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Fig. 2

image

Comparison between the optical and X-rays flux variability, calculated using Eq. (1), shown separately for the stars with transition disks and Class III objects (upper panels) and stars with inner disks, both passive and accreting (lower panels). Note the different y-axis scaling for the top and bottom rows. X-ray photons are selected in the broad-band (0.5−8 keV; left panels), soft band (0.5−1.5 keV; central panels), and hard band (1.5−8 keV; right panels). In each panel, the null-hypothesis probabilities of no correlation resulting from the Spearman (ρ) and Kendall (τ) rank correlation test are shown. Each point corresponds to the variability observed between two consecutive given Chandra frames for each source. The total number of stars and points used in each plot is also indicated.

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