Diversities and similarities exhibited by multi-planetary systems and their architectures - II. Radii of singles and multis

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Table 1

Properties of singles and multis orbiting different types of stars.

Spec. type	T_eff (K)	N_s	N_m	N_s excl. HJs	N_m excl. HJs	${\tilde{R}}_{s} (R_{\oplus})$ $Mathematical equation: $\[\widetilde{R}_{s}~(R_{\oplus})\]$$ excl. HJs	$\tilde{R_{m}} (R_{\oplus})$ $Mathematical equation: $\[\widetilde{R_{m}}~(R_{\oplus})\]$$ excl. HJs
F	5960–6200	239	227	163	226	2.25 ± 0.04	2.26 ± 0.03
G	5325–5960	814	644	621	634	2.36 ± 0.02	2.29 ± 0.02
K	3890–5325	534	526	448	519	2.09 ± 0.02	2.06 ± 0.02
M0-2	3450–3890	87	80	76	80	1.94 ± 0.04	1.64 ± 0.04
M3-9	2310–3450	56	45	48	45	1.53 ± 0.05	1.22 ± 0.03

Notes. N and $\tilde{R}$ $Mathematical equation: $\[\widetilde{R}\]$$ represent the number and the median radii, respectively, of the singles (s) and multis (m). The host stars are divided into five spectral types based on their effective temperatures T_eff. The tabulated uncertainties are computed via Monte Carlo simulations, assuming a Gaussian distribution for the radius of each planet (Sect. 3.3). Spectral types M0-2 and M3-9 correspond to early- and late-type M stars, respectively. The total of planets orbiting F-, G-, and K-type stars comprise the FGK sample analysed in this work. “Excluding hot Jupiters” (excl. HJs) refer to the samples after removing the hot Jupiters (P < 10 days and R > 6 R_⊕).

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