The primary external energy input to planetary atmospheres comes from solar radiation. Accurate estimates of solar irradiance are needed in order to understand atmospheric conditions at other planets. Many studies have interpolated Earth-based irradiance measurements at other planets, disregarding the evolution of solar features, which are responsible for the irradiance variability. We present an approach for assessing solar irradiance at other planets by using synthetic full surface magnetograms of the Sun, generated by the Surface Flux Transport Model, and then converted into sunspots and faculae areas. Following the Spectral And Total Irradiance REconstruction approach, we compute the irradiance as the sum of contributions from sunspots, faculae, and the quiet Sun. We calculate the S-index, which is a proxy for near-ultraviolet irradiance, and the total solar irradiance, which is the wavelength-integrated value. We demonstrate that a simple phase shift of the Earth-observed total solar irradiance does not produce reliable estimates in the ecliptic. By comparing and correlating our results with the interpolated measurements, we find that the two models agree in the S-index variability, because faculae have a long lifetime, so the effect of the solar rotation becomes less important. Conversely, the methods disagree strongly in the total solar irradiance, since sunspots have a short lifetime, and the interpolation does not take into account their emergence and evolution on the far-side of the Sun, as it only uses the information of the disc visible for an Earth-bound observer.