Deutsch
 
Hilfe Datenschutzhinweis Impressum
  DetailsucheBrowse

Datensatz

DATENSATZ AKTIONENEXPORT

Freigegeben

Zeitschriftenartikel

Origin of α-rich young stars: clues from C, N, and O

MPG-Autoren
/persons/resource/persons123110

Hekker,  Saskia
Max Planck Research Group in Stellar Ages and Galactic Evolution (SAGE), Max Planck Institute for Solar System Research, Max Planck Society;

Externe Ressourcen
Es sind keine externen Ressourcen hinterlegt
Volltexte (beschränkter Zugriff)
Für Ihren IP-Bereich sind aktuell keine Volltexte freigegeben.
Volltexte (frei zugänglich)
Es sind keine frei zugänglichen Volltexte in PuRe verfügbar
Ergänzendes Material (frei zugänglich)
Es sind keine frei zugänglichen Ergänzenden Materialien verfügbar
Zitation

Hekker, S., & Johnson, J. A. (2019). Origin of α-rich young stars: clues from C, N, and O. Monthly Notices of the Royal Astronomical Society, 487(3), 4343-4354. doi:10.1093/mnras/stz1554.


Zitierlink: https://hdl.handle.net/21.11116/0000-0003-F255-C
Zusammenfassung
A small set of chemically old stars that appear young by their independently derived masses has been detected. These are so-called α-rich young stars. For a sample of 51 red-giant stars, for which spectra are available from SDSS/APOGEE and masses are available from asteroseismic measures based on Kepler lightcurves, we derive the C, N, and O abundances through an independent analysis. These stars span a wide range of N/C surface number density ratios. We interpret the high-mass stars with low N/C as being products of mergers or mass transfer during or after first dredge up, because the dredge-up features are the same as for low-mass stars. The α-rich young stars with high N/C follow the expected trend of N/C for their mass, and could be either genuine young stars (leaving their high [α/Fe] unexplained) or the results of mergers on the main sequence.