The imprint of star formation on stellar pulsations

Steindl, T.; Zwintz, K.; Vorobyov, Eduard I.

doi:10.1038/s41467-022-32882-0

Cited by 10 publications

(6 citation statements)

References 65 publications

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“…The data that support the findings of this study are publicly available in zenodo with the identifier 10.5281/zenodo.6762319 68 .…”

Section: Data Availabilitysupporting

confidence: 68%

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The imprint of star formation on stellar pulsations

Steindl,

Zwintz,

Vorobyov

2022

Preprint

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In the earliest phases of their evolution, stars gain mass through the acquisition of matter from their birth clouds. The widely accepted classical concept of early stellar evolution neglects the details of this accretion phase and assumes the formation of stars with large initial radii that contract gravitationally. In this picture, the common idea is that once the stars begin their fusion processes, they have forgotten their past. By analysing stellar oscillations in recently born stars, we show that the accretion history leaves a potentially detectable imprint on the stars' interior structures. Currently available data from space would allow discriminating between these more realistic accretion scenarios and the classical early stellar evolution models. This opens a window to investigate the interior structures of young pulsating stars that will also be of relevance for related fields, such as stellar oscillations in general and exoplanet studies.

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“…The data that support the findings of this study are publicly available in zenodo with the identifier 10.5281/zenodo.6762319 68 .…”

Section: Data Availabilitysupporting

confidence: 68%

“…The input files of MESA and GYRE to reproduce the results of this study are available from the corresponding author upon reasonable request. The scripts to produce all Figures including supplementary material have been deposited in a zenodo repository with the identifier 10.5281/zenodo.7009252 68 .…”

Section: Data Availabilitymentioning

confidence: 99%

The imprint of star formation on stellar pulsations

Steindl,

Zwintz,

Vorobyov

2022

Preprint

Self Cite

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“…The functional dependency is controlled by four parameters: β 1 = 0.005, β 2 = 0.2, a midpoint accretion rate of Ṁm = 6.2 • 10 −6 M yr −1 and a crossover width of ∆ = 5.95 • 10 −6 M yr −1 . For comparability, we use the same values as in Steindl et al (2022), which were originally adapted from Jensen & Haugbølle (2018) for numerical stability. In our case, this translates to a constant value β at the beginning of the evolution which becomes gradually smaller as the accretion rate decreases (see Figure 2).…”

Section: Stellar Evolution With Mesamentioning

confidence: 99%

The influence of metallicity on a combined stellar and disk evolution

Gehrig

Steindl

Vorobyov

et al. 2023

A&A

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Context. The effects of an accretion disk are crucial to understanding the evolution of young stars. During the combined evolution, stellar and disk parameters influence each other, motivating a combined stellar and disk model. This makes a combined numerical model, evolving the disk alongside the star, the next logical step in the progress of studying early stellar evolution. Aims. We aim to understand the effects of metallicity on the accretion disk and the stellar spin evolution during the T Tauri phase. Methods. We combine the numerical treatment of a hydrodynamic disk with stellar evolution, including a stellar spin model, allowing a self-consistent calculation of the back-reactions between the individual components. Results. We present the self-consistent theoretical evolution of T-Tauri stars coupled to a stellar disk. We find that disks in low metallicity environments are heated differently and have shorter lifetimes, compared to their solar metallicity counterparts. Differences in stellar radii, the contraction rate of the stellar radius, and the shorter disk lifetimes result in faster rotation of low metallicity stars. Conclusions. We present an additional explanation for the observed short disk lifetimes in low metallicity clusters. A combination of our model with previous studies (e.g., a metallicity-based photo-evaporation) could help to understand disk evolution and dispersal at different metallicities. Furthermore, the stellar spin evolution model includes several important effects, previously ignored (e.g., the stellar magnetic field strength and a realistic calculation of the disk lifetime) and we motivate to include our results as initial or input parameters for further spin evolution models, covering the stellar evolution towards and during the main sequence.

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“…In the latter context, ages have been inferred asteroseismically for δ Scuti stars in Upper Centaurus-Lupus (Murphy et al 2021) and CFN (Kerr et al 2022), and have helped to constrain the age of the Gaia-Enceladus stream (Bedding et al 2020). However, the ages are only as good as the physics of the models, and the accretion physics of premain-sequence stars can be very complicated (Steindl et al 2022a(Steindl et al , 2022b.…”

Section: Asteroseismic Agesmentioning

confidence: 99%

SPYGLASS. III. The Fornax–Horologium Association and Its Traceback History within the Austral Complex

Kerr

Kraus

Murphy

et al. 2022

ApJ

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The study of young associations is essential for building a complete record of local star formation processes. The Fornax–Horologium association (FH), including the χ 1 Fornacis cluster, represents one of the nearest young stellar populations to the Sun. This association has recently been linked to the Tuc-Hor, Carina, and Columba associations, building an extensive “Austral Complex” almost entirely within 150 pc. Using Gaia astrometry and photometry in addition to new spectroscopic observations, we perform the deepest survey of FH to date, identifying over 300 candidate members, nearly doubling the known population. By combining this sample with literature surveys of the other constituent populations, we produce a contiguous stellar population covering the entire Austral Complex, allowing the definitions of subpopulations to be reassessed along with connections to external populations. This analysis recovers new definitions for FH, Tuc-Hor, Columba, and Carina, while also revealing a connection between the Austral complex and the Sco-Cen-affiliated Platais 8 cluster. This suggests that the Austral complex may be just a small component of a much larger and more diverse star formation event. Computing ages and tracing stellar populations back to formation reveals two distinct nodes of cospatial and continuous formation in the Austral Complex, one containing Tuc-Hor, and the other containing FH, Carina, and Columba. This mirrors recent work showing similar structure elsewhere, suggesting that these nodes, which only emerge through the use of traceback, may represent the clearest discrete unit of local star formation, and a key building block needed to reconstruct larger star-forming events.

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The imprint of star formation on stellar pulsations

Cited by 10 publications

References 65 publications

The imprint of star formation on stellar pulsations

The imprint of star formation on stellar pulsations

The influence of metallicity on a combined stellar and disk evolution

SPYGLASS. III. The Fornax–Horologium Association and Its Traceback History within the Austral Complex

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