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Korolik, Maria; Roettenbacher, Rachael M.; Fischer, Debra A.; Kane, Stephen R.; Perkins, Jean M.; Monnier, John D.; Davies, Claire L.; Kraus, Stefan; Le Bouquin, Jean-Baptiste; Anugu, Narsireddy; Gardner, Tyler; Lanthermann, Cyprien; Schaefer, Gail H.; Setterholm, Benjamin; Brewer, John M.; Llama, Joe; Zhao, Lily L.; Szymkowiak, Andrew E.; Henry, Gregory W.
The Astronomical journal, 09/2023, Letnik: 166, Številka: 3Journal Article
Abstract To accurately characterize the planets a star may be hosting, stellar parameters must first be well determined. τ Ceti is a nearby solar analog and often a target for exoplanet searches. Uncertainties in the observed rotational velocities have made constraining τ Ceti’s inclination difficult. For planet candidates from radial velocity (RV) observations, this leads to substantial uncertainties in the planetary masses, as only the minimum mass ( m sin i ) can be constrained with RV. In this paper, we used new long-baseline optical interferometric data from the CHARA Array with the MIRC-X beam combiner and extreme precision spectroscopic data from the Lowell Discovery Telescope with EXPRES to improve constraints on the stellar parameters of τ Ceti. Additional archival data were obtained from a Tennessee State University Automatic Photometric Telescope and the Mount Wilson Observatory HK project. These new and archival data sets led to improved stellar parameter determinations, including a limb-darkened angular diameter of 2.019 ± 0.012 mas and rotation period of 46 ± 4 days. By combining parameters from our data sets, we obtained an estimate for the stellar inclination of 7° ± 7°. This nearly pole-on orientation has implications for the previously reported exoplanets. An analysis of the system dynamics suggests that the planetary architecture described by Feng et al. may not retain long-term stability for low orbital inclinations. Additionally, the inclination of τ Ceti reveals a misalignment between the inclinations of the stellar rotation axis and the previously measured debris disk rotation axis ( i disk = 35° ± 10°).
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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