1. ASTEROSEISMOLOGY CoRoT session, January 13, 2007 Jadwiga Daszyńska-Daszkiewicz Instytut Astronomiczny, Uniwersytet Wrocławski

2. European Helio- and Asteroseismology Network

3. Participants

4. HELAS Activities: Global Helioseismology Local Helioseismology Local Helioseismology Asteroseismology Asteroseismology Public Outreach Public Outreach

5. CoRoT Mission

6. Sir Arthur Eddington (1882 – 1944) „At first sight it would seem that the deep interior of the sun and stars is less accessible to scientific investigation than any other region of the universe.”

7. Asteroseismology Investigation of stellar interiors by means of the oscillation frequencies

8. aster – aster – from Greek means star seismos – seismos – Gr. quake, tremor logos – logos – Gr. word, reason Helioseismology helios – helios – Gr. Sun

9. Changes of the brightness and/or the radial velocity are the observed evidences of pulsations. Pulsating star - star in which variability is due to pulsations, i.e. acoustic and/or gravity waves propagating in its envelope and interior.

10. WHY STARS PULSATE ?

11. 1. self-excitation 2. excitation by an external force Ad. 1. there are regions in a star which work like a heat engine, e.g. pulsation of classical Cepheids Ad. 2. stochastic excitation by turbulent convection in the near- surface regions, e.g. solar-like oscillations

12. When a Cepheid envelope begins to shrink (red arrows), it is almost transparent for the outgoing radiation (brown arrows). This phase corresponds to the onset of the compression stroke in an internal combustion engine. In the phase of maximum compression the envelope absorbs outgoing radiation and begins to expand. This phase corresponds to the ignition at the beginning of the combustion stroke.

14. The driving zone has to be located at an optimal geometrical depth in the stellar envelope. shallow The driving region located too shallow  the amount of the energy absorbed by thin matter will be insufficient to maintain pulsations deep The driving region located too deep  the amplitude of the temperature variations is very small and the layer will absorb too small amount of energy to be efficient

16. log T eff log (L/L  ) A star hotter than T eff ~7500K has regions of partial ionization too close to the surface. In a star cooler than T eff ~5500K convection prevents the accumulation of heat and pressure. Blue edge of the classical instability strip Red edge of the classical instability strip

17. Various types of pulsating stars in the HR diagram J. Christensen-Dalsgaard

18. The sound waves are generated by a stochastic velocity field in the near-surface convection, where turbulent motions have speeds close to the speed of sound. These waves propagate into the interior and produce the standing waves.

19. The main effect of excitation takes place in a thin subphotospheric layer, where the speeds are close to the sound speed, c s. Solar oscillations are damped oscillations excited stochasticaly by near-surface convection.

20. The Sun as pulsating star 5-minute oscillations of the Sun were discovered in 1962. amplitudes of the brightness variations: ~2  mag amplitudes of the radial velocity variations: ~20 cm/s oscillations periods: 3-25 min lifetimes of modes: of the order of days, weeks number of modes: ~ 10 7

21. HOW STARS PULSATE ?

22. 1-dimensional oscillations FundamentalFirst overtoneSecond overtone nodes D. Kurtz

23. 2-dimensional radial oscillations Fundamental First overtoneSecond overtone

24. 3-dimensional radial pulsations with n = 2

26. dipole =1quadrupole =2 2-dimensional non-radial oscillations

27. 3-dimensional non-radial oscillations 3-dimensional non-radial oscillations = 3 W. Zima

28. = 1, m=0 = 1, m=1 T. Bedding

29. = 2, m=1 = 2, m=2

30. = 3, m=0 = 3, m=1 = 3, m=2 = 3, m=3

31. = 4, m=1 = 4, m=2 = 4, m=4

32. = 5, m=0 = 5, m=2 = 5, m=3

33. = 8, m=1 = 8, m=2 = 8, m=3

34. CAN WE HEAR STELLAR PULSATIONS ? NO !

35. BUT WE CAN OBSERVE BUT WE CAN OBSERVE THE EFFECTS OF PULSATIONS

36. Mira Mira (  Cet ) – the first pulsating star discovered in 1596 by David Fabricius. Visual magnitude: from 3.5 to 9, period equal to 332 days

38. Doppler shift can be used to derive radial velocity

39. Line profile variations

40. Asteroseismology Amplitude Pulsation frequency [c/d]

42. = 2 = 20 = 25 = 75 http://astro.phys.au.dk/helio_outreach

44. SEISMIC MODEL OF THE STAR theoretical frequencies = observed frequencies

45. Which constraints can be obtained from asteroseismology ? MassAge Chemical abundance Efficiency of convection Test of atomic data (opacities) Internal rotation

46. Helioseismology Oscillation frequencies can be used to yield information on the structure and dynamics inside the Sun.

47. Periodogram from the radial velocity measurements on the Sun (BiSON experiment) measurements on the Sun (BiSON experiment)

48. What have we learnt from helioseismology ? Age of the Sun Depth of convection zone Test of opacities, equation of state Helium abundance Internal rotation rate of the Sun

49. Inferred rotation rate of the Sun as a function of radius for indicated heliographic latitudes; from MDI data. J. Christensen-Dalsgaard

50. Rotation of the Sun J. Christensen-Dalsgaard

51. L. Gizon Local helioseismology

52. ASTEROSEISMOLOGY: THE MUSIC OF THE SPHERES

53. The audible range from 20 to 20.000 Hz 1 cycle per second = 1 Hz 5 min 0.003 Hz

54. „SOUNDS” OF PULSATIONS  Centauri  Hydrae The Sun

55. Zoltan Kollath