We report new photometric and spectroscopic observations of the K2-99 planetary system. Asteroseismic analysis of the short-cadence light curve from K2's Campaign 17 allows us to refine the stellar properties. We find K2-99 to be significantly smaller than previously thought, with R* = 2.55 +/- 0.02 R-circle dot. The new light curve also contains four transits of K2-99 b, which we use to improve our knowledge of the planetary properties. We find the planet to be a non-inflated warm Jupiter, with R-b = 1.06 +/- 0.01 R-Jup. 60 new radial velocity measurements from HARPS, HARPS-N, and HIRES enable the determination of the orbital parameters of K2-99 c, which were previously poorly constrained. We find that this outer planet has a minimum mass M(c)sin i(c) = 8.4 +/- 0.2 M-Jup, and an eccentric orbit (e(c) = 0.210 +/- 0.009) with a period of 522.2 +/- 1.4 d. Upcoming TESS observations in 2022 have a good chance of detecting the transit of this planet, if the mutual inclination between the two planetary orbits is small.

K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant

Gandolfi, D;Goffo, E;Serrano, LM;
2022-01-01

Abstract

We report new photometric and spectroscopic observations of the K2-99 planetary system. Asteroseismic analysis of the short-cadence light curve from K2's Campaign 17 allows us to refine the stellar properties. We find K2-99 to be significantly smaller than previously thought, with R* = 2.55 +/- 0.02 R-circle dot. The new light curve also contains four transits of K2-99 b, which we use to improve our knowledge of the planetary properties. We find the planet to be a non-inflated warm Jupiter, with R-b = 1.06 +/- 0.01 R-Jup. 60 new radial velocity measurements from HARPS, HARPS-N, and HIRES enable the determination of the orbital parameters of K2-99 c, which were previously poorly constrained. We find that this outer planet has a minimum mass M(c)sin i(c) = 8.4 +/- 0.2 M-Jup, and an eccentric orbit (e(c) = 0.210 +/- 0.009) with a period of 522.2 +/- 1.4 d. Upcoming TESS observations in 2022 have a good chance of detecting the transit of this planet, if the mutual inclination between the two planetary orbits is small.
2022
Inglese
Esperti anonimi
510
4
5035
5049
15
https://academic.oup.com/mnras/article-abstract/510/4/5035/6448480?redirectedFrom=fulltext
planetary systems; planets and satellites: detection; planets and satellites: individual: K2-99 b; planets and satellites: individual: K2-99 c
   GANDOLFI D. - Fondaz.CRT - II tornata 2018 - Rif. 2018.2323 - "Gaseous or rocky? Unveiling the nature of small worlds"
   FONDAZIONE CRT
   Rif. 2018.2323
4 – prodotto già presente in altro archivio Open Access (arXiv, REPEC…)
262
32
Smith, AMS; Breton, SN; Csizmadia, S; Dai, F; Gandolfi, D; García, RA; Howard, AW; Isaacson, H; Korth, J; Lam, KWF; Mathur, S; Nowak, G; Hernández, FP...espandi
info:eu-repo/semantics/article
open
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/1948545
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