1. Tsevi Mazeh: Leuven-Spectrospic binaries 1 The orbital elements

2. Tsevi Mazeh: Leuven-Spectrospic binaries 2 The precession of the periastron

3. Tsevi Mazeh: Leuven-Spectrospic binaries 3 attributed to the following causes: The correction by 42.98" is 3/2 multiple of classical prediction with PPN parameters [6].PPN parameters [6] Sources of the precession of perihelion for Mercury Amount (arcsec/Julian century)Cause 531.63 Gravitational tugs of the other planets 0.0254 Oblateness of the Sun (quadrupole moment)quadrupole moment 42.98 [4][5] [4][5] General relativity 574.64±0.69Total 574.10±0.65 [3] [3] Observed attributed to the following causes: The correction by 42.98" is 3/2 multiple of classical prediction with PPN parameters [6].PPN parameters [6] Precession of the perihelion

4. 4Tsevi Mazeh: Leuven-Spectrospic binaries i to observer

5. Tsevi Mazeh: Leuven-Spectrospic binaries 5 The shape determines e and

6. Tsevi Mazeh: Leuven-Spectrospic binaries 6 Spectroscopic elements: P The orbital period K The RV amplitude The argument of periastron e The eccentricity The periastron passage The RV of the system a,e,,,, Constants of the motion The gravitatonal field

7. Tsevi Mazeh: Leuven-Spectrospic binaries 7 Single-lined spectroscopic binary (SB1)

8. Tsevi Mazeh: Leuven-Spectrospic binaries 8 Single-lined spectroscopic binary (SB1)

9. Tsevi Mazeh: Leuven-Spectrospic binaries 9

10. 10

11. Tsevi Mazeh: Leuven-Spectrospic binaries 11 Double-lined spectroscopic binary (SB2)

12. Tsevi Mazeh: Leuven-Spectrospic binaries 12 The relativistic Doppler effect (Margon et al. 1979)

13. Tsevi Mazeh: Leuven-Spectrospic binaries 13 t V Systematic surveys

14. Tsevi Mazeh: Leuven-Spectrospic binaries 14 t V

15. Tsevi Mazeh: Leuven-Spectrospic binaries 15 Latham, Mazeh et al. 1992

16. Tsevi Mazeh: Leuven-Spectrospic binaries 16 Latham, Mazeh et al. 1992

17. Tsevi Mazeh: Leuven-Spectrospic binaries 17 Short-period binaries Circularization of short-period binaries Mass-ratio distribution Extra-solar planets

18. Spin and orbital angular momentum exchange in binary star systems. Keppens, R. 1997 18Tsevi Mazeh: Leuven-Spectrospic binaries

19. 19 Circularization Synchronization Alignment Observational evidence

20. Tsevi Mazeh: Leuven-Spectrospic binaries 20 938 binaries found in LMC by the OGLE project, analyzed by EBAS (Mazeh, Tamuz & North 2006) Circularization Synchronization Alignment Observational evidence

21. PMS Melo, C. H. F.; Covino, E.; Alcalá, J. M.; Torres, G. 2001, A&A, 378, 898 21Tsevi Mazeh: Leuven-Spectrospic binaries

22. 22Tsevi Mazeh: Leuven-Spectrospic binaries Latham et al. 2002

23. 23Tsevi Mazeh: Leuven-Spectrospic binaries

24. 24Tsevi Mazeh: Leuven-Spectrospic binaries

25. 25Tsevi Mazeh: Leuven-Spectrospic binaries

26. 26Tsevi Mazeh: Leuven-Spectrospic binaries

27. 27Tsevi Mazeh: Leuven-Spectrospic binaries

28. 28 Short-period binaries Circularization of short-period binaries Mass-ratio distribution Extra-solar planets

29. 29 Mazeh et al. 2003 Tsevi Mazeh: Leuven-Spectrospic binaries

30. TODCOR ( and TRICOR ): How to derive radial velocities from composite spectra [ TwO-Dimensional CORrelation] Shay Zucker & Tsevi Mazeh 30Tsevi Mazeh: Leuven-Spectrospic binaries

31. 31 The Cross-Correlation Function Observed spectrum Template spectrum Radial Velocity Cross- Correlation Tsevi Mazeh: Leuven-Spectrospic binaries

32. 32 The Cross-Correlation Function Observed spectrum Template Tsevi Mazeh: Leuven-Spectrospic binaries

33. 33 Single-line Spectroscopic Binary SB1 Double-line Spectroscopic Binary SB2 Observed spectrum Tsevi Mazeh: Leuven-Spectrospic binaries

34. 34 The Cross-Correlation Function Two nicely separated peaks The two peaks are blended Tsevi Mazeh: Leuven-Spectrospic binaries

35. 35 The Cross-Correlation Function Spectral mismatch between secondary and template Faint secondary spectrum Blended peaks Tsevi Mazeh: Leuven-Spectrospic binaries

36. 36 Two-Dimensional CORrelation - Introduction Observed spectrum Primary template Secondary template Relative weight Zucker & Mazeh 1994 Tsevi Mazeh: Leuven-Spectrospic binaries

