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tokens: Batalha et al. 2013 ; Petigura et al. 2013 ). Radial velocity measurements (Weiss Marcy 2014 ) and transit timing variations (Wu Lithwick 2013 ) manifest that the masses of these super-Earths are in the range of 2–20 M ⊕ . The abundance of super-Earths presents a puzzle for the core instability theory. This theory indicates that when a protoplanet reaches super-Earth size, two physical processes make the survival of super-Earths difficult, leading to a planetary “desert” in this size range (Ida Lin 2004 ). Super-Earths excite density waves in protoplanetary disks (PPDs) and give rise to rapid type I migration. This type of migration causes the planet to be engulfed by its host star if the disk inner edge touches the stellar surface. Recent studies have sought various remedies for type I migration (Yu et al. 2011 ; Fung Chiang 2017 ). PPDs are expected to have an inner edge at the stellar magnetosphere (e.g., Long et al. 2005 ). For planets undergoing disk-driven migration, they are expected to pile up near this edge. They stay either at the edge because the gas runs out, inside the edge down to 2:1 resonance because that is where the tidal torque tapers off, or outside the edge because the standing waves generated by wave reflection off the inner edge stall planet migration (Tsang 2011 ). In this paper, we focus on another threat for super-Earths. Super-Earths have low mean density, which suggests that they must be surrounded by gas envelopes (Rogers Seager 2010 ). Since these observed super-Earths are in the range of critical mass, they trigger efficient gas runaway and accumulate massive gas envelopes. They become gas giants. As a result, super-Earths are supposed to be rare. However, Kepler ’s discovery wrecks these predictions. Lee et al. ( 2014 ) proposed a metallicity gradient inside the PPDs or the late assembly of cores to resolve the puzzle of super-Earth formation. Lee Chiang ( 2016 ) stressed that the late core assembly in transitional PPDs is more consistent with observations. In gas-poor environments, gas dynamical friction has weakened to allow proto-cores to stir one another and merge. In addition, this formation scenario ensures that super-Earth cores accrete mass with a few percent envelope mass fraction (EMF). Guillot Showman ( 2002 ) argued that the dissipation of the kinetic energy of the atmospheric wind, driven by intense irradiation, could bury heat inside the planet. Many studies extend this idea to explain the radius anomaly of hot Jupiters (Youdin Mitchell 2010 ; Ginzburg Sari 2015 ; Komacek Youdin 2017 ). These investigations focus on the late evolution after the disk dispersal. Unfortunately, this is invalid for the early evolution of super-Earths because they are still embedded within disks. The irradiation may not penetrate the disk and is not able to bury heat in the exoplanets. However, we note that tidal interactions between the host star and planet can periodically perturb the planet and generate mechanical