Blazars are active galactic nuclei (AGN) with relativistic jets whose non-thermal radiation is extremely variable on various timescales 1-3. This variability seems mostly random, although some quasi-periodic oscillations (QPOs), implying systematic processes, have been reported in blazars and other AGN. QPOs with timescales of days or hours are

The CLASP2 (Chromospheric LAyer Spectro-Polarimeter 2) sounding rocket mission was launched on 2019 April 11. CLASP2 measured the four Stokes parameters of the Mg II h and k spectral region around 2800 Å along a 200″ slit at three locations on the solar disk, achieving the first spatially and spectrally resolved observations of the solar

IntroductionComets are the leftovers from the formation of the Solar System. Understanding their composition allow us to investigate the physical and chemical processes occurring at the early stages of its formation. In this contribution we analyze high resolution spectra of comet C/2020 F3 (NEOWISE) obtained with the High Accuracy Radial Velocity

IntroductionThe observation of NEOs allows us to study the physical characteristics of the smallest size bodies of our Solar System as well as to impose constraints on their origin and evolution. Considering that these objects are in unstable orbits over the age of the Solar System, this implies that it is a transient population, which can be

IntroductionAsteroids lightcurves have been used extensively to derive many important physical characteristics such as rotational properties (rotational period and pole direction) and shape (Kaasalainen et al., 2004; Hanus et al., 2011; Durech et al., 2015), as well as to identify and characterize binary asteroids (Pravec et al., 2006). In addition

IntroductionThe asteroid (4660) Nereus is considered one of the most accessible targets for a rendez-vous space mission. It was proposed as a possible target for the NASA Near-Earth Asteroid Rendezvous (NEAR) and for JAXA Hayabusa spacecraft. The lightcurve analysis and the radar shape modeling revealed a long rotational period of ≅ 15.16 ± 0.04 h