Holdsworth, DL, Cunha, MS, Kurtz, DW, Antoci, V, Hey, DR, Bowman, DM, Kobzar, O, Buzasi, DL, Kochukhov, O, Niemczura, E, Ozuyar, D, Shi, F, Szabó, R, Samadi-Ghadim, A, Bognár, Z, Fox-Machado, L, Khalack, V, Lares-Martiz, M, Lovekin, CC, Mikołajczyk, P, Mkrtichian, D, Pascual-Granado, J, Paunzen, E, Richey-Yowell, T, Sódor, Á, Sikora, J, Yang, TZ, Brunsden, E, David-Uraz, A, Derekas, A, Hernández, AG, Guzik, JA, Hatamkhani, N, Handberg, R, Lambert, TS, Lampens, P, Murphy, SJ, Monier, R, Pollard, KR, Quitral-Manosalva, P, Ramón-Ballesta, A, Smalley, B ORCID: https://orcid.org/0000-0002-3456-087X, Stateva, I and Vanderspek, R (2021) TESS Cycle 1 observations of roAp stars with 2-min cadence data. Monthly Notices of the Royal Astronomical Society, 506 (1). pp. 1073-1110.

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Abstract

We present the results of a systematic search for new rapidly oscillating Ap (roAp) stars using the 2-min cadence data collected by the Transiting Exoplanet Survey Satellite (TESS) during its Cycle 1 observations. We identify 12 new roAp stars. Amongst these stars we discover the roAp star with the longest pulsation period, another with the shortest rotation period, and six with multiperiodic variability. In addition to these new roAp stars, we present an analysis of 44 known roAp stars observed by TESS during Cycle 1, providing the first high-precision and homogeneous sample of a significant fraction of the known roAp stars. The TESS observations have shown that almost 60 per cent (33) of our sample of stars are multiperiodic, providing excellent cases to test models of roAp pulsations, and from which the most rewarding asteroseismic results can be gleaned. We report four cases of the occurrence of rotationally split frequency multiplets that imply different mode geometries for the same degree modes in the same star. This provides a conundrum in applying the oblique pulsator model to the roAp stars. Finally, we report the discovery of non-linear mode interactions in $\alpha$ Cir (TIC 402546736, HD 128898) around the harmonic of the principal mode -- this is only the second case of such a phenomenon.

Item Type: Article
Additional Information: © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) This final version of this article can be accessed via; https://academic.oup.com/mnras/article/506/1/1073/6289936
Uncontrolled Keywords: asteroseismology; techniques: photometric; stars: chemically peculiar; stars: magnetic field; stars: oscillations; stars: variables
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 16 Jun 2021 09:39
Last Modified: 21 Oct 2021 15:02
URI: https://eprints.keele.ac.uk/id/eprint/9736

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