A diagnostic diagram for γ Doradus variables and slowly pulsating B-type stars

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  • M. Takata, PSL Research University, University of Tokyo
  • ,
  • R. M. Ouazzani, PSL Research University
  • ,
  • H. Saio, Tohoku University
  • ,
  • S. Christophe, PSL Research University
  • ,
  • J. Ballot, Universite Toulouse III - Paul Sabatier
  • ,
  • V. Antoci
  • ,
  • S. J.A.J. Salmon, University of Liege
  • ,
  • K. Hijikawa, University of Tokyo

Pulsating variables of γ Doradus type (γ Dor) and slowly pulsating B-type (SPB) stars are found on and near the main sequence with typical periods varying between one and several days, making them rather hard to detect from the ground. It is only with space missions such as CoRoT and Kepler that we became truly capable of determining their oscillation frequencies with enough precision to perform in-depth analyses. Here we present an efficient and easy-to-implement seismic tool, in which the frequency (ν) and the square root of the frequency difference ($ \sqrt{\Delta \nu} $) are plotted against each other as the abscissa and the ordinate, respectively. This allows us to immediately (1) perform mode identification; (2) estimate the average rotation rate and the characteristic period of gravity modes; and (3) recognise certain physical effects, including buoyancy glitches and avoided crossings. This diagnostic tool can only be applied to prograde sectoral g modes. To validate the tool presented here, we used stellar models and also applied it to three γ Dor (KIC 12066947, KIC 5608334 and KIC 4846809) and one SPB star (KIC 3459297), all observed with Kepler. Furthermore, we show that the rotation rates determined using this new tool are consistent with the results of previous studies.

Original languageEnglish
Article numberA106
JournalAstronomy and Astrophysics
Number of pages15
Publication statusPublished - 2020

    Research areas

  • Asteroseismology, Methods: data analysis, Stars: oscillations, Stars: rotation

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