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K2-19 hosts a planetary system composed of two outer planets, b and c, withsize of $7.0\pm 0.2~R_\oplus$ and $4.1\pm0.2~R_\oplus$ , and an inner planet,d, with a radius of $1.11\pm 0.05 R_\oplus$. A recent analysis ofTransit-Timing Variations (TTVs) suggested b and c are close to but not in 3:2mean motion resonance (MMR) because the classical resonant angles circulate.Such an architecture challenges our understanding of planet formation. Indeed,planet migration through the protoplanetary disk should lead to a capture intothe MMR. Here, we show that the planets are in fact, locked into the 3:2resonance despite circulation of the conventional resonant angles and alignedperiapses. However, we show that such an orbital configuration cannot bemaintained for more than a few hundred million years due to the tidaldissipation experienced by planet d. The tidal dissipation remains efficientbecause of a secular forcing of the innermost planet eccentricity by planets band c. While the observations strongly rule out an orbital solution where thethree planets are on close to circular orbits, it remains possible that afourth planet is affecting the TTVs such that the four planet system isconsistent with the tidal constraints.

Resonance in the K2-19 system is at odds with its high reported eccentricities