NASA Origins award [NNX09AB33G]
- NSF [1108595]
- Belgian Fund for Scientific Research (FNRS)
- Swiss National Science Fundation (SNF)
- Swiss National Science Foundation [PBGEP2-14559]
- STFC [ST/J00152X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/J00152X/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1007992, 1108595] Funding Source: National Science Foundation
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As part of the Binaries Are Not Always Neatly Aligned project (BANANA), we have found that the eclipsing binary CV Velorum has misaligned rotation axes. Based on our analysis of the Rossiter-McLaughlin effect, we find sky-projected spin-orbit angles of beta(p) = -52 degrees +/- 6 degrees and beta(s) = 3 degrees +/- 7 degrees for the primary and secondary stars (B2.5V + B2.5V, P = 6.9 days). We combine this information with several measurements of changing projected stellar rotation speeds (v sin i(star)) over the last 30 yr, leading to a model in which the primary star's obliquity is approximate to 65 degrees, and its spin axis precesses around the total angular momentum vector with a period of about 140 yr. The geometry of the secondary star is less clear, although a significant obliquity is also implicated by the observed time variations in the v sin i(star). By integrating the secular tidal evolution equations backward in time, we find that the system could have evolved from a state of even stronger misalignment similar to DI Herculis, a younger but otherwise comparable binary.
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