Aims:We study the emergence of magnetic flux from the near-surface layers of the solar convection zone into the photosphere. Methods: To model magnetic flux emergence, we carried out a set of numerical radiative magnetohydrodynamics simulations. Our simulations take into account the effects of compressibility, energy exchange via radiative transfer

We model the emergence of buoyant magnetic flux from the convection zone into the photosphere by means of 3D radiative MHD simulations using the MURaM code. In a series of simulations, we study how an initially buoyant magnetic flux tube rises in the presence of granular convection. The simulations take into account the effects of radiative energy

The primary goal of this project is to characterize the surface composition (and other properties such as radius, albedo and thermal inertia) of a sample of low perihelion Near- Earth Asteroids (NEAs), based on their 7 to 14 micron spectrum. NEAs with low perihelion distances represent a unique laboratory in which to study the effects of thermal

Context: High-redshift ultra luminous infrared galaxies contribute the bulk of the cosmic IR background and are the best candidates for very massive galaxies in formation at z>1.5. Aims: It is necessary to identify the energy source for their huge luminosities, starburst or AGN activity, in order to correctly interpret the role of ULIRGs in galaxy

The photospheric Mn I 539.4 nm line in the solar spectrum shows unusual variability with the solar cycle in that its depth decreases with increasing activity. citet{nv-2001A&A...369L..13D} claimed that this phenomenon is due to interlocking between the chromospheric Mg II h & k lines and an overlapping Mn I multiplet. In this contribution we test

We request 13.9 hours of IRS GTO time to observe two recently discovered very low-mass T dwarfs, the early-T HN PegB and the very late-T ULAS J0034. As inferred from models, the two T dwarfs have similar masses of around 20 MJupiter, and similar gravities, but very different effective temperatures of Teff ~1100 K and 650 K for HN PegB and ULAS