Publicación
Hot subdwarfs: further photometric observations of pulsating and non pulsating objects
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PublicaciónHot Subdwarfs: Magnetic, Oscillatory and Other Physical PropertiesHot subdwarf stars (hot sds) are blue subluminous objects. Only a few determinations are available to date regarding the study of such aspects as rotation...
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PublicaciónHow 4MOST and MOONS will improve constraints on the dynamical masses of Local Group galaxiesThe wide-field spectrographs 4MOST and MOONS are expected to enter operations in late 2024 at the ESO Paranal Observatory. These upcoming survey facilities will...
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PublicaciónHow a dust concentration mimics dynamical signatures around the nucleus of NGC 7331.Where the pheonomenon of wavelength-dependent kinematics has been observed in galaxies, it has been well modelled as a dust extinction effect. Therefore...
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PublicaciónHow AMBER will contribute to the search for brown dwarfs and extrasolar giant planetsVarious radial velocity surveys have now produced a number of candidates Very Low Mass Stars, Brown Dwarfs and Giant Extrasolar Planets to nearby G, K and M...
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PublicaciónHow anomalous is the interstellar extinction in NGC 3372, the Carina Nebula?Near-infrared JHKL photometry of more than 200 stars in the open clusters Tr 14, Tr 15, Tr 16, Cr 228, and Cr 232 in the Carina Nebula is presented. By...
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PublicaciónHow Binary Stars affect Galactic Chemical EvolutionAt least 60% of stars appear to be binary and about half of these are close enough to interact. Because of the enormous expansion on the AGB, many of these...
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PublicaciónHow do inaccuracies and unresolved structures in the measured solar photospheric magnetic vector influence the accuracy of coronal magnetic field models?Solar magnetic fields are usually extrapolated into the corona starting from photospheric mag-netic measurements that can suffer from significant uncertainties...
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PublicaciónHow do massive stars form? Finding targets for MIRADASObservations from massive stars in H II regions can help to clarify theories of massive star formation because they show the degree of isolation under which...