Optical design of the Tor vergata Synoptic Solar Telescope (TSST)

Abstract

Synoptic full-disk solar telescope are fundamental instruments for present and future Solar Physics and Space Weather. They are typically used to study and monitor the solar activity by using high temporal cadence observations at different wavelength. The TSST (Tor vergata Synoptic Solar Telescope) is a new synoptic telescope composed of two spectral channels: an Hα (656.3 nm) telescope and a Magneto Optical Filter (MOF)-based telescope in the Potassium (KI D1) absorption spectral line at 769.9 nm. Hα observations are fundamental for the identification of flaring regions. The MOF-based telescope will produce line of sight magnetograms and dopplergrams of the solar photosphere, which are respectively used to study the magnetic field's geometry in active regions and dynamics of the solar atmosphere. In this work, we present an overview on the TSST and the optical design and characteristics of the MOF-based telescope, whose optical scheme is a double-Keplerian 80mm refractor with an aberration-free imaging lens.

Flare Forecasting Algorithms Based on High-Gradient Polarity Inversion Lines in Active Regions

“…Moreover, the small dependence on the exact threshold value, due to the topological definition of complexity rather than to an accurate estimate of the magnetic energy reservoir, allows a simpler application in the case of ground-based synoptic telescopes (e.g. Elsworth et al 2015;Gosain et al 2018;Hill et al 2019;Giovannelli et al 2020;Viavattene et al 2020;Calchetti et al 2020).…”