Variability among stars in the M 67 field from<i>Kepler/K2-Campaign-5</i>light curves

González, Guillermo

doi:10.1093/mnras/stw700

Cited by 15 publications

(10 citation statements)

References 22 publications

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“…who concluded no or little mass loss (equivalent to Reimers η below 0.2) for the open clusters NGC 6819 and NGC 6791, which bracket the age of M67.Finally, we obtain an average age of Age grid = 3.46 ± 0.13 Gyr for our giants. This is on the lower side compared to traditional isochrone fitting results ranging 3.6-4.6 Gyr Gyr(Gonzalez 2016) and 4.2±0.2 Gyr(Barnes et al 2016), but individual star ages are statistically compatible with those from other methods(Table 1,…”

mentioning

confidence: 44%

The K2 M67 Study: Revisiting Old Friends With K2 Reveals Oscillating Red Giants in the Open Cluster M67

Stello

Vanderburg

Casagrande

et al. 2016

ApJ

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Observations of stellar clusters have had a tremendous impact in forming our understanding of stellar evolution. The open cluster M67 has a particularly important role as a calibration benchmark for stellar evolution theory due to its near solar composition and age. As a result, it has been observed extensively, including attempts to detect solar-like oscillations in its main sequence and red giant stars. However, any asteroseismic inference has so far remained elusive due to the difficulty in measuring these extremely low amplitude oscillations. Here we report the first unambiguous detection of solar-like oscillations in the red giants of M67. We use data from the Kepler ecliptic mission, K2, to measure the global asteroseismic properties. We find a model-independent seismic-informed distance of 816±11 pc, or (m − M ) 0 = 9.57 ± 0.03 mag, an average red-giant mass of 1.36 ± 0.01 M ⊙ , in agreement with the dynamical mass from an eclipsing binary near the cluster turn-off, and ages of individual stars compatible with isochrone fitting. We see no evidence of strong mass loss on the red giant branch. We also determine seismic log g of all the cluster giants with a typical precision of ∼ 0.01 dex. Our results generally show good agreement with independent methods and support the use of seismic scaling relations to determine global properties of red giant stars with near solar metallicity. We further illustrate that the data are of such high quality, that future work on individual mode frequencies should be possible, which would extend the scope of seismic analysis of this cluster.

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mentioning

confidence: 44%

The K2 M67 Study: Revisiting Old Friends With K2 Reveals Oscillating Red Giants in the Open Cluster M67

Stello

Vanderburg

Casagrande

et al. 2016

ApJ

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“…M 67. The sample was drawn from Gonzalez (2016), who, similar to Douglas et al (2014) and Rebull et al (2016), studied stellar variability in K2 LCs. They started with the sample used in the photometric survey by Nardiello et al (2016), which they supplemented with other recent membership studies by (Yadav et al 2008;proper motions) and (Geller et al 2015;radial velocities).…”

Section: Open Clusters In K2mentioning

confidence: 99%

Flares in open clusters with K2

Ilin

Schmidt

Davenport

et al. 2019

A&A

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Context. The presence and strength of a stellar magnetic field and activity is rooted in a star's fundamental parameters such as mass and age. Can flares serve as an accurate stellar "clock"? Aims. To explore if we can quantify an activity-age relation in the form of a flaring-age relation, we measured trends in the flaring rates and energies for stars with different masses and ages. Methods. We investigated the time-domain photometry provided by Kepler's follow-up mission K2 and searched for flares in three solar metallicity open clusters with well-known ages, M 45 (0.125 Gyr), M 44 (0.63 Gyr), and M 67 (4.3 Gyr). We updated and employed the automated flare finding and analysis pipeline Appaloosa, originally designed for Kepler. We introduced a synthetic flare injection and recovery sub-routine to ascribe detection and energy recovery rates for flares in a broad energy range for each light curve. Results. We collect a sample of 1761 stars, mostly late-K to mid-M dwarfs and found 751 flare candidates with energies ranging from 4 × 10 32 erg to 6 × 10 34 erg, of which 596 belong to M 45, 155 to M 44, and none to M 67. We find that flaring activity depends both on T eff , and age. But all flare frequency distributions have similar slopes with α ≈ 2.0−2.4, supporting a universal flare generation process. We discuss implications for the physical conditions under which flares occur, and how the sample's metallicity and multiplicity affect our results.

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“…The sample was drawn from Gonzalez (2016), who, similar to Douglas et al (2014) and Rebull et al (2016), studied stellar variability in K2 LCs. They started with the sample used in the photometric survey by Nardiello et al (2016), which they supplemented with other recent membership studies by Yadav et al (2008) (proper motions) and Geller et al (2015) (radial velocities).…”

Section: M67mentioning

confidence: 99%

Flares in Open Clusters with K2. I. M45 (Pleiades), M44 (Praesepe) and M67

Ilin,

Schmidt,

Davenport

et al. 2018

Preprint

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Context. The presence and strength of a stellar magnetic field and activity is rooted in a star's fundamental parameters such as mass and age. Can flares serve as an accurate stellar "clock"? Aims. To explore if we can quantify an activity-age relation in the form of a flaring-age relation, we measured trends in the flaring rates and energies for stars with different masses and ages. Methods. We investigated the time-domain photometry provided by Kepler's follow-up mission K2 and searched for flares in three solar metallicity open clusters with well-known ages, M45 (0.125 Gyr), M44 (0.63 Gyr), and M67 (4.3 Gyr). We updated and employed the automated flare finding and analysis pipeline Appaloosa, originally designed for Kepler. We introduced a synthetic flare injection and recovery subroutine to ascribe detection and energy recovery rates for flares in a broad energy range for each light curve. Results. We collected a sample of 1 761 stars, mostly late-K to mid-M dwarfs and found 751 flare candidates with energies ranging from 4 • 10 32 erg to 6 • 10 34 erg, of which 596 belong to M45, 155 to M44, and none to M67. We find that flaring activity depends both on T eff , and age. But all flare frequency distributions have similar slopes with α ≈ 2.0 − 2.4, supporting a universal flare generation process. We discuss implications for the physical conditions under which flares occur, and how the sample's metallicity and multiplicity affect our results.

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Variability among stars in the M 67 field fromKepler/K2-Campaign-5light curves

Cited by 15 publications

References 22 publications

The K2 M67 Study: Revisiting Old Friends With K2 Reveals Oscillating Red Giants in the Open Cluster M67

The K2 M67 Study: Revisiting Old Friends With K2 Reveals Oscillating Red Giants in the Open Cluster M67

Flares in open clusters with K2

Flares in Open Clusters with K2. I. M45 (Pleiades), M44 (Praesepe) and M67

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