Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355

C. Jiang; B.W. Jiang; Jørgen Christensen-Dalsgaard; T.R. Bedding; D. Stello; D. Huber; Søren Frandsen; Hans Kjeldsen; Christoffer Karoff; B. Mosser; P. Demarque; M.N. Fanelli; K. Kinemuchi; F. Mullally

doi:10.1088/0004-637X/742/2/120

Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355

C. Jiang, B.W. Jiang, Jørgen Christensen-Dalsgaard, T.R. Bedding, D. Stello, D. Huber, Søren Frandsen, Hans Kjeldsen, Christoffer Karoff, B. Mosser, P. Demarque, M.N. Fanelli, K. Kinemuchi, F. Mullally

Department of Physics and Astronomy

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaper › Journal article › Research › peer-review

27 Citations (Scopus)

Abstract

We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and νmax to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M ☉) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.

Original language	English
Journal	Astrophysical Journal
Volume	742
Issue	2
Pages (from-to)	Article id. 120
ISSN	0004-637X
DOIs	https://doi.org/10.1088/0004-637X/742/2/120
Publication status	Published - 2011

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Jiang, C., Jiang, B. W., Christensen-Dalsgaard, J., Bedding, T. R., Stello, D., Huber, D., Frandsen, S., Kjeldsen, H., Karoff, C., Mosser, B., Demarque, P., Fanelli, M. N., Kinemuchi, K., & Mullally, F. (2011). Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355. Astrophysical Journal, 742(2), Article id. 120. https://doi.org/10.1088/0004-637X/742/2/120

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title = "Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355",

abstract = "We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and νmax to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M ☉) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase. ",

author = "C. Jiang and B.W. Jiang and J{\o}rgen Christensen-Dalsgaard and T.R. Bedding and D. Stello and D. Huber and S{\o}ren Frandsen and Hans Kjeldsen and Christoffer Karoff and B. Mosser and P. Demarque and M.N. Fanelli and K. Kinemuchi and F. Mullally",

year = "2011",

doi = "10.1088/0004-637X/742/2/120",

language = "English",

volume = "742",

pages = "Article id. 120",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

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Jiang, C, Jiang, BW, Christensen-Dalsgaard, J, Bedding, TR, Stello, D, Huber, D, Frandsen, S , Kjeldsen, H , Karoff, C, Mosser, B, Demarque, P, Fanelli, MN, Kinemuchi, K & Mullally, F 2011, 'Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355', Astrophysical Journal, vol. 742, no. 2, pp. Article id. 120. https://doi.org/10.1088/0004-637X/742/2/120

Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355. / Jiang, C.; Jiang, B.W.; Christensen-Dalsgaard, Jørgen et al.
In: Astrophysical Journal, Vol. 742, No. 2, 2011, p. Article id. 120.

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaper › Journal article › Research › peer-review

TY - JOUR

T1 - Modeling Kepler Observations of Solar-like Oscillations in the Red Giant Star HD 186355

AU - Jiang, C.

AU - Jiang, B.W.

AU - Christensen-Dalsgaard, Jørgen

AU - Bedding, T.R.

AU - Stello, D.

AU - Huber, D.

AU - Frandsen, Søren

AU - Kjeldsen, Hans

AU - Karoff, Christoffer

AU - Mosser, B.

AU - Demarque, P.

AU - Fanelli, M.N.

AU - Kinemuchi, K.

AU - Mullally, F.

PY - 2011

Y1 - 2011

N2 - We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and νmax to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M ☉) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.

AB - We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and νmax to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M ☉) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.

U2 - 10.1088/0004-637X/742/2/120

DO - 10.1088/0004-637X/742/2/120

M3 - Journal article

SN - 0004-637X

VL - 742

SP - Article id. 120

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -