St Andrews Research Repository

St Andrews University Home
View Item 
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  • Login
JavaScript is disabled for your browser. Some features of this site may not work without it.

The EBLM Project VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey

Thumbnail
View/Open
Gill_2018_ELBM_Project_VI_AA_A119.pdf (2.221Mb)
Date
06/2019
Author
Gill, S.
Maxted, P. F. L.
Southworth, J.
Smalley, B.
Gary, B. L.
Anderson, D. R.
Bouchy, F.
Cameron, A. C.
Dominik, M.
Faedi, F.
Gillon, M.
Gomez Maqueo Chew, Y.
Hebb, L.
Hellier, C.
Jørgensen, U. G.
Longa-Peña, P.
Martin, D. V.
McCormac, J.
Pepe, F. V.
Pollaco, D.
Queloz, D.
Ségransan, D.
Snodgrass, C.
Turner, O. D.
Triaud, A. H. M.
Udry, S.
Snodgrass, R. G. West
Turner, O. D.
Triaud, A. H. M.
Udry, S.
West, R. G.
Keywords
Binaries: eclipsing
Stars: atmospheres
QB Astronomy
QC Physics
3rd-DAS
Metadata
Show full item record
Altmetrics Handle Statistics
Altmetrics DOI Statistics
Abstract
Some M-dwarfs around F-/G-type stars have been measured to be hotter and larger than predicted by stellar evolution models. Inconsistencies between observations and models need to be addressed with more mass, radius, and luminosity measurements of low-mass stars to test and refine evolutionary models. Our aim is to measure the masses, radii and ages of the stars in five low-mass eclipsing binary systems discovered by the WASP survey. We used WASP photometry to establish eclipse-time ephemerides and to obtain initial estimates for the transit depth and width. Radial velocity measurements were simultaneously fitted with follow-up photometry to find the best-fitting orbital solution. This solution was combined with measurements of atmospheric parameters to interpolate evolutionary models and estimate the mass of the primary star, and the mass and radius of the M-dwarf companion. We assess how the best fitting orbital solution changes if an alternative limb-darkening law is used and quantify the systematic effects of unresolved companions. We also gauge how the best-fitting evolutionary model changes if different values are used for the mixing length parameter and helium enhancement. We report the mass and radius of five M-dwarfs and find little evidence of inflation with respect to evolutionary models. The primary stars in two systems are near the “blue hook” stage of their post sequence evolution, resulting in two possible solutions for mass and age. We find that choices in helium enhancement and mixing-length parameter can introduce an additional 3−5% uncertainty in measured M-dwarf mass. Unresolved companions can introduce an additional 3−8% uncertainty in the radius of an M-dwarf, while the choice of limb-darkening law can introduce up to an additional 2% uncertainty. The choices in orbital fitting and evolutionary models can introduce significant uncertainties in measurements of physical properties of such systems.
Citation
Gill , S , Maxted , P F L , Southworth , J , Smalley , B , Gary , B L , Anderson , D R , Bouchy , F , Cameron , A C , Dominik , M , Faedi , F , Gillon , M , Gomez Maqueo Chew , Y , Hebb , L , Hellier , C , Jørgensen , U G , Longa-Peña , P , Martin , D V , McCormac , J , Pepe , F V , Pollaco , D , Queloz , D , Ségransan , D , Snodgrass , C , Turner , O D , Triaud , A H M , Udry , S , Snodgrass , R G W , Turner , O D , Triaud , A H M , Udry , S & West , R G 2019 , ' The EBLM Project VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey ' , Astronomy & Astrophysics , vol. 626 , A119 . https://doi.org/10.1051/0004-6361/201833054
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201833054
ISSN
0004-6361
Type
Journal article
Rights
© 2018, ESO. This work has been made available online in accordance with the publisher's policies. This is the final published version of the work, which was originally published at https://doi.org/10.1051/0004-6361/201833054
Description
Funding: Science and Technology Facilities Council ST/N50434/1, ST/M001040/1, ST/N504348/1 and ST/P000495/1 (SG, PM, JE); European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement n◦ 803193/BEBOP).
Collections
  • University of St Andrews Research
URL
http://arxiv.org/abs/1904.12695v1
URI
http://hdl.handle.net/10023/18014

Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.

Advanced Search

Browse

All of RepositoryCommunities & CollectionsBy Issue DateNamesTitlesSubjectsClassificationTypeFunderThis CollectionBy Issue DateNamesTitlesSubjectsClassificationTypeFunder

My Account

Login

Open Access

To find out how you can benefit from open access to research, see our library web pages and Open Access blog. For open access help contact: openaccess@st-andrews.ac.uk.

Accessibility

Read our Accessibility statement.

How to submit research papers

The full text of research papers can be submitted to the repository via Pure, the University's research information system. For help see our guide: How to deposit in Pure.

Electronic thesis deposit

Help with deposit.

Repository help

For repository help contact: Digital-Repository@st-andrews.ac.uk.

Give Feedback

Cookie policy

This site may use cookies. Please see Terms and Conditions.

Usage statistics

COUNTER-compliant statistics on downloads from the repository are available from the IRUS-UK Service. Contact us for information.

© University of St Andrews Library

University of St Andrews is a charity registered in Scotland, No SC013532.

  • Facebook
  • Twitter