Interferometric diameters of five evolved intermediate-mass planet-hosting stars measured with PAVO at the CHARA Array

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  • T. R. White, Georg August Univ Gottingen, University of Gottingen, Inst Astrophys, Max Planck Inst Sonnen Syst Forsch, Max Planck Society, Univ Hawaii, University of Hawaii System, Inst Astron
  • ,
  • D. Huber, Univ Hawaii, University of Hawaii System, Inst Astron, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys, SETI Inst
  • ,
  • A. W. Mann, Columbia Univ, Columbia University, Dept Astron
  • ,
  • L. Casagrande, ARC Ctr Excellence All Sky Astrophys 3 Dimens AST
  • ,
  • S. K. Grunblatt, Univ Hawaii, University of Hawaii System, Inst Astron
  • ,
  • A. B. Justesen
  • V. Silva Aguirre
  • T. R. Bedding, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys
  • ,
  • M. J. Ireland, Australian Natl Univ, Australian National University, Mt Stromlo Observ, Res Sch Astron & Astrophys
  • ,
  • G. H. Schaefer, CHARA Array Georgia State Univ, University System of Georgia, Georgia State University, Mt Wilson Observ
  • ,
  • P. G. Tuthill, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys

Debate over the planet occurrence rates around intermediate-mass stars has hinged on the accurate determination of masses of evolved stars, and has been exacerbated by a paucity of reliable, directly measured fundamental properties for these stars. We present long-baseline optical interferometry of five evolved intermediate-mass (similar to 1.5M(circle dot)) planet-hosting stars using the PAVO beam combiner at the CHARA Array, which we combine with bolometric flux measurements and parallaxes to determine their radii and effective temperatures. Wemeasured the radii and effective temperatures of 6 Lyncis (5.12 +/- 0.16 R-circle dot, 4949 +/- 58 K), 24 Sextantis (5.49 +/- 0.18 R-circle dot, 4908 +/- 65 K), kappa Coronae Borealis (4.77 +/- 0.07 R-circle dot, 4870 +/- 47 K), HR 6817 (4.45 +/- 0.08 R-circle dot, 5013 +/- 59 K), and HR8461 (4.91 +/- 0.12 R-circle dot, 4950 +/- 68 K). We find disagreements of typically 15 per cent in angular diameter and similar to 200K in temperature compared to interferometric measurements in the literature, yet good agreement with spectroscopic and photometric temperatures, concluding that the previous interferometric measurements may have been affected by systematic errors exceeding their formal uncertainties. Modelling based on BaSTI isochrones using various sets of asteroseismic, spectroscopic, and interferometric constraints tends to favour slightly (similar to 15 per cent) lower masses than generally reported in the literature.

OriginalsprogEngelsk
TidsskriftMonthly Notices of the Royal Astronomical Society
Vol/bind477
Nummer4
Sider (fra-til)4403-4413
Antal sider11
ISSN0035-8711
DOI
StatusUdgivet - jul. 2018

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