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Binaries

Binaries. Visual Binaries. Spectroscopic Binaries. Eclipsing Binaries. Double stars. Rev. John Mitchell - 1767 “it is highly probable in particular, and next to a certainty in general, that such double stars as appear to consist of two or more stars placed very near together, do really

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Binaries

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  1. Binaries Tsevi Mazeh: Leuven-Binaries

  2. Visual Binaries Spectroscopic Binaries Eclipsing Binaries Tsevi Mazeh: Leuven-Binaries

  3. Double stars Rev. John Mitchell - 1767 “it is highly probable in particular, and next to a certainty in general, that such double stars as appear to consist of two or more stars placed very near together, do really consist of stars placed near together, and under the influence of some general law.” The definitive existence of binary stars was demonstrated by William Herschel in 1802. Tsevi Mazeh: Leuven-Binaries

  4. Binary stars Visual spectroscopic astrometric eclipsing A multitude of types Unresolved by telescope, but two sets of spectral lines seen Resolved by telescope into two stars Oscillatory motion on the sky Stars periodically pass in front of each other in our LOS Tsevi Mazeh: Leuven-Binaries

  5. Example of Visual Binaries Krueger 60 : d = 4 pc M3.5V + M 4V, Period = 44.5 years Tsevi Mazeh: Leuven-Binaries

  6. Example of Visual Binaries Tsevi Mazeh: Leuven-Binaries

  7. Visual Binaries a d Tsevi Mazeh: Leuven-Binaries

  8. Kepler’s 3rd law: Tsevi Mazeh: Leuven-Binaries

  9. Ursa Major, The Big Bear (Big Dipper) • Mizarwas the first known binary, noticed in 1650 by Riccioli. Tsevi Mazeh: Leuven-Binaries

  10. Mizar: A binary within a binary Tsevi Mazeh: Leuven-Binaries

  11. Resolution of a telescope Tsevi Mazeh: Leuven-Binaries

  12. Binary system Mizar A Observed by NPOI Navy Prototype Optical Interferometer (NPOI) Array south of Flagstaff AZ, The Mizar images were obtained with the inner three 0.5m telescopes. A total of 10 telescopes will be operational starting in 2003. 0.01 arcsec Mizar A binary (period 20 days). Tsevi Mazeh: Leuven-Binaries

  13. Tsevi Mazeh: Leuven-Binaries

  14. Example: Wavelength λ=500nm, baseline B=100m Θ ~ 0.001“ = 1 mas • CHARA– Center for High Angular Resolution Astronomy at Georgia State University • SUSI– Sydney University Stellar Interferometer • NPOI - Navy Prototype Optical Interferometer • Mark III Interferometer • PTI - Palomar Testbed Interferometer Tsevi Mazeh: Leuven-Binaries

  15. Tsevi Mazeh: Leuven-Binaries

  16. Tsevi Mazeh: Leuven-Binaries

  17. Tsevi Mazeh: Leuven-Binaries

  18. Examples of Optical Interferometers Keck Interferometer (2x10m) Mauna Kea, Hawaii VLT Interferometer (4x8m) Chile (ESA) Tsevi Mazeh: Leuven-Binaries

  19. a1 a2 M2 M1 The binary motion CM Tsevi Mazeh: Leuven-Binaries

  20. Tsevi Mazeh: Leuven-Binaries

  21. Tsevi Mazeh: Leuven-Binaries

  22. Tsevi Mazeh: Leuven-Binaries

  23. Planet Tsevi Mazeh: Leuven-Binaries

  24. Kepler first law: Tsevi Mazeh: Leuven-Binaries

  25. Kepler second law: Tsevi Mazeh: Leuven-Binaries

  26. Origin of orbits of both stars Empty Periastron point Tsevi Mazeh: Leuven-Binaries

  27. The Masses of Sirius A & B • 5th closest star to us: d = 2.63pc • Sirius A is the brightest star in the sky Tsevi Mazeh: Leuven-Binaries

  28. Wobble of Sirius Tsevi Mazeh: Leuven-Binaries

  29. Sirius AB Binary System HST image Tsevi Mazeh: Leuven-Binaries

  30. Orbits of Sirius A and B Tsevi Mazeh: Leuven-Binaries

  31. Sirius AB Binary System Tsevi Mazeh: Leuven-Binaries

  32. Sirius AB Binary System • Ratio of motion: Distance estimate: a = 7.62” 20.04 AU at a distance of 2.63 pc Kepler’s 3rd law: M1 + M2 = (20.04)3/(49.9)2 = 3.23 Tsevi Mazeh: Leuven-Binaries

  33. Sirius AB Binary System • Hence M1 / M2 = 2.3 and M1 + M2 = 3.23 • so, unraveling the masses gives M1 = mass of Sirius A = 2.25 M M2 = mass of Sirius B = 0.98 M Tsevi Mazeh: Leuven-Binaries

  34. Sirius AB Binary System 1862- Clark resolved the two stars 1915-Adams obtained a spectrum of Sirius B T~25,000 K Tsevi Mazeh: Leuven-Binaries

  35. The H-R Diagram L = 4  R2  T4 Tsevi Mazeh: Leuven-Binaries

  36. The Sizes of Stars Tsevi Mazeh: Leuven-Binaries

  37. Gliese 229B 8’’ separation 10 mag difference in J,H,K (Nakajima 1995) Tsevi Mazeh: Leuven-Binaries

  38. Binary stars Visual spectroscopic astrometric eclipsing A multitude of types Unresolved by telescope, but two sets of spectral lines seen Resolved by telescope into two stars Oscillatory motion on the sky Stars periodically pass in front of each other in our LOS Tsevi Mazeh: Leuven-Binaries

  39. Visual Binaries Spectroscopic Binaries Eclipsing Binaries Tsevi Mazeh: Leuven-Binaries

  40. One star with a spectrum composed of two spectra Tsevi Mazeh: Leuven-Binaries

  41. The Doppler Effect Spectrum of Hydrogen in Lab Spectrum of a Star Tsevi Mazeh: Leuven-Binaries

  42. Spectroscopic binary Spectrum of Hydrogen in Lab Spectrum a Star…..Day 1 Spectrum a Star…..Day 2 Spectrum a Star…..Day 3 Spectrum a Star…..Day 4 Tsevi Mazeh: Leuven-Binaries

  43. To earth Tsevi Mazeh: Leuven-Binaries

  44. Spectroscopic Binaries If the Doppler shift of a star’s absorption lines changes with time (redshift, then blueshift, then redshift, etc.), it’s a spectroscopic binary. Tsevi Mazeh: Leuven-Binaries

  45. Spectroscopic Binaries Double-lined spectroscopic binary. Tsevi Mazeh: Leuven-Binaries

  46. Spectroscopic Binaries Tsevi Mazeh: Leuven-Binaries

  47. Single-lined spectroscopic binary (SB1) Tsevi Mazeh: Leuven-Binaries

  48. Single-lined spectroscopic binary (SB1) Tsevi Mazeh: Leuven-Binaries

  49. Visual Binaries Spectroscopic Binaries Eclipsing Binaries Tsevi Mazeh: Leuven-Binaries

  50. Eclipsing Binaries Animation Tsevi Mazeh: Leuven-Binaries

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