Detection Of Solar-Like Oscillations, Observational Constraints, And Stellar Models For Θ Cyg, The Brightest Star Observed By The Kepler Mission

J.~A. Guzik; G. Houdek; W.~J. Chaplin; B. Smalley; D.~W. Kurtz; R.~L. Gilliland; F. Mullally; J.~F. Rowe; S.~T. Bryson; M.~D. Still; V. Antoci; T. Appourchaux; S. Basu; T.~R. Bedding; O. Benomar; R.~A. Garcia; D. Huber; H. Kjeldsen; D.~W. Latham; T.~S. Metcalfe; P.~I. Pápics; T.~R. White; C. Aerts; J. Ballot; T.~S. Boyajian; M. Briquet; H. Bruntt; L.~A. Buchhave; T.~L. Campante; G. Catanzaro; J. Christensen-Dalsgaard; G.~R. Davies; G. Dou gan; D. Dragomir; A.~P. Doyle; Y. Elsworth; A. Frasca; P. Gaulme; M. Gruberbauer; R. Handberg; S. Hekker; C. Karoff; H. Lehmann; P. Mathias; S. Mathur; A. Miglio; J. Molenda-Zakowicz; B. Mosser; S.~J. Murphy; C. Régulo; V. Ripepi; D. Salabert; S.~G. Sousa; D. Stello; K. Uytterhoeven

doi:10.3847/0004-637X/831/1/17

Detection Of Solar-Like Oscillations, Observational Constraints, And Stellar Models For Θ Cyg, The Brightest Star Observed By The Kepler Mission

J.~A. Guzik, G. Houdek, W.~J. Chaplin, B. Smalley, D.~W. Kurtz, R.~L. Gilliland, F. Mullally, J.~F. Rowe, S.~T. Bryson, M.~D. Still, V. Antoci, T. Appourchaux, S. Basu, T.~R. Bedding, O. Benomar, R.~A. Garcia, D. Huber, H. Kjeldsen, D.~W. Latham, T.~S. MetcalfeP.~I. Pápics, T.~R. White, C. Aerts, J. Ballot, T.~S. Boyajian, M. Briquet, H. Bruntt, L.~A. Buchhave, T.~L. Campante, G. Catanzaro, J. Christensen-Dalsgaard, G.~R. Davies, G. Dou gan, D. Dragomir, A.~P. Doyle, Y. Elsworth, A. Frasca, P. Gaulme, M. Gruberbauer, R. Handberg, S. Hekker, C. Karoff, H. Lehmann, P. Mathias, S. Mathur, A. Miglio, J. Molenda-Zakowicz, B. Mosser, S.~J. Murphy, C. Régulo, V. Ripepi, D. Salabert, S.~G. Sousa, D. Stello, K. Uytterhoeven

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Abstract

_ Cygni is an F3 spectral-type main-sequence star with visual magnitude V=4.48. This star was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were obtained during Quarter 6 (June-September 2010) and subsequently in Quarters 8 and 12-17. We present analyses of the solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 oscillations in the range 1000-2700 μHz, with a large frequency separation of 83.9 ± 0.4 μHz, and frequency with maximum amplitude _max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, when combined with angular diameter measurements from interferometry and Hipparcos parallax, give Teff = 6697 ± 78 K, radius 1.49 ± 0.03 R⊙, [Fe/H] = -0.02 ± 0.06 dex, log g = 4.23 ± 0.03. We calculate stellar models matching the constraints using several methods, including using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses 1.35–1.39 M⊙ and ages 1.0–1.6 Gyr. _ Cyg’s Teff and log g place it cooler than the red edge of the Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The best-fitting models have envelope convection-zone base temperature of ∼320,000 to 395,000 K. The pulsation models show Dor gravity-mode pulsations driven by the convectiveblocking mechanism, with periods of 0.3 to 1 day (frequencies 11 to 33 μHz). However, gravity modes were not detected in the Kepler data; one signal at 1.776 c d−1 (20.56 μHz) may be attributable to a faint, possibly background, binary. Asteroseismic studies of _ Cyg, in conjunction with those for other A-F stars observed by Kepler and CoRoT, will help to improve stellar model physics to sort out the confusing relationship between _ Sct and Dor pulsations and their hybrids, and to test pulsation driving mechanisms.

Original language	English
Journal	The Astrophysical Journal
Volume	831
Issue number	1
DOIs	https://doi.org/10.3847/0004-637X/831/1/17
Publication status	Published - 21 Oct 2016

Keywords

Astrophysics - Solar and Stellar Astrophysics

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10.3847/0004-637X/831/1/17

Guzik_et_al_Detection_Solar-Like_Oscillations_Astrophysical_Journal
© 2016. The American Astronomical Society. All rights reserved. Final Version of Record available at: http://dx.doi.org/10.3847/0004-637X/831/1/17 Checked 23/1/2017
Final published version, 5.26 MBLicence: None: All rights reserved

Asteroseismology and Helioseismology at Birmingham and Queen Mary
Chaplin, B. (Principal Investigator), Elsworth, Y. (Co-Investigator) & Miglio, A. (Co-Investigator)
SCIENCE & TECHNOLOGY FACILITIES COUNCIL
1/04/15 → 30/09/18
Project: Research Councils

