期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 501, 期 4, 页码 5135-5148出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3970
关键词
techniques: photometric; stars: late-type; stars: mass-loss; stars: oscillations
资金
- PLATO grant from the Deutsches Zentrum fur Luft-und Raumfahrt [DLR 50OO1501]
- Max Planck Society
- National Natural Science Foundation of China (NSFC) [U2031203]
- Chinese Academy of Sciences (CAS) [U2031203]
- Australian Research Council
- Danish National Research Foundation [DNRF106]
- Alfred P. Sloan Foundation
- National Aeronautics and Space Administration [80NSSC19K0597]
- DLR
The study investigated the relationships between mass-loss, pulsations, and radiation in red giants, revealing that mass-loss rates are controlled by pulsation-enhanced dust-driven outflows, and vary with pulsation periods and luminosities of red giants, with mass-loss rates in Miras independent of luminosity. This indicates that mass-loss is not currently a limiting factor for stellar age estimates in galactic archaeology studies.
Mass-loss by red giants is an important process to understand the final stages of stellar evolution and the chemical enrichment of the interstellar medium. Mass-loss rates are thought to be controlled by pulsation-enhanced dust-driven outflows. Here, we investigate the relationships between mass-loss, pulsations, and radiation, using 3213 luminous Kepler red giants and 13 5000 ASAS-SN semiregulars and Miras. Mass-loss rates are traced by infrared colours using 2MASS and Wide-field Infrared Survey Explorer(WISE) and by observed-to-model WISE fluxes, and are also estimated using dust mass-loss rates from literature assuming a typical gas-to-dust mass ratio of 400. To specify the pulsations, we extract the period and height of the highest peak in the power spectrum of oscillation. Absolute magnitudes are obtained from the 2MASS K-s band and the Gaia DR2 parallaxes. Our results follow. (i) Substantial mass-loss sets in at pulsation periods above similar to 60 and similar to 100 d, corresponding to Asymptotic-Giant-Branch stars at the base of the period-luminosity sequences C-' and C. (ii) The mass-loss rate starts to rapidly increase in semiregulars for which the luminosity is just above the red-giant-branch tip and gradually plateaus to a level similar to that of Miras. (iii) The mass-loss rates in Miras do not depend on luminosity, consistent with pulsation-enhanced dust-driven winds. (iv) The accumulated mass-loss on the red giant branch consistent with asteroseismic predictions reduces the masses of red-clump stars by 6.3 per cent, less than the typical uncertainty on their asteroseismic masses. Thus mass-loss is currently not a limitation of stellar age estimates for galactic archaeology studies.
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