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Title: The Monitor project: JW 380-a 0.26-, 0.15-M-circle dot, pre-main-sequence eclipsing binary in the Orion nebula cluster
Authors: Irwin, J.
Aigrain, S.
Hodgkin, S.
Stassun, K. G.
Hebb, L.
Irwin, M.
Moraux, E.
Bouvier, J.
Alapini, A.
Alexander, R.
Bramich, D. M.
Holtzman, J.
Martin, E. L.
McCaughrean, M. J.
Pont, F.
Verrier, P. E.
Osorio, M. R. Z.
First Published: 11-Sep-2007
Royal Astronomical Society (RAS)
Citation: Monthly Notices of the Royal Astronomical Society, 2007, 380 (2), pp. 541-550
Abstract: We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1σ of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii ofGraphic for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross-correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2–3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass–radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature.
DOI Link: 10.1111/j.1365-2966.2007.12117.x
ISSN: 0035-8711
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2007 the authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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