On the origin of the Galactic thin and thick discs, their abundance gradients and the diagnostic potential of their abundance ratios
Metadatos
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Oxford University Press
Materia
Galaxy: general Galaxy: abundances Galaxy: disc Galaxies: evolution Galaxies: formation Galaxy: Solar neighbourhood
Fecha
2023-05-25Referencia bibliográfica
Nikos Prantzos and others, On the origin of the Galactic thin and thick discs, their abundance gradients and the diagnostic potential of their abundance ratios, Monthly Notices of the Royal Astronomical Society, Volume 523, Issue 2, August 2023, Pages 2126–2145. [https://doi.org/10.1093/mnras/stad1551]
Patrocinador
Centre National d’Etudes Spatiales (CNES); Gaia Data Processing and Analysis Consortium DPAC; European Space Agency ESA; Centre National d’Etudes Spatiales PGC2018-095317-B-C21 CNES; Ministerio de Ciencia e Innovación MICINN; Agencia Estatal de Investigación PID2021-123110NB-I00 AEIResumen
Using a semi-analytical model of the evolution of the Milky Way, we show how secular evolution can create distinct overdensities in the phase space of various properties (e.g. age versus metallicity or abundance ratios versus age) corresponding to the thin and thick discs. In particular, we show how key properties of the Solar vicinity can be obtained by secular evolution, with no need for external or special events, like galaxy mergers or paucity in star formation. This concerns the long established double-branch behaviour of [alpha/Fe] versus metallicity and the recently found non-monotonic evolution of the stellar abundance gradient, evaluated at the birth radii of stars. We extend the discussion to other abundance ratios and we suggest a classification scheme, based on the nature of the corresponding yields (primary versus secondary or odd elements) and on the lifetimes of their sources (short-lived versus long-lived ones). The latter property is critical in determining the single- or double- branch behaviour of an elementary abundance ratio in the Solar neighbourhood. We underline the high diagnostic potential of this finding, which can help to separate clearly elements with sources evolving on different time-scales and help determining the site of e.g. the r-process(es). We define the ‘abundance distance’ between the thin and thick disc sequences as an important element for such a separation. We also show how the inside-out evolution of the Milky Way disc leads rather to a single-branch behaviour in other disc regions.
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