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The Si I 6560.58 \r{A} line in the H$\alpha$ blue wing is blended with atelluric absorption line from water vapor in ground-based observations. Recentobservations with the space-based telescope CHASE provide a new window to studythis line. We aim to study the Si I line statistically and to explore possiblediagnostics. We select three scannings in the CHASE observations, and measurethe equivalent width (EW) and the full width at half maximum (FWHM) for eachpixel on the solar disk. We then calculate the theoretical EW and FWHM from theVALC model. An active region is also studied in particular for difference inthe quiet Sun and the sunspots. The Si I line is formed at the bottom of thephotosphere. The EW of this line increases from the disk center to $\mu$ = 0.2,and then decreases toward the solar limb, while the FWHM shows a monotonicallyincreasing trend. Theoretically predicted EW agrees well with observations,while the predicted FWHM is far smaller due to the absence of unresolvedturbulence in models. The macroturbulent velocity is estimated to be 2.80 kms$^{-1}$ at the disk center, and increases to 3.52 km s$^{-1}$ at $\mu$ = 0.2.We do not find any response to flare heating in current observations. Dopplershifts and line widths of the Si I 6560.58 \r{A} and Fe I 6569.21 \r{A} linescan be used to study the mass flows and turbulence of the differentphotospheric layers. The Si I line has good potentials to diagnose the dynamicsand energy transport in the photosphere.

Statistical analysis of the Si I 6560.58 \r{A} line observed by CHASE