期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 447, 期 4, 页码 3526-3535出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu2726
关键词
Galaxy: abundances; Galaxy: disc; Galaxy: evolution; Galaxy: kinematics and dynamics; Galaxy: stellar content
资金
- Australian Astronomical Observatory
- Leibniz-Institut fur Astrophysik Potsdam (AIP)
- Australian National University
- Australian Research Council
- French National Research Agency
- German Research Foundation [SPP 1177, SFB 881]
- European Research Council [ERC-StG 240271 Galactica]
- Instituto Nazionale di Astrofisica at Padova
- Johns Hopkins University
- National Science Foundation of the USA [AST-0908326]
- W. M. Keck foundation
- Macquarie University
- Netherlands Research School for Astronomy
- Natural Sciences and Engineering Research Council of Canada
- Slovenian Research Agency
- Swiss National Science Foundation
- Science & Technology Facilities Council of the UK
- Opticon
- Strasbourg Observatory
- University of Groningen
- University of Heidelberg
- University of Sydney
- NSF [OIA-1124403, 1066293]
- European Research Council under the European Union [321067]
- STFC [ST/G002509/1, PP/D001528/1, ST/K000985/1, ST/K00106X/1, ST/G002479/1, ST/K000977/1, PP/D001242/1, ST/J00149X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000977/1, ST/K000985/1] Funding Source: researchfish
- Office of Integrative Activities
- Office Of The Director [1124403] Funding Source: National Science Foundation
Using the RAdial Velocity Experiment fourth data release (RAVE DR4), and a new metallicity calibration that will be also taken into account in the future RAVE DR5, we investigate the existence and the properties of supersolar metallicity stars ([M/H] greater than or similar to +0.1 dex) in the sample, and in particular in the solar neighbourhood. We find that RAVE is rich in supersolar metallicity stars, and that the local metallicity distribution function declines remarkably slowly up to +0.4 dex. Our results show that the kinematics and height distributions of the supersolar metallicity stars are identical to those of the [M/H] less than or similar to 0 thin-disc giants that we presume were locally manufactured. The eccentricities of the supersolar metallicity stars indicate that half of them are on a roughly circular orbit (e <= 0.15), so under the assumption that the metallicity of the interstellar medium at a given radius never decreases with time, they must have increased their angular momenta by scattering at corotation resonances of spiral arms from regions far inside the solar annulus. The likelihood that a star will migrate radially does not seem to decrease significantly with increasing amplitude of vertical oscillations within range of oscillation amplitudes encountered in the disc.
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