A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler

S. Mathur, T. S. Metcalfe, M. Woitaszek, H. Bruntt, G. A. Verner, J. Christensen-Dalsgaard, O. L. Creevey, G. Dogan, S. Basu, C. Karoff, D. Stello, T. Appourchaux, T. L. Campante, W. J. Chaplin, R. A. García, T. R. Bedding, Othman Benomar, A. Bonanno, S. Deheuvels, Y. ElsworthP. Gaulme, J. A. Guzik, R. Handberg, S. Hekker, W. Herzberg, M. J.P.F.G. Monteiro, L. Piau, P. O. Quirion, C. Régulo, M. Roth, D. Salabert, A. Serenelli, M. J. Thompson, R. Trampedach, T. R. White, J. Ballot, I. M. Brandão, J. Molenda-Zakowicz, H. Kjeldsen, J. D. Twicken, K. Uddin, B. Wohler

Research output: Contribution to journalArticle

Abstract

Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their hoststars, but also a new window on stellar structure and evolution for the large sample of solar-typestars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ∼1% precision, and ages to ∼2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.

Original languageEnglish (US)
Article number152
JournalAstrophysical Journal
Volume749
Issue number2
DOIs
StatePublished - Apr 20 2012

Fingerprint

oscillation
stars
oscillations
radii
grids
stellar structure
asteroseismology
stellar evolution
extrasolar planets
signal-to-noise ratio
modeling
signal to noise ratios
telescopes
estimates
analysis
method

Keywords

  • methods: numerical
  • stars: evolution
  • stars: interiors
  • stars: oscillations

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Mathur, S., Metcalfe, T. S., Woitaszek, M., Bruntt, H., Verner, G. A., Christensen-Dalsgaard, J., ... Wohler, B. (2012). A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler. Astrophysical Journal, 749(2), [152]. https://doi.org/10.1088/0004-637X/749/2/152

A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler. / Mathur, S.; Metcalfe, T. S.; Woitaszek, M.; Bruntt, H.; Verner, G. A.; Christensen-Dalsgaard, J.; Creevey, O. L.; Dogan, G.; Basu, S.; Karoff, C.; Stello, D.; Appourchaux, T.; Campante, T. L.; Chaplin, W. J.; García, R. A.; Bedding, T. R.; Benomar, Othman; Bonanno, A.; Deheuvels, S.; Elsworth, Y.; Gaulme, P.; Guzik, J. A.; Handberg, R.; Hekker, S.; Herzberg, W.; Monteiro, M. J.P.F.G.; Piau, L.; Quirion, P. O.; Régulo, C.; Roth, M.; Salabert, D.; Serenelli, A.; Thompson, M. J.; Trampedach, R.; White, T. R.; Ballot, J.; Brandão, I. M.; Molenda-Zakowicz, J.; Kjeldsen, H.; Twicken, J. D.; Uddin, K.; Wohler, B.

In: Astrophysical Journal, Vol. 749, No. 2, 152, 20.04.2012.

