Recent MHD 3D modelling of the Proxima system predicts that the interaction of the planet Proxima b with its host star, Proxima, would be proceeding in the supra-Alfvénic regime. In this case, no radio emission from the star-planet interaction should be observed. In https://doi.org/10.5281/zenodo.7043419 {this poster}, we present multi-epoch radio

Common envelope events have been associated with the formation of a planetary nebulae since its proposition more than forty five years ago. However, until recently there have been doubts as to whether a common envelope while the donor is ascending the red giant branch, rather than the subsequent asymptotic red giant branch, would result in a

Aims: We aim to constrain the origin of the non-detection of the metastable He I triplet at ≈10 830 Å obtained for the hot Jupiter WASP-80b. Methods: We measure the X-ray flux of WASP-80 from archival observations and use it as input to scaling relations accounting for the coronal [Fe/O] abundance ratio in order to infer the extreme-ultraviolet

We present radial velocity follow-up obtained with ESPRESSO of the M-type star LTT 1445A (TOI-455), for which a transiting planet b with an orbital period of 5.4 days was detected by TESS. We report the discovery of a second transiting planet (LTT 1445A c) and a third non-transiting candidate planet (LTT 1445A d) with orbital periods of 3.12 and 24

Many binary companions to the central stars of planetary nebulae (PNe) are found to be inflated, perhaps indicating that accretion onto the central star might occur during the planetary nebula (PN) phase. The discovery of a handful of nova eruptions and supersoft X-ray sources inside PNe supports this hypothesis. In this paper, we investigate the

We have created a new Planetary Nebulae (PNe) catalogue by using astrometric and photometric data from Gaia EDR3. Firstly, we have developed an algorithm that selects the most reliable source from EDR3 to be the Central Star (CS) of each PN, among all sources in the neighbourhood of them. This algorithm considers both the angular distance to PN