Context. So far, surface magnetic fields have never been detected on Mira stars. Only recently have the spectropolarimetric capabilities of measuring it via the Zeeman effect become available to us. Then, to complete the knowledge of the magnetic field and of its influence during the transition from asymptotic giant branch to planetary nebulae

Formation of stars is now believed to be tightly linked to the dynamical evolution of interstellar filaments in which they form. In this paper we analyze the density structure and kinematics of a small network of infrared dark filaments, SDC13, observed in both dust continuum and molecular line emission with the IRAM 30 m telescope. These

Aims: In a companion paper we have presented many products derived from the application of the spectral synthesis code starlight to datacubes from the CALIFA survey, including 2D maps of stellar population properties (such as mean ages, mass, and extinction) and 1D averages in the temporal and spatial dimensions. Our goal here is to assess the

We present a new approach for estimating the 3.6 μm stellar mass-to-light ratio Υ3.6 in terms of the [3.6]-[4.5] colors of old stellar populations. Our approach avoids several of the largest sources of uncertainty in existing techniques using population synthesis models. By focusing on mid-IR wavelengths, we gain a virtually dust extinction-free

We study Rayleigh-Taylor instability (RTI) at the coronal-prominence boundary by means of 2.5D numerical simulations in a single-fluid MHD approach including a generalized Ohm's law. The initial configuration includes a homogeneous magnetic field forming an angle with the direction in which the plasma is perturbed. For each field inclination we

We outline the purpose, strategy and first results of a deep, high-cadence, photometric survey of the Kepler field using the Isaac Newton Telescope on La Palma and the MDM 1.3 m Telescope on Kitt Peak. Our goal was to identify sources located in the Kepler field of view which are variable on a time-scale of a few minutes to 1 h. The astrophysically