We report the confirmation of a transiting planet around the bright weakly active M0.5 V star TOI-1235 (TYC 4384-1735-1, V ≈ 11.5 mag), whose transit signal was detected in the photometric time series of sectors 14, 20, and 21 of the TESS space mission. We confirm the planetary nature of the transit signal, which has a period of 3.44 d, by using

At least 20% of PNe host a post-common-envelope central star, and theoretical considerations predict that a significant fraction of these should come from common envelopes during the RGB (as opposed to the AGB). However, only a handful of candidate post-RGB PNe are known. Here, we present the discovery of a new post-RGB binary central star -

Using the Ultraviolet Visual Echelle Spectrograph (UVES) at the Very Large Telescope (VLT), we study the photoionized Herbig-Haro object HH529 in two associated bowshocks: HH529II and HH529III and its nebular background emission. We spatially isolate each bowshock and separate its blueshifted emission from the nebular background thanks to the very

PHOEBE2 (PHysics of Eclipsing BinariEs 2) is an open source binary star modelling code, which reproduces and fits light and radial velocity curves, spectral line profiles and astrometric orbits. The code represents a modern implementation of the Wilson-Devinney code with significant refinements, principally with the aim of providing an open

Thanks to missions such as CoRoT and Kepler/K2, asteroseismology has demonstrated that it is a powerful tool to determine precise stellar parameters. Now, with the NASA TESS (Transiting Exoplanet Survey Satellite) mission, a new opportunity arose to use this technique on a sample of more than 20,000 bright main-sequence and subgiant stars. The

Variability studies of blazars have identified in the past hints of quasi-periodic emission for different sources, although strong evidences are still lacking. The understanding of whether this emission is truly periodic or not can help to explain the structure of blazars and the emission mechanisms taking place in these objects. We present the