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Montalban22/09/2022, 14:30
With the advent of high-precision photometry missions such as CoRoT, Kepler and TESS it has been possible to detect oscillations similar to those observed in the Sun in a huge number of G-K type stars, dwarfs and giant stars. The simple link between the global features of the their oscillation spectra ($\Delta \nu$ y $\nu_{\rm max}$) and stellar parameters (Mass and Radius) open the door to...
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E. Willett22/09/2022, 15:00
The helium mass fraction, Y, is an important constraint in stellar models. For low mass stars, its value is usually estimated by assuming a linear helium-to-metal enrichment ratio, DY/DZ, and so obtaining Y from the measured metal mass fraction, Z. However, the behaviour of DY/DZ is uncertain, and varies significantly between methods presented in the literature.
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We use the luminosity of red... -
S. Murphy22/09/2022, 15:20
The ages of stars are notoriously difficult to determine, especially for young stars that are still shrouded in dust or surrounded by discs. Here, every Myr matters, as we try to probe the processes of planet formation and stellar composition build-up. We typically rely on ensemble ages determined for clusters or associations, but age gradients and age dispersion limit the accuracy of this...
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L. Prisinzano22/09/2022, 15:40
With an unprecedented astrometric and photometric data precision, Gaia EDR3 gives us the opportunity to systematically and homogeneously detect and map the low mass populations of the star forming regions (SFRs)/very young clusters in the Milky Way in the optical bands.
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We present a catalogue of the young stellar objects (YSOs) identified with Gaia EDR3 data in the solar neighbourhood (within... -
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