So close, so different: characterization of the K2-36 planetary system with HARPS-N

Abstract

K2-36 is a K dwarf orbited by two small ($R_{\mathrm{b}}=1.43\pm 0.08$ $R_{\oplus }$ and $R_{\mathrm{c}}=3.2\pm 0.3$ $R_{\oplus }$), close-in ($a_{\mathrm{b}}$=0.022 AU and $a_{\mathrm{c}}$=0.054 AU) transiting planets discovered by Kepler/K2. They are representatives of two families of small planets ($R_{\mathrm{p}}$<4 $R_{\oplus }$) recently emerged from the analysis of Kepler data, with likely a different structure, composition and evolutionary pathways. We revise the fundamental stellar parameters and the sizes of the planets, and provide the first measurement of their masses and bulk densities, which we use to infer their structure and composition. We observed K2-36 with the HARPS-N spectrograph over $\sim$3.5 years, collecting 81 useful radial velocity measurements. The star is active, with evidence for increasing levels of magnetic activity during the observing time span. The radial velocity scatter is $\sim$17 \ms due to the stellar activity contribution, which is much larger that the semi-amplitudes of the planetary signals. We tested different methods for mitigating the stellar activity contribution to the radial velocity time variations and measuring the planet masses with good precision. We found that K2-36 is likely a $\sim$1 Gyr old system, and by treating the stellar activity through a Gaussian process regression, we measured the planet masses $m_{\mathrm{b}}$=3.9$\pm$1.1 $M_{\oplus }$ and $m_{\mathrm{c}}$=7.8$\pm$2.3 $M_{\oplus }$. The derived planet bulk densities ${\rho }_{\mathrm{b}}$=7.2${}_{-2.1}^{+2.5}$ $g/c{m}^3$ and ${\rho }_{\mathrm{c}}$=1.3${}_{-0.5}^{+0.7}$ $g/c{m}^3$ point out that K2-36\,b has a rocky, Earth-like composition, and K2-36\,c is a low-density sub-Neptune. Composed of two planets with similar orbital separations but different densities, K2-36 represents an optimal laboratory for testing the role of the atmospheric escape in driving the evolution of close-in, low-mass planets after $\sim$1 Gyr from their formation.

Accepted for publication on Astronomy $\&$ Astrophysics

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