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Characteristics of Oscillations in G-type Giants - Convection Zone in giants -

Characteristics of Oscillations in G-type Giants - Convection Zone in giants -. 安藤裕康 (Ando Hiroyasu) 坪井優介 (Tsuboi Yusuke) 神戸栄治 (Kambe Eiji) 佐藤文衛 (Sato Bun’ei). 2009 年 10 月 7 日. Objective. Internal Structure via Oscillations. Helioseismology and Asteroseismology

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Characteristics of Oscillations in G-type Giants - Convection Zone in giants -

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  1. Characteristics of Oscillations in G-type Giants - Convection Zone in giants - 安藤裕康(Ando Hiroyasu) 坪井優介(Tsuboi Yusuke) 神戸栄治(Kambe Eiji) 佐藤文衛(Sato Bun’ei) 2009年10月7日

  2. Objective Internal Structure via Oscillations Helioseismology and Asteroseismology Ex. Sun, α Cen A,B, 70 Oph Extend to Sub-giants and giants Excitation Mechanism Convective motion still actives in giants ?

  3. Present status of oscillations in giants giants subgiants dwarfs ξHya and εOph Propose observation of oscillations in G-type giants

  4. Characteristics of oscillations even odd Echelle diagram for frequency Solar 5 min. oscillations

  5. Scaling laws

  6. αCen A at VLT and AAT (Butler et al. 2004)

  7. Stellar parameters for Observational objects（G-type giants）　

  8. Stars with extra-solar planet Some relation between planet-hosting and oscillation ?

  9. ζ Hya 11 Com ε Tau η Her

  10. Log g ζ Hya 2.30 11 Com 2.51 ε Tau 2.57 η Her 2.79

  11. ζ Hya 11 Com ε Tau η Her

  12. Summary of observations

  13. Parameters for Solar-like oscillation stars

  14. Scaling law for νmax

  15. Scaling law △ν

  16. Damping time

  17. Summary of characteristics of Oscillations in G giants 1　（ν max, △ν) follows scaling law 2echelle diagram of mode frequencies 　　　＝＞　detect not only radial oscillations, but also non- radial oscillations ３　Damping time is around 2 days 　　　（not all eigen modes is excited simultaneously） ４　Detected oscillations are solar-like oscillations 5 Oscillations have no correlation with planet-hovering stars

  18. One unexpected results Non-radial oscillations are detected as many as in dwarfs

  19. ZAMS stage P-region and G-region separated P G Subgiant stage Weak resonance

  20. Giant stage • Strong resonance • Amplitude reduced at • surface P G If convective zone is deeper, P-region and G-region separated Non-radial modes easily detectable

  21. To expain the observation, One possibility is that surface convection zone is deeper than predicted by current convective theory

  22. Thank you

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