Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the formation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA's Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show

Results on theoretical work, astronomical observations and laboratory measurements of the new form of carbon known as fullerenes and their hydrogenated forms (fulleranes) are reviewed. These molecules can be responsible for diffuse interstellar bands, for the UV bump, a prominent feature in the extinction curves observed in many lines of sight of

δ Sct are one of the most abundant pulsating stars in our Galaxy. In addition, they have moderate to fast rotations and periods of several hours. That makes them the suitable targets for studying the effects of rotation on stellar evolution. In this work, we show how to infer the mean density and the surface gravity of an A-type pulsanting star

LoTr 5 is a planetary nebula with an unusual long-period binary central star. The pair consists of a rapidly rotating G-type star and a hot star, which is responsible for the ionization of the nebula. Both components are in a wide orbit with a period of about 2700 days, one of the longest in central star of planetary nebulae. In this contribution

The study of minor planets is motivated both by fundamental science of Solar system origins (some of these bodies contain the most pristine materials from the early ages of the planetary nebula) and by practical reasons concerning space exploration and impact frequency with Earth. Among minor bodies, near-Earth asteroids are a particularly

NSVS 10653195 is a double-line detached eclipsing binary star found in 2007 by te{coughlin2007} among the NSVS periodic variable stars. The first analysis of the optical VRI light curves by te{coughlin2007} show that this binary could be composed by two low mass stars. Other authors analyzed new optical light curves for this system, obtaining some