2. The wind speeds, dust content, and mass-loss rates of evolved stars at varying metallicity.
Steve Goldman
8 August, 2016
ICISE

13. Regeneration of the universe

14. New maser observations
Spectral energy distribution fitting
Deriving mass loss rates and gas-to-dust ratios
New mass loss prescription
Fundamental parameters

15. 64 m

16. six 22 m dishes
longest baselines: 6 km

17. Wood et al. (1992)
Marshall et al. (2004)

18. Wood et al. (1992)
Marshall et al. (2004)

19. *
Wood et al. (1992)
Marshall et al. (2004)

20. Past work Galactic: >2000 LMC: 8 SMC: 0 GCs: 0
Marshall et al. (2004)

21. Past work Galactic: >2000 LMC: 8 5 SMC: 0 GCs: 0
Marshall et al. (2004)

22. Awarded 92 hours
Four new OH masers
Doubled the number of reliable Vexp

25. 0 masers

26. Our work νexp ∝ ψ1/2 L1/4 νexp = 0.13 Z L0.4 Galactic: >2000
LMC: 13
SMC: 0
GCs: 0
νexp = 0.13 Z L0.4
Goldman et al. (submitted)

27. Spectral Energy Distribution (SED) Fitting

28. Goldman et al. (submitted)

29. Photometry from: 2MASS, DENIS, MSX, AKARI, IRAS, Spitzer
Spitzer phot and Spitzer (IRS) spectra
Best fit DUSTY spectra: dotted line
Blue within 95% confidence
Goldman et al. (submitted)

30. Photometry from: 2MASS, DENIS, MSX, AKARI, IRAS, Spitzer
Spitzer phot and Spitzer (IRS) spectra
Best fit DUSTY spectra: dotted line
Blue within 95% confidence
Luminosity
Expected expansion velocity
Mass loss rate
Goldman et al. (submitted)

31. Photometry from: 2MASS, DENIS, MSX, AKARI, IRAS, Spitzer
Spitzer phot and Spitzer (IRS) spectra
Best fit DUSTY spectra: dotted line
Blue within 95% confidence
Luminosity
Expected expansion velocity
Mass loss rate
OH Expected gas-to-dust
Goldman et al. (submitted)

32. Photometry from: 2MASS, DENIS, MSX, AKARI, IRAS, Spitzer
Spitzer phot and Spitzer (IRS) spectra
Best fit DUSTY spectra: dotted line
Blue within 95% confidence
Luminosity
Expected expansion velocity
Mass loss rate
OH Expected gas-to-dust
νexp ∝ ψ1/2 L1/4
Goldman et al. (submitted)

33. Goldman et al. (submitted)

34. Goldman et al. (submitted)

35. Goldman et al. (submitted)

36. Goldman et al. (submitted)

37. νexp = 0.13 Z L0.4
Goldman et al. (submitted)

38. Goldman et al. (submitted)

39. Goldman et al. (submitted)

40. Goldman et al. (submitted)

41. Mass loss Reimers 1975 Schroder & Cuntz 2005 van Loon 2005
Baud & Habing 1983
Zijlstra et al. 1996

42. Goldman et al. (submitted)

43. van Loon et al. (2000)

44. Conclusions Discovered 4 new circumstellar OH masers
Increased the number of reliable wind speeds from 5  13
Developed a method of deriving gas-to-dust ratios (needs testing)
Continue to see a strong dependence on both metallicity and luminosity of expansion velocity
See a strong correlation between luminosity and mass loss
Gas-to-dust ratio has shown to have little effect on the mass loss of AGB and RSGs
This suggests that mass loss is (nearly) independent of metallicity between a half and twice solar

50. νexp ∝ ψ1/2 L1/4

51. S. Höfner