The stellar corona-chromosphere connection - A comprehensive study of X-ray and Ca II IRT fluxes from eROSITA and Gaia

Open Access

Fig. 5

X-ray to bolometric flux ratio as function of the index $R_{IRT}^{'}$ $\[R_{\text {IRT }}^{\prime}\]$ for the VHA sources. For the detected sources, the color scales with the logarithm of the G_BP − G_RP color (same as in Fig. 4) and the upper limits are indicated by the black triangles. The black solid line represents the best fit of Fig. 4.

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