Keele Research Repository
Explore the Repository
Guzik, JA, Houdek, G, Chaplin, WJ, Smalley, B, Kurtz, DW, Gilliland, RL, Mullally, F, Rowe, JF, Bryson, ST, Still, MD, Antoci, V, Appourchaux, T, Basu, S, Bedding, TR, Benomar, O, Garcia, RA, Huber, D, Kjeldsen, H, Latham, DW, Metcalfe, TS, Papics, PI, White, TR, Aerts, C, Ballot, J, Boyajian, TS, Briquet, M, Bruntt, H, Buchhave, LA, Campante, TL, Catanzaro, G, Christensen-Dalsgaard, J, Davies, GR, Dogan, G, Dragomir, D, Doyle, AP, Elsworth, Y, Frasca, A, Gaulme, P, Gruberbauer, M, Handberg, R, Hekker, R, Karoff, C, Lehmann, H, Mathias, P, Mathur, S, Miglio, A, Molenda-Zakowicz, J, Mosser, B, Murphy, SJ, Regulo, C, Ripepi, V, Salabert, D, Sousa, SG, Stello, D and Uytterhoeven, K (2016) Detection of Solar-Like Oscillations, Observational Constraints, and Stellar Models for theta Cyg, the Brightest Star Observed by the Kepler Mission. The Astrophysical Journal: an international review of astronomy and astronomical physics, 831 (1). ISSN 1538-4357
1607.01035v1.pdf - Accepted Version
Available under License Creative Commons Attribution Non-commercial.
Download (4MB) | Preview
Abstract
θ Cygni is an F3 spectral type magnitude V = 4.48 main-sequence star that was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were first obtained during Quarter 6 (2010 June–September) and subsequently in Quarters 8 and 12–17. We present analyses of solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 modes with frequencies of 1000–2700 μHz, a large frequency separation of 83.9 ± 0.4 μHz, and maximum oscillation amplitude at frequency ν max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T eff = 6697 ± 78 K, radius 1.49 ± 0.03 R ⊙, [Fe/H] = −0.02 ± 0.06 dex, and log g = 4.23 ± 0.03. We calculate stellar models matching these constraints using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses of 1.35–1.39 M ⊙ and ages of 1.0–1.6 Gyr. θ Cyg's T eff and log g place it cooler than the red edge of the γ Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The pulsation models show γ Dor gravity modes driven by the convective blocking mechanism, with frequencies of 1–3 cycles per day (11 to 33 μHz). However, gravity modes were not seen in Kepler data; one signal at 1.776 cycles per day (20.56 μHz) may be attributable to a faint, possibly background, binary.
Item Type: | Article |
---|---|
Additional Information: | Guzik, J.A. et al., 2016. DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FOR θ CYG, THE BRIGHTEST STAR OBSERVED BY THE KEPLER MISSION. The Astrophysical Journal, 831(1), p.17. Available at: http://dx.doi.org/10.3847/0004-637x/831/1/17, © 2016. The American Astronomical Society. |
Uncontrolled Keywords: | asteroseismology, stars, fundamental parameters, stars, interiors, stars, solar-type |
Subjects: | Q Science > QB Astronomy |
Divisions: | Faculty of Natural Sciences > School of Physical and Geographical Sciences |
Depositing User: | Symplectic |
Date Deposited: | 31 Aug 2016 11:04 |
Last Modified: | 08 Apr 2019 09:09 |
URI: | https://eprints.keele.ac.uk/id/eprint/2140 |