Characterizing Variability in Bright Metallic-Line A (Am) Stars Using Data from the NASA TESS Spacecraft

Guzik, Joyce A.; Jackiewicz, Jason; Catanzaro, G.; Soukup, Michael S.

doi:10.48550/arxiv.2107.09479

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“…Stars with different metallicities can pass through a given location in the H-R diagram at different ages and with different opacities in the driving zone. This will affect pulsations driven by the κ (opacity) mechanism (Guzik et al 2018) and even more so for chemically peculiar stars (Murphy et al 2015;Guzik et al 2021), so it is likely that chemical composition is part of the explanation. But even in open clusters, which are assumed to have a uniform metallicity (De Silva et al 2006;Sestito et al 2007;Bovy 2016), the pulsator fraction is much less than 1.…”

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confidence: 99%

TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars

Bedding

Murphy

Crawford

et al. 2023

ApJL

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We studied 89 A- and F-type members of the Pleiades open cluster, including five escaped members. We measured projected rotational velocities ( v sin i ) for 49 stars and confirmed that stellar rotation causes a broadening of the main sequence in the color–magnitude diagram. Using time-series photometry from NASA’s TESS Mission (plus one star observed by Kepler/K2), we detected δ Scuti pulsations in 36 stars. The fraction of Pleiades stars in the middle of the instability strip that pulsate is unusually high (over 80%), and their range of effective temperatures agrees well with theoretical models. On the other hand, the characteristics of the pulsation spectra are varied and do not correlate with stellar temperature, calling into question the existence of a useful ν max relation for δ Scutis, at least for young main-sequence stars. By including δ Scuti stars observed in the Kepler field, we show that the instability strip is shifted to the red with increasing distance by interstellar reddening. Overall, this work demonstrates the power of combining observations with Gaia and TESS for studying pulsating stars in open clusters.

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