1 / 38

Aiying ZHOU 周 爱 英

Overview of Oscillating Binaries. —— Several Observational Aspects. Aiying ZHOU 周 爱 英. National Astronomical Observatories, CAS. 2010.03.31 Beijing. Light variations seems universal & much interesting. Every star varies ！. RRab. What are the Most Interesting Light Curves?. Puls. (A).

kolina
Download Presentation

Aiying ZHOU 周 爱 英

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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！

More Related