Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819

By A. Miglio, K. Brogaard, D. Stello, W. Chaplin, F. D’Antona, J. Montalbán, S. Basu, A. Bressan, F. Grundahl, M. Pinsonneault and 14 more. 2011

211 citations recorded by the source corpus.

Mass-loss of red giant branch (RGB) stars is still poorly determined, despite its crucial role in the chemical enrichment of galaxies. Thanks to the recent detection of solar-like oscillations in G–K giants in open clusters with Kepler, we can now directly determine stellar masses for a statistically significant sample of stars in the old open clusters NGC 6791 and 6819. The aim of this work is to constrain the integrated RGB mass-loss by comparing the average mass of stars in the red clump (RC) with that of stars in the low-luminosity portion of the RGB [i.e. stars with L L(RC)]. Stellar masses were determined by combining the available seismic parameters νmax and �ν with additional photometric constraints and with independent distance estimates. We measured the masses of 40 stars on the RGB and 19 in the RC of the old metal-rich cluster NGC 6791. We find that the difference between the average mass of RGB and RC stars is small, but significant [� M = 0.09 ± 0.03 (random) ±0.04 (systematic)

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ea5ea031692e1a50f848ef0611d7a6982ed21fae

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In Astronomy and Astrophysics

1. D. Stello
2. W. Chaplin
3. T. Bedding
4. B. Mosser
5. L. Girardi
6. Luca Casagrande
7. Hans-Walter Rix
8. Martin Asplund

In Instrumentation

1. D. Stello
2. W. Chaplin
3. B. Mosser
4. T. Bedding
5. L. Girardi
6. S. Hekker
7. Y. Elsworth
8. M. Martig

Citations in the corpus

• Age determination for 269 Gaia DR2 open clusters (2019, background): “Article number, page 6 of 14 D. Bossini et al.: Age determination for 269 Gaia DR2 Open Clusters NGC 6791 Seismic determination of the average RGB mass for NGC 6791 gives a value of M = 1.22 ± 0.01 M (Miglio et al. 2012, considering stars up to the RC luminosity).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, background): “…recent work has cautioned about the predictions from scaling relations in first ascent red giant and red clump stars (Miglio et al. 2012), expected masses of metalpoor stars (Epstein et al. 2014), and open cluster properties of main-sequence binaries (Brogaard et al. 2012; Miglio et al. 2012).”
• Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “Open clusters in the Kepler field suggest a value of η between 0.1 and 0.3 (Miglio et al. 2012) for solar-metallicity stars of masses ∼1.2– 1.5 M ; observations of globular clusters reveal that mass-loss seems to be episodic and increasingly important when ascending the red giant branch (see e.g.…”
• Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, methodology): “Mass-loss on the RGB of low-mass stars, instead, is taken into account by simply removing the amount of mass inferred from the Reimers (1975) formula with a multiplicative factor ηRei = 0.2 (see Miglio et al. 2012), as we pass from the RGB-tip to the initial stage of core-helium burning.”
• parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (2012, background): “The latter is set asη = 0.2, which is representative of the modest values recently determined by Miglio et al. (2012), based on the asteroseismic data for two star clusters in theKepler fields.”
• Confirming chemical clocks: asteroseismic age dissection of the Milky Way disc(s) (2017, methodology): “The latter was implemented following the Reimers prescription (Reimers 1977) with an efficiency of η = 0.4, representing the extreme of the commonly adopted values around η = 0.1–0.2 supported by various observations (e.g. Miglio et al. 2012; Origlia et al. 2014; Miglio et al. 2016).”
• Mixed modes in red giants: a window on stellar evolution (2014, background): “We did not take into L5, page 3 of 5 account the scaling revision proposed by Miglio et al. (2012) for red-clump stars.”
• The connection between stellar granulation and oscillation as seen by the Kepler mission (2014, background): “This is presumably due to the mass loss that stars undergo when evolving up the giant branch (see, e.g., Miglio et al. 2012).”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “Miglio et al. (2012) studied the mass of stars in open clusters and found an offset between the mass of RC and RGB stars that cannot be explained by mass-loss alone.”