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Internal Rotation of Gravity Mode Pulsators in the Pleiades Dario Fritzewski TASC 9/KASC 16 Klosterneuburg – 7July 2025 KPNO/NOIRLab/NSF/AURA/Tad Denton/Adam Block
2 Why open cluster asteroseismology? •Calibration of asteroseismically-informed stellar models •Homogeneous populations with different masses •Empirical relations from open clusters ordered by age Challenges •Membership •Crowded fields leading to contamination •Especially challenging for TESS (21”/px) APOD / Rogelio Bernal Andreo
3 Breger (1972) 𝑀0 𝑉 (𝑏−𝑦)0 50+ years in history of Pulsators in the Pleiades
3 Bedding et al. (2023) Breger (1972) 𝑀0 𝑉 (𝑏−𝑦)0 50+ years in history of Pulsators in the Pleiades
3 Bedding et al. (2023) Mostly δ Sct stars known Two candidate ɣ Dor (Martín & Rodríguez, 2000) Breger (1972) 𝑀0 𝑉 (𝑏−𝑦)0 50+ years in history of Pulsators in the Pleiades
HD 23375 - A pure g-mode pulsator 4 3 sectors 2 sectors ~2 yr gap Photometry from TESS FFI Custom aperture to reduce contamination Detrending to remove long-term trends
HD 23375 - A pure g-mode pulsator 4 3 sectors 2 sectors ~2 yr gap Photometry from TESS FFI Custom aperture to reduce contamination Detrending to remove long-term trends
HD 23375 - A pure g-mode pulsator 4 3 sectors 2 sectors ~2 yr gap Photometry from TESS FFI Custom aperture to reduce contamination Detrending to remove long-term trends
HD 23375 - A pure g-mode pulsator 4 3 sectors 2 sectors ~2 yr gap Photometry from TESS FFI Custom aperture to reduce contamination Detrending to remove long-term trends
Period spacing patterns are rare 6 Typical patterns in TESS data are short. 3/25 stars with patterns in the Pleiades Even clear ɣ Dor stars do not show patterns Low amplitude peaks missing amplitude [ppt] ΔP [s]
7 Near-core rotation from dominant frequencies near-core rotation freq. [d-1] dominant mode frequency [d-1] Aerts et al. (2025)
7 Assumption: prograde dipole mode •Most common dominant modes •Many stars with observed dipole and quadrupole modes secure identification Near-core rotation from dominant frequencies near-core rotation freq. [d-1] dominant mode frequency [d-1] Aerts et al. (2025)
Near-core rotation rates in Pleiades members 8
Near-core rotation rates in Pleiades members 8
Near-core rotation rates in Pleiades members 8 Including data from Rebull et al. (2016a,b)
Near-core rotation rates in Pleiades members 8 Including data from Rebull et al. (2016a,b)
Near-core rotation in the Pleiades vs. NGC 2516 Including data from Irwin et al. (2007), Rebull et al. (2016), Fritzewski et al. (2020), Healy & McCullough (2020), Bouma et al. (2021), Li et al. (2024) 9
Near-core rotation in the Pleiades vs. NGC 2516 Including data from Irwin et al. (2007), Rebull et al. (2016), Fritzewski et al. (2020), Healy & McCullough (2020), Bouma et al. (2021), Li et al. (2024) 9
Near-core rotation in the Pleiades vs. NGC 2516 ~3 d-1 (0.5 v/vcrit) ~2 d-1 (0.3 v/vcrit) Including data from Irwin et al. (2007), Rebull et al. (2016), Fritzewski et al. (2020), Healy & McCullough (2020), Bouma et al. (2021), Li et al. (2024) 9
Additional Material
13 53% of δ Sct stars are hybrid pulsators p-mode dominated both g-mode dominated With more observations: Even lower amplitude g-modes might be visible Are most δ Sct hybrids?
Pleiades and NGC 2516: Two coeval open clusters 14 Fritzewski et al. (2020) See also Jeffries et al. (1998) Identical cool stars rotation period distributions and lithium depletion common age Bouma et al. (2021) NGC 2516
