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, Othman Benomar, R. A. Garcia, D. Huber, H. Kjeldsen, D. W. Latham, T. S. Metcalfe & 35 others P. I. P�pics, 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. Dogan, 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. R�gulo, V. Ripepi, D. Salabert, S. G. Sousa, D. Stello, K. Uytterhoeven

    Research output: Contribution to journalArticle

    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 o, [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 o 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.

    Original languageEnglish (US)
    Article number17
    JournalAstrophysical Journal
    Volume831
    Issue number1
    DOIs
    StatePublished - Nov 1 2016

    Fingerprint

    solar oscillations
    oscillation
    gravity
    gravitation
    cycles
    modeling
    stellar models
    main sequence stars
    spacecraft
    coolers
    apertures
    stars
    oscillations
    radii

    Keywords

    • asteroseismology
    • stars: fundamental parameters
    • stars: interiors
    • stars: solar-type

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    DETECTION of SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, and STELLAR MODELS for θ CYG, the BRIGHTEST STAR OBSERVED by the KEPLER MISSION. / 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, Othman; Garcia, R. A.; Huber, D.; Kjeldsen, H.; Latham, D. W.; Metcalfe, T. S.; P�pics, P. I.; White, T. R.; Aerts, C.; Ballot, J.; Boyajian, T. S.; Briquet, M.; Bruntt, H.; Buchhave, L. A.; Campante, T. L.; Catanzaro, G.; Christensen-Dalsgaard, J.; Davies, G. R.; Dogan, G.; Dragomir, D.; Doyle, A. P.; 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, S. J.; R�gulo, C.; Ripepi, V.; Salabert, D.; Sousa, S. G.; Stello, D.; Uytterhoeven, K.

    In: Astrophysical Journal, Vol. 831, No. 1, 17, 01.11.2016.

    Research output: Contribution to journalArticle

    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, P�pics, 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, S, Karoff, C, Lehmann, H, Mathias, P, Mathur, S, Miglio, A, Molenda-Zakowicz, J, Mosser, B, Murphy, SJ, R�gulo, 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', Astrophysical Journal, vol. 831, no. 1, 17. https://doi.org/10.3847/0004-637X/831/1/17
    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, Othman ; Garcia, R. A. ; Huber, D. ; Kjeldsen, H. ; Latham, D. W. ; Metcalfe, T. S. ; P�pics, P. I. ; White, T. R. ; Aerts, C. ; Ballot, J. ; Boyajian, T. S. ; Briquet, M. ; Bruntt, H. ; Buchhave, L. A. ; Campante, T. L. ; Catanzaro, G. ; Christensen-Dalsgaard, J. ; Davies, G. R. ; Dogan, G. ; Dragomir, D. ; Doyle, A. P. ; 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, S. J. ; R�gulo, C. ; Ripepi, V. ; Salabert, D. ; Sousa, S. G. ; Stello, D. ; Uytterhoeven, K. / DETECTION of SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, and STELLAR MODELS for θ CYG, the BRIGHTEST STAR OBSERVED by the KEPLER MISSION. In: Astrophysical Journal. 2016 ; Vol. 831, No. 1.
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    title = "DETECTION of SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, and STELLAR MODELS for θ CYG, the BRIGHTEST STAR OBSERVED by the KEPLER MISSION",
    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 {\"i}¿½ 0.4 μHz, and maximum oscillation amplitude at frequency ν max = 1829 {\"i}¿½ 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T eff = 6697 {\"i}¿½ 78 K, radius 1.49 {\"i}¿½ 0.03 R o, [Fe/H] = -0.02 {\"i}¿½ 0.06 dex, and log g = 4.23 {\"i}¿½ 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 o 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.",
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    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, Othman

    AU - Garcia, R. A.

    AU - Huber, D.

    AU - Kjeldsen, H.

    AU - Latham, D. W.

    AU - Metcalfe, T. S.

    AU - P�pics, 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 - Dogan, 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 - R�gulo, C.

    AU - Ripepi, V.

    AU - Salabert, D.

    AU - Sousa, S. G.

    AU - Stello, D.

    AU - Uytterhoeven, K.

    PY - 2016/11/1

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    N2 - 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 o, [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 o 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.

    AB - 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 o, [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 o 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.

    KW - asteroseismology

    KW - stars: fundamental parameters

    KW - stars: interiors

    KW - stars: solar-type

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