1. Changes of light curve parameters of LPVs and classification of Miras and semiregular variables KOLOS-2015 V.I. Marsakova, Odessa National University

2. Mira-type variables: pulsating red giants T Cep

3. Semiregular variables: pulsating red giants and supergiants AF Cyg

4. Observations We have used observations from the databases of the  French Association of Variable Stars Observers (AFOEV)  Variable Stars Observers League of Japan (VSOLJ)  American Association of Variable Star Observers (AAVSO), which allow to study the variability of these stars during the time interval of about 100 years. We have used observations from the databases of the  French Association of Variable Stars Observers (AFOEV)  Variable Stars Observers League of Japan (VSOLJ)  American Association of Variable Star Observers (AAVSO), which allow to study the variability of these stars during the time interval of about 100 years.

5. Methods We have used:  “Asymptotic parabolae” and “running parabolae” fitting to determine the characteristics of extrema  Trigonometrical polynomial to obtain the characteristics of the mean phase light curves  Wavelet analysis and “running sines” to study the stability of the periods and the light curves  Andronov I.L., AsAp Suppl., 1997, V. 124, 207.  Andronov I.L. ASP Conf. Ser. 2003, V. 229 P.391  Chinarova L.L. Odessa Astron. Publ. 2010. V. 23. P. 25.  Marsakova V.I., Andronov I.L. ASP Conf. Ser. 2000. V. 203. P. 131.  Andronov I.L., Marsakova V.I. Astrophysics. 2006. V.49. P. 370.  Kudashkina L.S., Andronov I.L., Odessa Astron. Publ., 1996, V. 9, 108. We have used:  “Asymptotic parabolae” and “running parabolae” fitting to determine the characteristics of extrema  Trigonometrical polynomial to obtain the characteristics of the mean phase light curves  Wavelet analysis and “running sines” to study the stability of the periods and the light curves  Andronov I.L., AsAp Suppl., 1997, V. 124, 207.  Andronov I.L. ASP Conf. Ser. 2003, V. 229 P.391  Chinarova L.L. Odessa Astron. Publ. 2010. V. 23. P. 25.  Marsakova V.I., Andronov I.L. ASP Conf. Ser. 2000. V. 203. P. 131.  Andronov I.L., Marsakova V.I. Astrophysics. 2006. V.49. P. 370.  Kudashkina L.S., Andronov I.L., Odessa Astron. Publ., 1996, V. 9, 108.

6. 1.Small irregular period variations ( C 7) Have some variables of C and S spectral classes and variables with multiperiodicity O-C

7. V Aur (C6) O-C J.D. -2400000

8. R Cyg (S2) O-C J.D. -2400000

9. 2. Switching of similar values of the period with sawtooth O-C curves

10. R Boo O-C J.D. -2400000

11. R Cas O-C J.D. -2400000

12. X Cas  Cyg O-C J.D. -2400000

13. R Dra O-C

14. X Oph O-C J.D. -2400000

15. Switching of similar values of the period with sawtooth O-C curves There are not dependence on the main pulsational period

16. 3. Smooth cyclic at timescale approximately 17000–22000 days

17. are acompanied changes of the shape of the light curve

18. T Cep Results of cross-correlation analysis

19. V Cas O-C J.D. -2400000

20. U Cyg O-C J.D. -2400000

21. R UMa O-C J.D. -2400000

22. U UMi O-C J.D. -2400000

23. Smooth cyclic at timescale approximately 17000–23000 days

24. For comparison: Switching of similar values of the period with sawtooth O-C curves

25. 4. Progressive changes (continuous changes of the same sign)

26. Residuals from parabola are sawtooth

29. Luminositiy variation during the helium-flash stage Wood P.R., Zarro D.M. Astrophys. J., 1981, V. 247, P. 247.

30. Superposition of the effects  Thomas Karlsson (Swedish Variable Observations database): http://var.astronet.se/ mirainfooc.http://var.astronet.se/ mirainfooc. AFOEV+VSOLJ J.D. -2400000

31. The red dots are maxima that are fitted from observations, the lightblue are maxima published by AAVSO and the darkblue are maxima collected from various other published sources. The fitted maxima are based on observation data from the organizations AAVSO, AFOEV, VSOLJ and BAA/VSS using approimation by 12 order polynomial fit to the mean lightcurve at maximum AFOEV+VSOLJ

32. J.D. -2400000

33. Smooth cyclic or progressive changes? 546.2466.2 350.5

34. Mira-type variability of S Aql before JD 2450000 5.Multiperiodicity. S Aql Variability of S Aql : with trigonometric polynomial fit (with two periods 146.7 d (4 harmonics), 245.2 d (2 harmonics)) 147 245 104.6 frequency S(f) “semiregular” interval

