http://arxiv.org/abs/2211.02547
We used TESS light curves and HARPS-N spectrograph radial velocity measurements to establish the physical properties of the transiting exoplanet candidate found around the star HD 20329 (TOI-4524). We performed a joint fit of the light curves and radial velocity time series to measure the mass, radius, and orbital parameters of the candidate. We confirm and characterize HD 20329b, an ultra-short-period (USP) planet transiting a solar-type star. The host star (HD 20329, $V = 8.74$ mag, $J = 7.5$ mag) is characterized by its G5 spectral type with $\mathrm{M}\star= 0.90 \pm 0.05$ M$\odot$, $\mathrm{R}\star = 1.13 \pm 0.02$ R$\odot$, and $\mathrm{T}{\mathrm{eff}} = 5596 \pm 50$ K; it is located at a distance $d= 63.68 \pm 0.29$ pc. By jointly fitting the available TESS transit light curves and follow-up radial velocity measurements, we find an orbital period of $0.9261 \pm (0.5\times 10^{-4})$ days, a planetary radius of $1.72 \pm 0.07$ $\mathrm{R}\oplus$, and a mass of $7.42 \pm 1.09$ $\mathrm{M}\oplus$, implying a mean density of $\rho\mathrm{p} = 8.06 \pm 1.53$ g cm$^{-3}$. HD 20329b joins the $\sim$30 currently known USP planets with radius and Doppler mass measurements.
F. Murgas, G. Nowak, T. Masseron, et. al.
Mon, 7 Nov 22
59/67
Comments: Accepted for publication in A&A, 26 pages
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