The HD 137496 system: A dense, hot super-Mercury and a cold Jupiter

Abstract

Most of the currently known planets are small worlds with radii between that of the Earth and that of Neptune. The characterization of planets in this regime shows a large diversity in compositions and system architectures, with distributions hinting at a multitude of formation and evolution scenarios. Using photometry from the K2 satellite and radial velocities measured with the HARPS and CORALIE spectrographs, we searched for planets around the bright and slightly evolved Sun-like star HD 137496. We precisely estimated the stellar parameters, $M_{\ast }$ = 1.035 +/- 0.022 $M_{\odot }$, $R_{\ast }$ = 1.587 +/- 0.028 $R_{\odot }$, $T_{\text{eff}}$ = 5799 +/- 61 K, together with the chemical composition of the slightly evolved star. We detect two planets orbiting HD 137496. The inner planet, HD 137496 b, is a super-Mercury (an Earth-sized planet with the density of Mercury) with a mass of $M_b$ = 4.04 +/- 0.55 $M_{\oplus }$, a radius of $R_b=1.31_{-0.05}^{+0.06}{R}_{\oplus },$ and a density of ${\rho }_b=10.49_{-1.82}^{+2.08}$ $\mathrm{gc}{\mathrm{m}}^{-3}$. With an interior modeling analysis, we find that the planet is composed mainly of iron, with the core representing over 70% of the planet's mass ($M_{core}/M_{total}=0.73_{-0.12}^{+0.11}$). The outer planet, HD 137496 c, is an eccentric ($e$ = 0.477 +/- 0.004), long period ($P$ = $479.9_{-1.1}^{+1.0}$ days) giant planet ($M_c\sin i_c$ = 7.66 +/- 0.11 $M_{Jup}$) for which we do not detect a transit. HD 137496 b is one of the few super-Mercuries detected to date. The accurate characterization reported here enhances its role as a key target to better understand the formation and evolution of planetary systems. The detection of an eccentric long period giant companion also reinforces the link between the presence of small transiting inner planets and long period gas giants.

arXiv comment20 pages, 14 figures, 10 tables. To be published in A&A

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