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Guzik, J. A., Houdek, G., Chaplin, W. J., Smalley, B., Kurtz, D. W., Gilliland, R. L., Mullally, F., Rowe, J. F., Bryson, S. T., Still, M. D., Antoci, V., Appourchaux, T., Basu, S., Bedding, T. R., Benomar, O., Garcia, R. A., Huber, D., Kjeldsen, H., Latham, D. W., ... Uytterhoeven, K. (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). https://doi.org/10.3847/0004-637X/831/1/17

@article{173f74985a4447b889114f76c5ca708b,

title = "Detection Of Solar-Like Oscillations, Observational Constraints, And Stellar Models For Θ Cyg, The Brightest Star Observed By The Kepler Mission",

abstract = "_ Cygni is an F3 spectral-type main-sequence star with visual magnitude V=4.48. This star was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were obtained during Quarter 6 (June-September 2010) and subsequently in Quarters 8 and 12-17. We present analyses of the solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 oscillations in the range 1000-2700 μHz, with a large frequency separation of 83.9 ± 0.4 μHz, and frequency with maximum amplitude _max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, when combined with angular diameter measurements from interferometry and Hipparcos parallax, give Teff = 6697 ± 78 K, radius 1.49 ± 0.03 R⊙, [Fe/H] = -0.02 ± 0.06 dex, log g = 4.23 ± 0.03. We calculate stellar models matching the constraints using several methods, including using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses 1.35–1.39 M⊙ and ages 1.0–1.6 Gyr. _ Cyg{\textquoteright}s Teff and log g place it cooler than the red edge of the Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The best-fitting models have envelope convection-zone base temperature of ∼320,000 to 395,000 K. The pulsation models show Dor gravity-mode pulsations driven by the convectiveblocking mechanism, with periods of 0.3 to 1 day (frequencies 11 to 33 μHz). However, gravity modes were not detected in the Kepler data; one signal at 1.776 c d−1 (20.56 μHz) may be attributable to a faint, possibly background, binary. Asteroseismic studies of _ Cyg, in conjunction with those for other A-F stars observed by Kepler and CoRoT, will help to improve stellar model physics to sort out the confusing relationship between _ Sct and Dor pulsations and their hybrids, and to test pulsation driving mechanisms. ",

keywords = "Astrophysics - Solar and Stellar Astrophysics",

author = "J.~A. Guzik and G. Houdek and W.~J. Chaplin and B. Smalley and D.~W. Kurtz and R.~L. Gilliland and F. Mullally and J.~F. Rowe and S.~T. Bryson and M.~D. Still and V. Antoci and T. Appourchaux and S. Basu and T.~R. Bedding and O. Benomar and R.~A. Garcia and D. Huber and H. Kjeldsen and D.~W. Latham and T.~S. Metcalfe and P.~I. P{\'a}pics and T.~R. White and C. Aerts and J. Ballot and T.~S. Boyajian and M. Briquet and H. Bruntt and L.~A. Buchhave and T.~L. Campante and G. Catanzaro and J. Christensen-Dalsgaard and G.~R. Davies and {Dou gan}, G. and D. Dragomir and A.~P. Doyle and Y. Elsworth and A. Frasca and P. Gaulme and M. Gruberbauer and R. Handberg and S. Hekker and C. Karoff and H. Lehmann and P. Mathias and S. Mathur and A. Miglio and J. Molenda-Zakowicz and B. Mosser and S.~J. Murphy and C. R{\'e}gulo and V. Ripepi and D. Salabert and S.~G. Sousa and D. Stello and K. Uytterhoeven",

year = "2016",

month = oct,

day = "21",

doi = "10.3847/0004-637X/831/1/17",

language = "English",

volume = "831",

journal = "The Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing Ltd",

number = "1",

}

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, Pápics, PI, White, TR, Aerts, C, Ballot, J, Boyajian, TS, Briquet, M, Bruntt, H, Buchhave, LA, Campante, TL, Catanzaro, G, Christensen-Dalsgaard, J, Davies, GR, Dou gan, G, Dragomir, D, Doyle, AP, Elsworth, Y, Frasca, A, Gaulme, P, Gruberbauer, M, Handberg, R, Hekker, S, Karoff, C, Lehmann, H, Mathias, P, Mathur, S, Miglio, A, Molenda-Zakowicz, J, Mosser, B, Murphy, SJ, Régulo, C, Ripepi, V, Salabert, D, Sousa, SG, Stello, D & Uytterhoeven, K 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, vol. 831, no. 1. https://doi.org/10.3847/0004-637X/831/1/17

TY - JOUR

T1 - Detection Of Solar-Like Oscillations, Observational Constraints, And Stellar Models For Θ Cyg, The Brightest Star Observed By The Kepler Mission

AU - Guzik, J.~A.

AU - Houdek, G.

AU - Chaplin, W.~J.

AU - Smalley, B.

AU - Kurtz, D.~W.

AU - Gilliland, R.~L.

