Refining the Stellar Parameters of τ Ceti: a Pole-on Solar Analog

• Published in: The Astronomical journal 2023-09, Vol.166 (3), p.123
• Main Authors: 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.
• Format: Article
• Language: English
• Subjects: Astronomy; Beam combiners; Constraints; Datasets; Diameters; Extrasolar planets; G dwarf stars; Inclination; Long baseline interferometry; Misalignment; Orbital stability; Parameters; Planet detection; Radial velocity; Rotating disks; Solar analogs; Spectroscopy; Stellar properties; Stellar rotation; System dynamics; Uncertainty
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/ace906

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°).