35. Multiperiodicity: S Aql smoothing curve phase Running sines: Phase trends J.D. -2400000

36. Multiperiodicity: Y Per Running sines 769 245.3 149.4 129 253 247.3 147.6 Phase trend

37. VariableP 1, (S)P 2, (S)Period ratioGCVS classification GCVS Spectral class T Col226.1 (0.60) 229.8 (0.11) 139.6 (0.06)1.62MM3e-M6e DN Her225.3 (0.52) 230.7 (0.18) 139.3 (0.13)1.62MM6.5 EL Lyr235.8 (0.57) 230.8 (0.31) 143.3 (0.20)1.65 1.61 M S Tri249.5 (0.16) 240.4 (0.08) 148.1 (0.07)1.68 1.62 MM2e Y Per253 (0.32). 245.3 (0.08) 149.4 (0.04)1.70MC4,3e S Sex254.7 (0.32) 258.8 (0.26) 264.6 (0.20) 150 (0.15)1.70 1.72 1.76 MM2-M5e UZ Hya266.3 (0.59)153.8 (0.2)1.73MM4e AN Peg272.0 (0.6)156.0 (0.26)1.74MM5 S Aql146.7(0.48)245.2 (0.18)1.67SRaM3-M5.5e RU And234.3 (0.08) 245.7 (0.07) 124,7 (0,03) 146,8 (0,02) 1.87 1.67 SRaM5-M6e V Boo257.5(0.49) 260 (0.17) 151 (0.07)1.70 SRaM6e X Mon257.6 (0.37) 260.8 (0.07) 151.1 (0.06)1.71SRaM1e-M6ep RR Her236.7 (0.24) 261.3 (0.05) 143.5 (0.05)1.61SRbC5,7e-8,1e ST Her256.5 (0.07)150.8 (0.06) 152.1 (0.06) 1.70 1.68 SRbM6-M7 S Sct268.6 (0.03)151.3 (0.02)1.77SRbC6,4 Multiperiodicity 250/150

38. O-C S Aql J.D. -2400000

39. O-C V Boo Phase trend J.D. -2400000

40. Amplitude changes (SRA) (M)

41. S PER, SRC J.D. -2400000 mm

42. A diagram of spectral type versus relative amplitude scatter. The subtype increases rightwards. BG Cyg S Aql W Hya S Tri T Ari T CVn,

43. A diagram of the relative period scatter versus the relative amplitude scatter. S Aql, S Per S Tri T Ari W Hya BG Cyg T CVn

44. Main publications  Marsakova V.I. Variations of light curve parameters in Miras with progressive period changes. // Astron. Soc. Pacif. Conference Series. – 2000. – 203, 130  Marsakova V.I., Andronov I.L. Unusual secondary variations in the Mira star T Cep. // Astron. Soc. Pacif. Conference Series. – 2000. – 203, 131–132  Marsakova V.I., Andronov I.L. Variability of long-period pulsating stars. II. Additional parameters for classifying stars. – 2006. – Astrophysics, 49, 506-522  Marsakova V.I., Andronov I.L. Miras or SRa’s – the transient type variables. // Odessa Astronomical Publications, 2012, 25, № 1, p. 60-64.  Marsakova V.I. T Cep, U UMi, Z Sco – Mira-type variables with cyclic period changes // Odessa Astronomical Publications, 2013, 26, № 1, p. 78-82.  Marsakova V.I. Secular Variations of the Photometric Parameters of Mira Ceti Variables and Semiregular Variables. Bulletin of the Crimean Astrophysical Observatory, 2014, 110, 23–29.  Marsakova V.I. Characteristics of the Period Changes in Mira-type Variables // Odessa Astronomical Publications, 2014, v.27, № 1, 225-234.  Kudashkina L.S., Marsakova V.I. Statistical Studies of Long – Period Variable Stars in Odessa // Częstochowski Kalendarz Astronomiczny-2015  Częstochowa, 2014. .  Andronov I. L., Marsakova V. I., Kudashkina L. S., Chinarova L. L.. Inter-Longitude Astronomy project: long period variable stars // Advances in Astronomy and Space Physics, 4, 3-8 (2014).  Marsakova V.I. Variations of light curve parameters in Miras with progressive period changes. // Astron. Soc. Pacif. Conference Series. – 2000. – 203, 130  Marsakova V.I., Andronov I.L. Unusual secondary variations in the Mira star T Cep. // Astron. Soc. Pacif. Conference Series. – 2000. – 203, 131–132  Marsakova V.I., Andronov I.L. Variability of long-period pulsating stars. II. Additional parameters for classifying stars. – 2006. – Astrophysics, 49, 506-522  Marsakova V.I., Andronov I.L. Miras or SRa’s – the transient type variables. // Odessa Astronomical Publications, 2012, 25, № 1, p. 60-64.  Marsakova V.I. T Cep, U UMi, Z Sco – Mira-type variables with cyclic period changes // Odessa Astronomical Publications, 2013, 26, № 1, p. 78-82.  Marsakova V.I. Secular Variations of the Photometric Parameters of Mira Ceti Variables and Semiregular Variables. Bulletin of the Crimean Astrophysical Observatory, 2014, 110, 23–29.  Marsakova V.I. Characteristics of the Period Changes in Mira-type Variables // Odessa Astronomical Publications, 2014, v.27, № 1, 225-234.  Kudashkina L.S., Marsakova V.I. Statistical Studies of Long – Period Variable Stars in Odessa // Częstochowski Kalendarz Astronomiczny-2015  Częstochowa, 2014. .  Andronov I. L., Marsakova V. I., Kudashkina L. S., Chinarova L. L.. Inter-Longitude Astronomy project: long period variable stars // Advances in Astronomy and Space Physics, 4, 3-8 (2014).

45. Conclusion 1. Several types of period variations for Mira-type variables were separated:  small irregular period variations,  switching of similar values of the period with sawtooth O-C curves (amplitude is smaller),  smooth cyclic at timescale approximately 17000–22000 days (amplitude is higher, shape of curve is changed),  progressive (continuous changes of the same sign),  effects of multiperiodicity. 2. Some multiperiodic variables can be classified as ones belonging to a transient type between Mira-type and semiregular variables 1. Several types of period variations for Mira-type variables were separated:  small irregular period variations,  switching of similar values of the period with sawtooth O-C curves (amplitude is smaller),  smooth cyclic at timescale approximately 17000–22000 days (amplitude is higher, shape of curve is changed),  progressive (continuous changes of the same sign),  effects of multiperiodicity. 2. Some multiperiodic variables can be classified as ones belonging to a transient type between Mira-type and semiregular variables

46. Author are grateful to L.S. Kudashkina and I.L. Andronov for collaboration and discussions. Thank You for attention!