Research output: Contribution to journalArticle

Mathur, S, Metcalfe, TS, Woitaszek, M, Bruntt, H, Verner, GA, Christensen-Dalsgaard, J, Creevey, OL, Dogan, G, Basu, S, Karoff, C, Stello, D, Appourchaux, T, Campante, TL, Chaplin, WJ, García, RA, Bedding, TR, Benomar, O, Bonanno, A, Deheuvels, S, Elsworth, Y, Gaulme, P, Guzik, JA, Handberg, R, Hekker, S, Herzberg, W, Monteiro, MJPFG, Piau, L, Quirion, PO, Régulo, C, Roth, M, Salabert, D, Serenelli, A, Thompson, MJ, Trampedach, R, White, TR, Ballot, J, Brandão, IM, Molenda-Zakowicz, J, Kjeldsen, H, Twicken, JD, Uddin, K & Wohler, B 2012, 'A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler', Astrophysical Journal, vol. 749, no. 2, 152. https://doi.org/10.1088/0004-637X/749/2/152
Mathur S, Metcalfe TS, Woitaszek M, Bruntt H, Verner GA, Christensen-Dalsgaard J et al. A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler. Astrophysical Journal. 2012 Apr 20;749(2). 152. https://doi.org/10.1088/0004-637X/749/2/152
Mathur, S. ; Metcalfe, T. S. ; Woitaszek, M. ; Bruntt, H. ; Verner, G. A. ; Christensen-Dalsgaard, J. ; Creevey, O. L. ; Dogan, G. ; Basu, S. ; Karoff, C. ; Stello, D. ; Appourchaux, T. ; Campante, T. L. ; Chaplin, W. J. ; García, R. A. ; Bedding, T. R. ; Benomar, Othman ; Bonanno, A. ; Deheuvels, S. ; Elsworth, Y. ; Gaulme, P. ; Guzik, J. A. ; Handberg, R. ; Hekker, S. ; Herzberg, W. ; Monteiro, M. J.P.F.G. ; Piau, L. ; Quirion, P. O. ; Régulo, C. ; Roth, M. ; Salabert, D. ; Serenelli, A. ; Thompson, M. J. ; Trampedach, R. ; White, T. R. ; Ballot, J. ; Brandão, I. M. ; Molenda-Zakowicz, J. ; Kjeldsen, H. ; Twicken, J. D. ; Uddin, K. ; Wohler, B. / A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler. In: Astrophysical Journal. 2012 ; Vol. 749, No. 2.
@article{c668cb4f8b664801a964707bae800d49,
title = "A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler",
abstract = "Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their hoststars, but also a new window on stellar structure and evolution for the large sample of solar-typestars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ∼1{\%} precision, and ages to ∼2.5{\%} precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.",
keywords = "methods: numerical, stars: evolution, stars: interiors, stars: oscillations",
author = "S. Mathur and Metcalfe, {T. S.} and M. Woitaszek and H. Bruntt and Verner, {G. A.} and J. Christensen-Dalsgaard and Creevey, {O. L.} and G. Dogan and S. Basu and C. Karoff and D. Stello and T. Appourchaux and Campante, {T. L.} and Chaplin, {W. J.} and Garc{\'i}a, {R. A.} and Bedding, {T. R.} and Othman Benomar and A. Bonanno and S. Deheuvels and Y. Elsworth and P. Gaulme and Guzik, {J. A.} and R. Handberg and S. Hekker and W. Herzberg and Monteiro, {M. J.P.F.G.} and L. Piau and Quirion, {P. O.} and C. R{\'e}gulo and M. Roth and D. Salabert and A. Serenelli and Thompson, {M. J.} and R. Trampedach and White, {T. R.} and J. Ballot and Brand{\~a}o, {I. M.} and J. Molenda-Zakowicz and H. Kjeldsen and Twicken, {J. D.} and K. Uddin and B. Wohler",
year = "2012",
month = "4",
day = "20",
doi = "10.1088/0004-637X/749/2/152",
language = "English (US)",
volume = "749",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler

AU - Mathur, S.

AU - Metcalfe, T. S.

AU - Woitaszek, M.

AU - Bruntt, H.

AU - Verner, G. A.

AU - Christensen-Dalsgaard, J.

AU - Creevey, O. L.

AU - Dogan, G.

AU - Basu, S.

AU - Karoff, C.

AU - Stello, D.

AU - Appourchaux, T.

AU - Campante, T. L.

AU - Chaplin, W. J.

AU - García, R. A.

AU - Bedding, T. R.

AU - Benomar, Othman

AU - Bonanno, A.

AU - Deheuvels, S.

AU - Elsworth, Y.

AU - Gaulme, P.

AU - Guzik, J. A.

AU - Handberg, R.

AU - Hekker, S.

AU - Herzberg, W.

AU - Monteiro, M. J.P.F.G.

AU - Piau, L.

AU - Quirion, P. O.

AU - Régulo, C.

AU - Roth, M.

AU - Salabert, D.

AU - Serenelli, A.

AU - Thompson, M. J.

AU - Trampedach, R.

AU - White, T. R.

AU - Ballot, J.

AU - Brandão, I. M.

AU - Molenda-Zakowicz, J.

AU - Kjeldsen, H.

AU - Twicken, J. D.

AU - Uddin, K.

AU - Wohler, B.

PY - 2012/4/20

Y1 - 2012/4/20

N2 - Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their hoststars, but also a new window on stellar structure and evolution for the large sample of solar-typestars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ∼1% precision, and ages to ∼2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.

AB - Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their hoststars, but also a new window on stellar structure and evolution for the large sample of solar-typestars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ∼1% precision, and ages to ∼2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.

KW - methods: numerical

KW - stars: evolution

KW - stars: interiors

KW - stars: oscillations

UR - http://www.scopus.com/inward/record.url?scp=84859622474&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84859622474&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/749/2/152

DO - 10.1088/0004-637X/749/2/152

M3 - Article

VL - 749

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 152

ER -