37. 37 Two-Dimensinal CORrelation - Introduction Tsevi Mazeh: Leuven-Spectrospic binaries

38. 38 Two-Dimensinal CORrelation - Introduction Tsevi Mazeh: Leuven-Spectrospic binaries

39. 39 Two-Dimensinal CORrelation - Introduction Function of two variables Two main ridges “Cuts” along the ridges (“freeze” one Velocity) Estimated pair of velocities Tsevi Mazeh: Leuven-Spectrospic binaries

40. 40 Two-Dimensinal CORrelation - Introduction Freeze the secondary velocity Freeze the primary velocity Tsevi Mazeh: Leuven-Spectrospic binaries

41. 41Tsevi Mazeh: Leuven-Spectrospic binaries

42. 42Tsevi Mazeh: Leuven-Spectrospic binaries

43. 43 SB1 SB2 Measuring mass ratios of SBs: Tsevi Mazeh: Leuven-Spectrospic binaries

44. 44 q=0.29+/-0.04 Mazeh et al. 2003 Tsevi Mazeh: Leuven-Spectrospic binaries

45. 45 The Mass-Ratio Distribution 2-3 measurements are enough ! G62-61 G26-38 Already have primary solution Just need to constrain the secondary solution Tsevi Mazeh: Leuven-Spectrospic binaries

46. 46 Mazeh et al. 2003 Tsevi Mazeh: Leuven-Spectrospic binaries

47. 47 Short-period binaries Circularization of short-period binaries Mass-ratio distribution Extra-solar planets

48. 48 i to observer Radial Velocity Time P K Tsevi Mazeh: Leuven-Spectrospic binaries Test particle (planet) around a star with mass M Reflex motion of star

49. Tsevi Mazeh: Leuven-Spectrospic binaries 49 HD 114762

50. Tsevi Mazeh: Leuven-Spectrospic binaries 50

51. Tsevi Mazeh: Leuven-Spectrospic binaries 51 Grether & Lineweaver 2006 The Brown-Dwarf Desert

52. Extrasolar Planets Aug 201252 Earth Jupiter Neptune RV Going smaller ~20% of the nearby stars have super-earth planets with periods < 50 d

53. 53 HD 41004 A visual pair – K1V/M2V Separation ~ 0.5 arc-sec V-magnitude difference 3.7 Parallax 23 milli-arc-sec Observed regularly in CORALIE Tsevi Mazeh: Leuven-Spectrospic binaries

54. 54 HD 41004 A long-term trend of the residuals Santos et al. 2002 A B Tsevi Mazeh: Leuven-Spectrospic binaries

55. 55 HD 41004 HD41004B HD41004A A long-term trend Short-period modulation disappeared Zucker, Mazeh, Santos, Udry & Mayor 2003 TODMOR – Two Dimension Correlation A B Ba Tsevi Mazeh: Leuven-Spectrospic binaries

56. 56 HD 41004 Follow-up revealed the orbit of a planet around HD41004A Zucker, Mazeh, Santos, Udry & Mayor 2004 Tsevi Mazeh: Leuven-Spectrospic binaries

57. 57 HD 41004 B A Tsevi Mazeh: Leuven-Spectrospic binaries

58. 58Tsevi Mazeh: Leuven-Spectrospic binaries

59. 59 (Not to scale!) A Planet and a Brown Dwarf in the same system Tsevi Mazeh: Leuven-Spectrospic binaries

60. 60 Kepler mission

61. Tsevi Mazeh: Leuven-Spectrospic binaries 61

62. Tsevi Mazeh: Leuven-Spectrospic binaries 62

63. Tsevi Mazeh: Leuven-Spectrospic binaries 63

64. Tsevi Mazeh: Leuven-Spectrospic binaries 64

65. Tsevi Mazeh: Leuven-Spectrospic binaries 65 http://astro4.ast.villanova.edu/aprsa/kepler/detached Kepler binaries

66. Tsevi Mazeh: Leuven-Spectrospic binaries 66

67. Tsevi Mazeh: Leuven-Spectrospic binaries 67

68. Tsevi Mazeh: Leuven-Spectrospic binaries 68

69. Tsevi Mazeh: Leuven-Spectrospic binaries 69

70. Tsevi Mazeh: Leuven-Spectrospic binaries 70

71. Tsevi Mazeh: Leuven-Spectrospic binaries 71

72. Tsevi Mazeh: Leuven-Spectrospic binaries 72

73. Tsevi Mazeh: Leuven-Spectrospic binaries 73 Kepler GO 0025

74. Tsevi Mazeh: Leuven-Spectrospic binaries 74 Kepler GO 0025

75. 75Tsevi Mazeh: Leuven-Spectrospic binaries Test particle around a star with mass M

76. 76 Spectroscopic Binaries Tsevi Mazeh: Leuven-Spectrospic binaries

77. 77 Single-lined spectroscopic binary (SB1)

78. Tsevi Mazeh: Leuven-Spectrospic binaries 78 Double-lined spectroscopic binary (SB2)