About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet 1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R ⊕), or apparently rocky planets smaller than 2 R ⊕. Such lack of planets of intermediate size (the `hot Neptune

We present the results of two-dimensional, grid-type hydrodynamical simulations, with parsec-scale central resolution, for the evolution of the hot gas in isolated early-type galaxies (ETGs). The simulations include a physically self-consistent treatment of the mechanical (from winds) and radiative AGN feedback, and were run for a large set of

We present surface photometry and stellar kinematics of NGC 4264, a lenticular galaxy in the region of the Virgo Cluster undergoing a tidal interaction with its neighbour, NGC 4261. We measured the bar radius and strength from SDSS imaging and the bar pattern speed from MUSE integral-field spectroscopy. We find that NGC 4264 hosts a strong and

With the LAMOST DR4 and Gaia DR2 common red clump giant stars, we investigate the three-dimensional kinematics of Milky Way disk stars in mono-age populations between Galactocentric distances of R = 6 and 15 kpc. We confirm the 3D asymmetrical motions of recent works, and provide time tagging of the Galactic outer disk asymmetrical motions. Radial

The recent discovery of low-amplitude dipolar oscillation mixed modes in massive red giants indicates the presence of a missing physical process inside their cores. Stars more massive than ∼ 1.3 M ☉ are known to develop a convective core during the main-sequence: the dynamo process triggered by this convection could be the origin of a strong

Rotation plays an important role in the evolution of stars. For decades rotation-age relationships have been used as surface rotation can be measured rather easily. Here we show the result of the measurement of rotation periods for a large number of Kepler solar-like stars along with their level of magnetic activity. We also study solar-like stars