On the first δ Sct–roAp hybrid pulsator and the stability of p and g modes in chemically peculiar A/F stars

Murphy, Simon J, Saio, Hideyuki, Takada-Hidai, Masahide, Kurtz, Donald Wayne orcid iconORCID: 0000-0002-1015-3268, Shibahashi, Hiromoto, Takata, Masao and Hey, Daniel R (2020) On the first δ Sct–roAp hybrid pulsator and the stability of p and g modes in chemically peculiar A/F stars. Monthly Notices of the Royal Astronomical Society, 498 (3). pp. 4272-4286. ISSN 0035-8711

[thumbnail of Version of Record]
PDF (Version of Record) - Published Version
Available under License Creative Commons Attribution.


Official URL: https://doi.org/10.1093/mnras/staa2667


Abstract Strong magnetic fields in chemically peculiar A-type (Ap) stars typically suppress low-overtone pressure modes (p modes) but allow high-overtone p modes to be driven. KIC 11296437 is the first star to show both. We obtained and analysed a Subaru spectrum, from which we show that KIC 11296437 has abundances similar to other magnetic Ap stars, and we estimate a mean magnetic field modulus of 2.8 ± 0.5 kG. The same spectrum rules out a double-lined spectroscopic binary, and we use other techniques to rule out binarity over a wide parameter space, so the two pulsation types originate in one δ Sct–roAp hybrid pulsator. We construct stellar models depleted in helium and demonstrate that helium settling is second to magnetic damping in suppressing low-overtone p modes in Ap stars. We compute the magnetic damping effect for selected p and g modes, and find that modes with frequencies similar to the fundamental mode are driven for polar field strengths ≲ 4 kG, while other low-overtone p modes are driven for polar field strengths up to ∼1.5 kG. We find that the high-order g modes commonly observed in γ Dor stars are heavily damped by polar fields stronger than 1–4 kG, with the damping being stronger for higher radial orders. We therefore explain the observation that no magnetic Ap stars have been observed as γ Dor stars. We use our helium-depleted models to calculate the δ Sct instability strip for metallic-lined A (Am) stars, and find that driving from a Rosseland mean opacity bump at ∼5 × 104 K caused by the discontinuous H-ionization edge in bound-free opacity explains the observation of δ Sct pulsations in Am stars.

Repository Staff Only: item control page