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Context. The exoplanet K2-18 b lies near the radius valley that separates super-Earths and sub-Neptunes, marking a key transitional regime in planetary and atmospheric composition. The system offers a valuable opportunity to study how M-dwarf high-energy stellar radiation influences atmospheric stability and the potential for sustaining volatile species, which is especially important in the context of the upcoming ELT and its ANDES spectrograph. Aims. This study characterizes the high-energy environment of K2-18 with X-ray observations from eROSITA, the soft X-ray instrument on the Spectrum-Roentgen-Gamma mission, Chandra , and XMM-Newton . Methods. We derived a representative 0.2–2 keV X-ray flux with an APEC thermal plasma model fit with the Bayesian X-ray Analysis (BXA). With the observed X-ray flux from the exoplanet host star, we estimated the photoevaporative mass loss of exoplanet K2-18b using the energy-limited model. In addition, we examined the thermal structure of the system based on a hydrodynamic model. Results. In a 100 ks XMM-Newton observation, we identified K2-18 as a very faint X-ray source with F X = 10 −15 erg s −1 cm −2 and an activity level of (Lx/Lbol) ∼10 −5 . A small flare was detected during the observation. The planet is irradiated by an X-ray flux of F pl , X = 12 ± 3 erg s −1 cm −2 . Conclusions. The X-ray flux measurement of K2-18 gives important limitations for the atmospheric escape and photochemical modeling of its exoplanets. Despite its near orbit around an M-dwarf star, K2-18b’s low-activity-level environment suggests that it can retain an atmosphere, supporting recent tentative detections of atmospheres.
Rukdee et al. (Sun,) studied this question.