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The advent of Gaia, capable of measuring stellar wobbles caused by orbitingplanets, raised an interest to the astrometric detection of exoplanets. Anothersource of such wobbles (often also called jitter) is stellar magnetic activity.A quantitative assessment of the stellar astrometric jitter is important for amore reliable astrometric detection and characterisation of exoplanets. Wecalculate the displacement of the solar photocentre due to the magneticactivity for an almost 16-year period (February 2, 1999 - August 1, 2014). Wealso investigate how the displacement depends on the spectral passband chosenfor observations, including the wavelength range to be covered by the upcomingSmall-JASMINE mission of JAXA. This is done by extending the SATIRE-S model forsolar irradiance variability to calculating the displacement of the solarphotocentre caused by the magnetic features on the surface of the Sun. We foundthat the peak to peak amplitude of the solar photocentre displacement wouldreach 0.5 mas if the Sun were located 10 pc away from the observer and observedin the Gaia G filter. This is by far too small to be detected by the Gaiamission. However, the Sun is a relatively inactive star so that one can expectsignificantly larger signals for younger, and, consequently, more active stars.The model developed in this study can be combined with the simulations ofemergence and surface transport of magnetic flux which have recently becameavailable to model the astrometric jitter over the broad range of magneticactivities.

Predictions of astrometric jitter for Sun-like stars. I. The model and its application to the Sun as seen from the ecliptic