Recent observations have shown in some sunspots the presence of structures that have been called umbral filaments (UFs). These consist of bright filamentary features intruding sunspot umbrae, different in morphology, evolution, and magnetic configuration from usually observed light bridges. We report on the properties of an UF observed inside the

We select a sample of 179 local (0 ≤ z 0.35) galaxies from the Hershel Science Archive to investigate possible relationships between the 65μm, 71μm, 79μm, 84μm, 119μm, and 163μm OH lines and the central region of the galaxy. The sample was observed using the PACS instrument, and contains a wide range of Seyfert galaxies, LINERs, and non-active

Context. The Gaia Collaboration has used Gaia-DR2 sources with six-dimensional (6D) phase space information to derive kinematical maps within 5 kpc of the Sun, which is a reachable range for stars with relative error in distance lower than 20%. Aims: Here we aim to extend the range of distances by a factor of two to three, thus adding the range of

We present an analysis of the microlensing event OGLE-2015-BLG-0232. This event is challenging to characterize for two reasons. First, the light curve is not well sampled during the caustic crossing due to the proximity of the full Moon impacting the photometry quality. Moreover, the source brightness is difficult to estimate because this event is

Coupling between fast magnetoacoustic and Alfvén waves can be observed in fully ionized plasmas mediated by stratification and 3D geometrical effects. In Paper I, Cally & Khomenko have shown that in a weakly ionized plasma, such as the solar photosphere and chromosphere, the Hall current introduces a new coupling mechanism. The present study

We study the kinematics of runaway stars using GAIA DR2 proper motions (PMs) of 304 field OB stars in the Small Magellanic Cloud (SMC) from the RIOTS4 survey. To identify runaways, we remove the SMC systemic motion from, and apply geometric corrections to, the PMs to obtain the residual peculiar velocities. We find that the SMC Wing has a systemic