AU - Mullally, F.

AU - Rowe, J.~F.

AU - Bryson, S.~T.

AU - Still, M.~D.

AU - Antoci, V.

AU - Appourchaux, T.

AU - Basu, S.

AU - Bedding, T.~R.

AU - Benomar, O.

AU - Garcia, R.~A.

AU - Huber, D.

AU - Kjeldsen, H.

AU - Latham, D.~W.

AU - Metcalfe, T.~S.

AU - Pápics, P.~I.

AU - White, T.~R.

AU - Aerts, C.

AU - Ballot, J.

AU - Boyajian, T.~S.

AU - Briquet, M.

AU - Bruntt, H.

AU - Buchhave, L.~A.

AU - Campante, T.~L.

AU - Catanzaro, G.

AU - Christensen-Dalsgaard, J.

AU - Davies, G.~R.

AU - Dou gan, G.

AU - Dragomir, D.

AU - Doyle, A.~P.

AU - Elsworth, Y.

AU - Frasca, A.

AU - Gaulme, P.

AU - Gruberbauer, M.

AU - Handberg, R.

AU - Hekker, S.

AU - Karoff, C.

AU - Lehmann, H.

AU - Mathias, P.

AU - Mathur, S.

AU - Miglio, A.

AU - Molenda-Zakowicz, J.

AU - Mosser, B.

AU - Murphy, S.~J.

AU - Régulo, C.

AU - Ripepi, V.

AU - Salabert, D.

AU - Sousa, S.~G.

AU - Stello, D.

AU - Uytterhoeven, K.

PY - 2016/10/21

Y1 - 2016/10/21

N2 - _ Cygni is an F3 spectral-type main-sequence star with visual magnitude V=4.48. This star was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were obtained during Quarter 6 (June-September 2010) and subsequently in Quarters 8 and 12-17. We present analyses of the solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 oscillations in the range 1000-2700 μHz, with a large frequency separation of 83.9 ± 0.4 μHz, and frequency with maximum amplitude _max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, when combined with angular diameter measurements from interferometry and Hipparcos parallax, give Teff = 6697 ± 78 K, radius 1.49 ± 0.03 R⊙, [Fe/H] = -0.02 ± 0.06 dex, log g = 4.23 ± 0.03. We calculate stellar models matching the constraints using several methods, including using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses 1.35–1.39 M⊙ and ages 1.0–1.6 Gyr. _ Cyg’s Teff and log g place it cooler than the red edge of the Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The best-fitting models have envelope convection-zone base temperature of ∼320,000 to 395,000 K. The pulsation models show Dor gravity-mode pulsations driven by the convectiveblocking mechanism, with periods of 0.3 to 1 day (frequencies 11 to 33 μHz). However, gravity modes were not detected in the Kepler data; one signal at 1.776 c d−1 (20.56 μHz) may be attributable to a faint, possibly background, binary. Asteroseismic studies of _ Cyg, in conjunction with those for other A-F stars observed by Kepler and CoRoT, will help to improve stellar model physics to sort out the confusing relationship between _ Sct and Dor pulsations and their hybrids, and to test pulsation driving mechanisms.

AB - _ Cygni is an F3 spectral-type main-sequence star with visual magnitude V=4.48. This star was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were obtained during Quarter 6 (June-September 2010) and subsequently in Quarters 8 and 12-17. We present analyses of the solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 oscillations in the range 1000-2700 μHz, with a large frequency separation of 83.9 ± 0.4 μHz, and frequency with maximum amplitude _max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, when combined with angular diameter measurements from interferometry and Hipparcos parallax, give Teff = 6697 ± 78 K, radius 1.49 ± 0.03 R⊙, [Fe/H] = -0.02 ± 0.06 dex, log g = 4.23 ± 0.03. We calculate stellar models matching the constraints using several methods, including using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses 1.35–1.39 M⊙ and ages 1.0–1.6 Gyr. _ Cyg’s Teff and log g place it cooler than the red edge of the Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The best-fitting models have envelope convection-zone base temperature of ∼320,000 to 395,000 K. The pulsation models show Dor gravity-mode pulsations driven by the convectiveblocking mechanism, with periods of 0.3 to 1 day (frequencies 11 to 33 μHz). However, gravity modes were not detected in the Kepler data; one signal at 1.776 c d−1 (20.56 μHz) may be attributable to a faint, possibly background, binary. Asteroseismic studies of _ Cyg, in conjunction with those for other A-F stars observed by Kepler and CoRoT, will help to improve stellar model physics to sort out the confusing relationship between _ Sct and Dor pulsations and their hybrids, and to test pulsation driving mechanisms.

KW - Astrophysics - Solar and Stellar Astrophysics

UR - http://arxiv.org/abs/1607.01035

U2 - 10.3847/0004-637X/831/1/17

DO - 10.3847/0004-637X/831/1/17

M3 - Article

SN - 0004-637X

VL - 831

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 1

ER -

Detection Of Solar-Like Oscillations, Observational Constraints, And Stellar Models For Θ Cyg, The Brightest Star Observed By The Kepler Mission

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