Journal
ASTROPHYSICAL JOURNAL
Volume 891, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab7233
Keywords
Chemically peculiar stars; Chemical abundances; Stellar kinematics; Globular star clusters; Milky Way stellar halo; CN stars; Spectroscopy; Stellar dynamics; Milky Way evolution
Categories
Funding
- National Natural Science Foundation of China [U1931102, 11603037, 11973052]
- hundred-talent project of Sun Yat-sen University
- FONDECYT [3180210]
- Becas Iberoam 'erica Investigador 2019, Banco Santander, Chile
- Youth Innovation Promotion Association, CAS
- Astronomical Big Data Joint Research Center
- Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA) BASAL grant [AFB-170002]
- Direccion de Investigacion y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigacion de Academicos (PIA-DIDULS)
- National Development and Reform Commission
- Centre National D'Etudes Spatiale (CNES) [0101973]
- UTINAM Institute of the Universite de Franche-Comte - Region de Franche-Comte
- Institut des Sciences de l'Univers (INSU)
- Region de Franche-Comte
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Interesting chemically peculiar field stars may reflect their stellar evolution history and their possible origin in a different environment from where they are found now; this is one of the most important research fields in Galactic archeology. To explore this further, we have used the CN-CH bands around 4000 A to identify N-rich metal-poor field stars in LAMOST DR3. Here we expand our N-rich, metal-poor field star sample to similar to 100 stars in LAMOST DR5, where 53 of them are newly found in this work. We investigate light elements of common stars between our sample and APOGEE DR14. While Mg, Al, and Si abundances generally agree with the hypothesis that N-rich metal-poor field stars come from enriched populations in globular clusters, it is still inconclusive for C, N, and O. After integrating the orbits of our N-rich field stars and a control sample of normal metal-poor field stars, we find that N-rich field stars have different orbital parameter distributions compared to the control sample-specifically, apocentric distances, maximum vertical amplitude (Z(max)), orbital energy, and z-direction angular momentum (L-z). The orbital parameters of N-rich field stars indicate that most of them are inner-halo stars. The kinematics of N-rich field stars support their possible GC origin. The spatial and velocity distributions of our bona fide N-rich field star sample are important observational evidence to constrain simulations of the origin of these interesting objects.
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