THE AGE of the DIRECTLY IMAGED PLANET HOST STAR κ ANDROMEDAE DETERMINED from INTERFEROMETRIC OBSERVATIONS

Jeremy Jones; R. J. White; S. Quinn; M. Ireland; T. Boyajian; G. Schaefer; E. K. Baines

doi:10.3847/2041-8205/822/1/L3

THE AGE of the DIRECTLY IMAGED PLANET HOST STAR κ ANDROMEDAE DETERMINED from INTERFEROMETRIC OBSERVATIONS

Jeremy Jones, R. J. White, S. Quinn, M. Ireland, T. Boyajian, G. Schaefer, E. K. Baines

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Abstract

κ Andromedae, an early-type star that hosts a directly imaged low-mass companion, is expected to be oblate due to its rapid rotational velocity (v sin i = ∼162 km s^-1). We observed the star with the CHARA Array's optical beam combiner, PAVO, measuring its size at multiple orientations and determining its oblateness. The interferometric measurements, combined with photometry and this v sin i value are used to constrain an oblate star model that yields the fundamental properties of the star and finds a rotation speed that is ∼85% of the critical rate and a low inclination of ∼30°. Three modeled properties (the average radius, bolometric luminosity, and equatorial velocity) are compared to MESA evolution models to determine an age and mass for the star. In doing so, we determine an age for the system of Myr. Based on this age and previous measurements of the companion's temperature, the BHAC15 evolution models imply a mass for the companion of M _J.

Original language	English
Article number	L3
Journal	Astrophysical Journal Letters
Volume	822
Issue number	1
DOIs	https://doi.org/10.3847/2041-8205/822/1/L3
Publication status	Published - 1 May 2016

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title = "THE AGE of the DIRECTLY IMAGED PLANET HOST STAR κ ANDROMEDAE DETERMINED from INTERFEROMETRIC OBSERVATIONS",

abstract = "κ Andromedae, an early-type star that hosts a directly imaged low-mass companion, is expected to be oblate due to its rapid rotational velocity (v sin i = ∼162 km s-1). We observed the star with the CHARA Array's optical beam combiner, PAVO, measuring its size at multiple orientations and determining its oblateness. The interferometric measurements, combined with photometry and this v sin i value are used to constrain an oblate star model that yields the fundamental properties of the star and finds a rotation speed that is ∼85% of the critical rate and a low inclination of ∼30°. Three modeled properties (the average radius, bolometric luminosity, and equatorial velocity) are compared to MESA evolution models to determine an age and mass for the star. In doing so, we determine an age for the system of Myr. Based on this age and previous measurements of the companion's temperature, the BHAC15 evolution models imply a mass for the companion of M J.",

keywords = "planetary systems, stars: early-type, stars: evolution, stars: individual (kappa Andromedae), stars: rotation, techniques: interferometric",

author = "Jeremy Jones and White, {R. J.} and S. Quinn and M. Ireland and T. Boyajian and G. Schaefer and Baines, {E. K.}",

year = "2016",

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doi = "10.3847/2041-8205/822/1/L3",

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T1 - THE AGE of the DIRECTLY IMAGED PLANET HOST STAR κ ANDROMEDAE DETERMINED from INTERFEROMETRIC OBSERVATIONS

AU - Jones, Jeremy

AU - White, R. J.

AU - Quinn, S.

AU - Ireland, M.

AU - Boyajian, T.

AU - Schaefer, G.

AU - Baines, E. K.

PY - 2016/5/1

Y1 - 2016/5/1

N2 - κ Andromedae, an early-type star that hosts a directly imaged low-mass companion, is expected to be oblate due to its rapid rotational velocity (v sin i = ∼162 km s-1). We observed the star with the CHARA Array's optical beam combiner, PAVO, measuring its size at multiple orientations and determining its oblateness. The interferometric measurements, combined with photometry and this v sin i value are used to constrain an oblate star model that yields the fundamental properties of the star and finds a rotation speed that is ∼85% of the critical rate and a low inclination of ∼30°. Three modeled properties (the average radius, bolometric luminosity, and equatorial velocity) are compared to MESA evolution models to determine an age and mass for the star. In doing so, we determine an age for the system of Myr. Based on this age and previous measurements of the companion's temperature, the BHAC15 evolution models imply a mass for the companion of M J.

AB - κ Andromedae, an early-type star that hosts a directly imaged low-mass companion, is expected to be oblate due to its rapid rotational velocity (v sin i = ∼162 km s-1). We observed the star with the CHARA Array's optical beam combiner, PAVO, measuring its size at multiple orientations and determining its oblateness. The interferometric measurements, combined with photometry and this v sin i value are used to constrain an oblate star model that yields the fundamental properties of the star and finds a rotation speed that is ∼85% of the critical rate and a low inclination of ∼30°. Three modeled properties (the average radius, bolometric luminosity, and equatorial velocity) are compared to MESA evolution models to determine an age and mass for the star. In doing so, we determine an age for the system of Myr. Based on this age and previous measurements of the companion's temperature, the BHAC15 evolution models imply a mass for the companion of M J.

KW - planetary systems

KW - stars: early-type

KW - stars: evolution

KW - stars: individual (kappa Andromedae)

KW - stars: rotation

KW - techniques: interferometric

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DO - 10.3847/2041-8205/822/1/L3

M3 - Article

SN - 2041-8205

VL - 822

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L3

ER -

THE AGE of the DIRECTLY IMAGED PLANET HOST STAR κ ANDROMEDAE DETERMINED from INTERFEROMETRIC OBSERVATIONS

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