Stellar Chromospheric Activity and Age Relation from Open Clusters in the LAMOST Survey

Zhang, Jiajun; Zhao, Jingkun; Oswalt, Terry D.; Fang, X.-S.; Zhao, Gang; Liang, Xian-Ting; Ye, Xianhao; Zhong, Jianxin

doi:10.3847/1538-4357/ab4efe

Cited by 30 publications

(18 citation statements)

References 31 publications

(48 reference statements)

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“…Maldonado et al 2015), and activity proxies (e.g. Zhang et al 2019;Messina 2021). Asteroseismic analysis allows us to obtain the age of single stars in our Galaxy (Lebreton & Montalbán 2009).…”

Section: Introductionmentioning

confidence: 99%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

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Context. Gyrochronology is one of the methods currently used to estimate the age of stellar open clusters. Hundreds of new clusters, associations, and moving groups unveiled by Gaia and complemented by accurate rotation period measurements provided by recent space missions such as Kepler and TESS are allowing us to significantly improve the reliability of this method. Aims. We use gyrochronology, that is, the calibrated age-mass-rotation relation valid for low-mass stars, to measure the age of the recently discovered moving group Group X. Methods. We extracted the light curves of all candidate members from the TESS full frame images and measured their rotation periods using different period search methods. Results. We measured the rotation period of 168 of a total of 218 stars and compared their period-colour distribution with those of two age-benchmark clusters, the Pleiades (125 Myr) and Praesepe (625 Myr), as well as with the recently characterised open cluster NGC 3532 (300 Myr). Conclusions. As result of our analysis, we derived a gyro age of 300 ± 60 Myr. We also applied as independent methods the fitting of the entire isochrone and of the three brightest candidate members individually with the most precise stellar parameters, deriving comparable values of 250 Myr and 290 Myr, respectively. Our dating of Group X allows us to definitively rule out the previously proposed connection with the nearby but much older Coma Berenices cluster.

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Section: Introductionmentioning

confidence: 99%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

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“…The field was given a significant renewed impetus by the availability of high-cadence photometric observations obtained as part of the Kepler Space Telescope's main and K2 surveys (2009-2018). More recently, the Zwicky Transient Facility (ZTF) 2 and the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) Medium-Resolution Survey have further opened up this field by providing large numbers of high-quality photometric and spectroscopic time-series observations, respectively [53,303,304].…”

Section: Open Questions and Current Trendsmentioning

confidence: 99%

“…The wealth of new observational data has not yet been mined beyond the proverbial low-hanging fruit. Statistical studies yielding improved stellar ages-including 'chromospheric ages' [163]-are crucial for understanding stellar chromospheric activity as a function of the host star's age and evolutionary stage [275,303]. Beyond simply expanding our samples to achieve statistically significant compilations, to better understand the growing samples of solar twins we should also expand our wavelength coverage from the commonly used Ca II H and K triplet lines to both shorter (extreme UV, X-rays) and longer (infrared, radio) wavelengths.…”

Section: Open Questions and Current Trendsmentioning

confidence: 99%

Stellar Chromospheric Variability

Grijs

Kamath

2021

Universe

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Cool stars with convective envelopes of spectral types F and later tend to exhibit magnetic activity throughout their atmospheres. The presence of strong and variable magnetic fields is evidenced by photospheric starspots, chromospheric plages and coronal flares, as well as by strong Ca ii H+K and Hα emission, combined with the presence of ultraviolet resonance lines. We review the drivers of stellar chromospheric activity and the resulting physical parameters implied by the observational diagnostics. At a basic level, we explore the importance of stellar dynamos and their activity cycles for a range of stellar types across the Hertzsprung–Russell diagram. We focus, in particular, on recent developments pertaining to stellar rotation properties, including the putative Vaughan–Preston gap. We also pay specific attention to magnetic variability associated with close binary systems, including RS Canum Venaticorum, BY Draconis, W Ursae Majoris and Algol binaries. At the present time, large-scale photometric and spectroscopic surveys are becoming generally available, thus leading to a resurgence of research into chromospheric activity. This opens up promising prospects to gain a much improved understanding of chromospheric physics and its wide-ranging impact.

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“…Several studies have intended to calibrate this emission as a function of age (e.g. Soderblom et al 1991;Lachaume et al 1999;Mamajek & Hillenbrand 2008;Lorenzo-Oliveira et al 2018;Booth et al 2020;Zhang et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…Average Ca II R HK index evolution of 0.8-1.0 M stars with nearsolar metallicity derived from their rotation period evolution compared with previous studies. These include (i) the relationship of Lorenzo-Oliveira et al (2018) for 0.8 and 1.0 M stars with solar metallicity, (ii) the age-activity relationships ofMamajek & Hillenbrand (2008) for F7-K2 dwarfs (0.5 < B−V < 0.9), and (iii) the age-activity relationship ofZhang et al (2019) for stars with 4000 K < T eff < 5500 K.…”

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confidence: 99%

Chromospheric activity of nearby Sun-like stars

Gondoin

2020

A&A

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Context. The chromospheric emission in the cores of the Ca II H & K lines of late-type dwarfs is a well known indicator of magnetic activity that decreases with increasing stellar age. Aims. I use this indicator to investigate the formation history of nearby G- and early K-type stars with origins at galactocentric distances similar to that of the region where the Sun was born. Methods. A parent sample of single main-sequence stars with near-solar metallicity and known magnetic activity levels is built from catalogues of stellar atmospheric parameters and chromospheric activity indices. A kinematical approach uses Gaia astrometric data to differentiate thin disc stars from thick disc stars. Measured distributions of R′HK chromospheric activity indices are compared with Monte Carlo simulations based on an empirical model of chromospheric activity evolution. Results. The thin disc includes a significant fraction of Sun-like stars with intermediate activity levels (2 × 10−5 ≤ R′HK ≤ 6 × 10−5), while most early K- and G-type stars from the thick disc are inactive (R′HK < 2 × 10−5). The chromospheric activity distribution among nearby Sun-like dwarfs from the thin disc can be explained by a combination of an old (>6–7 Gyr) star formation event (or events) and a more recent (<3 Gyr) burst of star formation. Such an event is not required to account for the R′HK index distributions of nearby thick disc stars. Conclusions. The distribution of magnetic activity among local G- and early K-type stars with a near-solar metallicity bears the imprint of an important star formation event that occurred ~1.9–2.6 Gyr ago in the thin disc of the Milky Way.

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Stellar Chromospheric Activity and Age Relation from Open Clusters in the LAMOST Survey

Cited by 30 publications

References 31 publications

Gyrochronological dating of the stellar moving group Group X

Gyrochronological dating of the stellar moving group Group X

Stellar Chromospheric Variability

Chromospheric activity of nearby Sun-like stars

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