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Barnes, J. R.; Standing, M. R.; Haswell, C. A.; Staab, D.; Doherty, J. P. J.; Waller-Bridge, M.; Fossati, L.; Soto, M.; Anglada-Escudé, G.; Llama, J.; McCune, C. and Lewis, F. W.
(2023).
DOI: https://doi.org/10.1093/mnras/stad2109
Abstract
We present radial velocity measurements of the very bright (V ∼ 5.7) nearby F star, DMPP-4 (HD 184960). The anomalously low Ca ii H&K emission suggests mass loss from planets orbiting a low activity host star. Periodic radial velocity variability with ∼10 m s−1 amplitude is found to persist over a > 4 year timescale. Although the non-simultaneous photometric variability in four TESS sectors supports the view of an inactive star, we identify periodic photometric signals and also find spectroscopic evidence for stellar activity. We used a posterior sampling algorithm that includes the number of Keplerian signals, Np, as a free parameter to test and compare (1) purely Keplerian models (2) a Keplerian model with linear activity correlation and (3) Keplerian models with Gaussian processes. A preferred model, with one Keplerian and quasi-periodic Gaussian process indicates a planet with a period of d and corresponding minimum mass of
M⊕. Without further high time resolution observations over a longer timescale, we cannot definitively rule out the purely Keplerian model with 2 candidates planets with
d, minimum mass
M⊕ and
d and corresponding minimum mass of
M⊕. The candidate planets lie in the region below the lower-envelope of the Neptune Desert. Continued mass loss may originate from the highly irradiated planets or from an as yet undetected body in the system.
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