Stellar atmospheres separate the hot and dense stellar interiors from the emptiness of space. Radiation escapes from the outermost layers of a star, carrying direct physical information. Underneath the atmosphere, the very high opacity keeps radiation thermalized and resembling a black body with the local temperature. In the atmosphere the opacity
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The Shapes of Stellar SpectraAllende Prieto, Carlos32023Citations2
Evolution of the Size–Mass Relation of Star-forming Galaxies Since z = 5.5 Revealed by CEERS
We combine deep imaging data from the CEERS early release JWST survey and Hubble Space Telescope imaging from CANDELS to examine the size–mass relation of star-forming galaxies and the morphology–quenching relation at stellar masses M ⋆ ≥ 109.5 M ⊙ over the redshift range 0.5 < z < 5.5. In this study with a sample of 2450 galaxies, we separate starWard, Ethan et al.
Hydrogenated amorphous carbon grains as an alternative carrier of the 9-13 μm plateau feature in the fullerene planetary nebula Tc 1
Fullerenes have been observed in several astronomical objects since the discovery of C60 in the mid-infrared (mid-IR) spectrum of the planetary nebula (PN) Tc 1. It has been suggested that the carriers of the broad unidentified infrared (UIR) plateau features, such as the 9-13 μm emission feature (12 μm hereafter), may be related to the formationGómez-Muñoz, M. A. et al.
MANCHA3D Code: Multipurpose Advanced Nonideal MHD Code for High-Resolution Simulations in Astrophysics
The MANCHA3D code is a versatile tool for numerical simulations of magnetohydrodynamic (MHD) processes in solar/stellar atmospheres. The code includes nonideal physics derived from plasma partial ionization, a realistic equation of state and radiative transfer, which allows performing high-quality realistic simulations of magnetoconvection, as wellModestov, M. et al.
Planet formation around intermediate-mass stars. I. Different disc evolutionary pathways as a function of stellar mass
Context. The study of protoplanetary disc evolution and theories of planet formation has predominantly concentrated on solar- (and low-) mass stars since they host the majority of confirmed exoplanets. Nevertheless, the confirmation of numerous planets orbiting stars more massive than the Sun (up to ~3 M⊙) has sparked considerable interest inRonco, M. P. et al.
PSR J0210+5845: Ultra-wide binary pulsar with a B6 V main sequence star companion
We report on radio timing observations of PSR J0210+5845 that reveal large deviations from typical pulsar spin-down behaviour. We interpret these deviations as being due to the binary motion around the V = 13.5 star 2MASS J02105640+5845176, which is coincident in terms of its celestial position and distance with the pulsar. Archival observationsvan der Wateren, E. et al.