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Exploring the Intriguing Universe of Oscillating Binaries: Observational Insights

This study delves into the fascinating phenomena of oscillating binary stars, focusing on the observational characteristics and light variations associated with them. The discussion includes the behavior of pulsating components within eclipsing binaries and their implications for understanding stellar evolution. We explore the differences in pulsation characteristics compared to single stars and highlight the advantages of studying these systems, such as accurate mass and radius determination, and the ability to identify pulsation modes during eclipses. Join us as we uncover the complexities of binary systems and their role in astrophysical research.

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Exploring the Intriguing Universe of Oscillating Binaries: Observational Insights

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  1. Overview of Oscillating Binaries —— Several Observational Aspects Aiying ZHOU 周 爱 英 National Astronomical Observatories, CAS 2010.03.31 Beijing

  2. Light variations seems universal & much interesting Every star varies！

  3. RRab

  4. What are the Most Interesting Light Curves?

  5. Puls. (A) Orbital motion

  6. Solar-like oscillation LC for the parent star of CoRoT-exo-2b, 1.4RJ, 3.5MJ, 140d, ±0m.00016 78 transits Porb =1d.74

  7. Eclipsing Binaries with Pulsating Components

  8. Interests in such studies • If no mechanism damping pulsations in close binaries, percentage of pulsating stars expected among A-F components of detached & semi-detached eclipsing binaries should be at least the same as for single A-F type stars. • Pulsation characteristics of such systems are similar to those of single pulsators, but their evolutions are quite different due to mass accretion.

  9. Advantages in such studies • Possibility of precise mass and radius determinations • Possibility of mode identification during the eclipse orbital phases using the observed pulsational amplitude and phase changes (Nather & Robinson 1974, ApJ, 190, 637). • Precise estimation of the accretion rate using the pulsation period changes of the gainer/accreting star caused by accretion. …… Ref.: 1. Aerts et al. 2004, ASP Conf. Ser. 318, 325 2. Lampens P. 2006, ASP Conf. Ser. 349, 153

  10. δScuti in an Algol-type binary (oEA): AB Cas Puls. (A) Orbital motion

  11. The A-F spectral type, mass-accreting, main-sequence pulsating stars in semi-detached Algol-type eclipsing binary systems, i.e. oscillating EA (oEA)

  12. They cataloged: • 25 DCST-type oEA: 20 semidetached +4 detached +1 unclassified • 90 semidetached + 71 detached + 36 from Hipparcos in theδScuti region of H-R diagram.

  13. 25 +197

  14. How many now ?

  15. In summary, • > 72, DSCT–type oEA • > 100, All kinds, oscillating E. B. • > 420, various binary/multiple stellar systems with Puls. Comp.

  16. Interesting works • How can binarity modify the pulsational properties? In what manner? • How can binarity/multiplicity help to identify the pulsation modes? • Search for pulsating M,K giants and subgaint stars in E. B. • Search for extra-solar planets around a pulsator. • Search for extragalactic E. B. with Puls. Comp. • Search for RR in E. B.

  17. Summary • Why • Statistics • Furture works

  18. This talk is based on Zhou A.-Y., 2010, arXiv:1002.2729 (to be updated) Thanks！

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