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. MetcalfeP. 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

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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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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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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, 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

Y1 - 2016/11/1

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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