1. Beijing, March 20101 Variability of post-AGB objects R. Szczerba & M. Hajduk N. Copernicus Astronomical Center Toruń, Poland

2. Kunming, March 2010 2 NCAC TORUN TORUŃ - N. COPERNICUS (1473-1543)

3. 3 NCAC TORUN OVERVIEW Introduction: post-AGB objects ASAS & variability of post-AGBs Variability of 21 m emitting post-AGBs Concluding remarks

4. 4 Introduction: post-AGB objects

5. 5 (F.Herwig, 2005 – Mi = 2 Mo, Z=0.02) ‏

6. 6 Introduction Post-AGBs pulsate

7.  Prior to the IRAS satelite (1983), post-AGBs remained as an observational „missing link” in the post-MS evolution of low- and intermadiate-mass stars.  IRAS allowed to identify about 50 of them  Now we know about 470 (including RV Tau stars – counted as post-AGBs: Jura, 1986) post-AGBs see: http://www.ncac.torun/postabg2  Post-AGBs: some facts NCAC TORUN

8. 8 ASAS & variability of post-AGBs

9. ASAS & OGLE telescopes The All Sky Automated Survey (ASAS) system is fully automated system of telescopes located at Las Campanas, Chile. On site assistance by the OGLE observers (the OGLE telescope is visible in the background of the photograph).

10. ASAS ASAS is a low cost project dedicated to constant photometric monitoring of the whole available sky, which is approximately 10^7 stars brighter than 14 magnitude. The project's ultimate goal is detection and investigation of of any kind of the photometric variability. One of the main objectives of ASAS is to find and catalogue variable stars.

11. ASAS Presently, ASAS consists of two observing stations, one in LCO, Chile (since 1997) and the other on Haleakala, Maui, Hawaii (since 2006). Both are equipped with two wide-field 200/2.8 instruments, observing simultaneously in V and I band.

12. ASAS ASAS Sky Coverage (δ<28Deg North) (Pojmanski et al., AcA, 2005)

13. ASAS Southern hemisphere – observed for ~10 years now

14. ASAS ASAS photometry accuracy vs star brightness, (Pojmanski, AcA, 2002)

15.  Kiss et al. (2007) analyzed photometric (light curves) data for 29+2 (ASAS + NSVS) (suspected) binary post- AGBs from De Ruyter et a. (2006) to determine pulsational and orbital periods.  Almost half of the sample is composd of RV Tau- type variables.  They found a strong correlation between V-band amplitudes and T eff.  Post-AGBs with ASAS NCAC TORUN

16. Kiss et al. (2007) T eff is a good indicator of the post-AGB evolutionary phase open circles – single periodic stars triangles – multiperiodic / semiregular stars squares –variability due to orbital motion

17. Kiss et al. (2007) Post-AGB objects on H-R diagram together with “classical” instability strip from Christensn-Dalsgaard (2003)

18. 22 post-AGB stars from our catalogue (other than RV Tau type & no-analyzed by KISS et al (2007)) were detected in ASAS database.

19. Red Rectangle – known binary

20. Two stars have dominant period longer than ~150d – candidates for binaries: IRAS 07253-2001

21. IRAS 08005-2356

22. Some other show possible binary modulation in addition to the stellar pulsation – e.g. V4728 Sgr

23. Most of them show several frequencies with rather well defined dominant frequency, e.g. V0552 Pup

24. or BT Lib

25. Temperature (spectral type) was determined for 10 out of 22 object rather weak (no?) correlation of the period with the temperature, but …

26. Hrivnak et al. (2010, ApJ, 709, 1042) carried out ~14 years long V & R monitoring of 12 post-AGBs with 21 m emission

27. e.g., IRAS 22272+5435 – see: http://www.ncac.torun.p/postagb2

28. IRAS 22272+5435 – see: http://www.ncac.torun.p/postagb2

29. Hrivnak et al. (2010) V – the amplitude of the variations decrease with T eff

30. Hrivnak et al. (2010) P – period is becoming shorter when the object is hotter

31. 31 Concluding remarks

32.  All (?) post-AGBs are variable stars, with period from about 30 up to more than 150 days (!) – this upper limit is surprising since evolutionary calculations predict maximum period shorther than about 100 days.  Colder post-AGB objects have longer periods and the larger light variations (in agreement with the results of modelling by Fokin et al. 2001).  More model calculations, like those done by Fokin et al. (2001), especially for longer periods are needed.  Post-AGB stars are rather dim (mV>10-12 mag.), and due to their long periods, are (probably?) not good candidates for the SONG observations, but... Concluding remarks NCAC TORUN

33.  - there are several post-AGBs with mV < 7-8 mag., &  - while searching for plantes in crowded regions with SONG, we can get precise photometry for coincident post-AGBs as a by-product.  Concluding remarks NCAC TORUN