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Searches for small exoplanets around solar-type stars are limited by stellar physical variability. While chromospheric variability is well studied, observing, modeling. and understanding the much smaller fluctuations in photospheric spectral line strengths, shapes, and shifts is challenging. Extreme precision radial-velocity spectrometers now enable extreme precision stellar spectroscopy and time series of the Sun seen as a star permit monitoring of its photospheric variability. Fluctuations in their line strengths may well correlate with radial-velocity excursions and identify observable proxies for their monitoring. From three years of HARPS-N observations of the Sun-as-a-star, one thousand low-noise spectra are selected, and line absorption measured in Fe I, Fe II, Mg I, Mn I, H-alpha, H-beta, H-gamma, Na I, and the G-band. Their variations and likely atmospheric origins are examined, also with respect to simultaneously measured chromospheric emission and apparent radial velocity. Systematic line-strength variability is seen, largely shadowing the solar-cycle evolution of Ca II H & K emission, but with smaller amounts, typically on a sub-percent level. Among iron lines, greatest amplitudes are for Fe II in the blue, while the trends change sign among differently strong lines in the green Mg I triplet and between Balmer lines. Variations in the G-band core are greater than of the full G-band, in line with theoretical predictions. No variation is detected in the semi-forbidden Mg I 457.1 nm. Hyperfine split Mn I behaves largely similar to Fe I. For lines at longer wavelengths, telluric absorption limits the achievable precision. Microvariability in the solar photospheric spectrum thus displays systematic signatures among various features. These measure something different than the classical Ca II H & K index while still reflecting a strong influence from magnetic regions.
Dravins et al. (Thu,) studied this question.