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Benjamin Sargent

GRAMS Modeling of Oxygen-Rich Dust around Red Supergiant and AGB Stars in the Large Magellanic Cloud. Benjamin Sargent Collaborators: Sundar Srinivasan , Dave Riebel , Martha Boyer, Margaret Meixner March 28, 2012 Space Telescope Science Institute. Image: Gordon & SAGE team

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Benjamin Sargent

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  1. GRAMS Modeling of Oxygen-Rich Dust around Red Supergiant and AGB Stars in the Large Magellanic Cloud Benjamin Sargent Collaborators: SundarSrinivasan, Dave Riebel, Martha Boyer, Margaret Meixner March 28, 2012 Space Telescope Science Institute Image: Gordon & SAGE team (Meixner et al. 2006)

  2. Lifecycle of Matter: How much mass is lost from stars? AGB Stars: O-rich and C-rich dust produced RSG Stars: O-rich only

  3. Modeling Evolved Stars • Assume a spherical cow … • R-2 density drop-off from assumption of constant mass loss • Drawing not to scale! • Rout = 1000*Rmin assumption

  4. GRAMS: Grid of Red supergiant and AGB ModelS • GRAMS computed using 2Dust (Ueta & Meixner2003) radiative transfer modeling code • http://www.stsci.edu/science/2dust/grams_models.cgi • GRAMS  returns Mass Loss Rate, Luminosity, and Dust Chemistry

  5. Color-Color Diagram • O-rich models • C-rich models • O-rich AGBs • C-rich AGBs • Extreme AGBs • RSGs • O-rich (spec) • C-rich (spec) From Sargent et al 2011 X-axis (K-[3.6]) is stellar color, Y-axis ([3.6]-[24]) is overall IR color

  6. Comparison to Other Work • Generally, good agreement, except GRAMS MLRs disagree with G09 for low MLRs • GRAMS uses one dust type for all models; G09 used many dust types, but no dependence upon MLR, so dust type not behind factor x6 MLR discrepancy

  7. O-rich AGB Dust Properties • SEDs: U, B, V, I from MCPS (Zaritsky et al 1997); J, H, Ks from 2MASS (Skrutskie et al 2006), IRAC and MIPS-24 from SAGE • Right, SED of oxygen-rich (O-rich) AGB star; 2Dust (Ueta & Meixner 2003) model of O-rich AGB (Sargent et al 2010) • But …

  8. One Dust Type Doesn’t Fit All

  9. Isolating Dust Emission • SED is fit by GRAMS, star is subtracted • Measure centroid of features, continuum slope

  10. Spitzer-IRS Spectroscopic Studies of AGBs and RSGs • Average AGB 10μm feature centroid displaced to shorter λ‘s than RSGs’ (Sargent et al, in prep) • Similar discrepancy seen between Miras and non-Miras by Marengo et al (2001)

  11. RSG vs AGB Silicates • Star-subtracted continuum slope relatively independent of 10 μm silicate feature centroid

  12. RSG vs AGB Silicates, con’t • RSG shells have hotter dust, but if continuum slope were affecting centroid, hotter dust would mean shorter-wavelength centroids

  13. Conclusions • NASA ADAP grant NNX11AB06G • GRAMS model grid useful for determining mass loss from AGB and RSG stars • Difference between AGB and RSG average 10 μm feature centroid. Different avg dust optical properties? • Silicate feature peak wavelength difference not due to temperature effect on continuum • Thank you!

  14. Asplund, M., et al., 2004, A&A, 417, 751 Bekki, K., & Chiba, M., 2005, MNRAS, 356, 680 Dufour, R. J., et al., 1982, ApJ, 252, 461 Gautschy-Loidl, R., et al., 2004, A&A, 422, 289 Houck, J. R., et al., 2004, ApJS, 154, 18 Kučinskas, A., et al, 2005, A&A, 442, 281 Kučinskas, A., et al, 2006, A&A, 452, 1021 Marengo, M., et al., 2001, MNRAS, 324, 1117 Meixner, M., et al., 2006, AJ, 132, 2268 Ossenkopf, V., et al., 1992, A&A, 261, 567 Pégourié, B., 1988, A&A, 194, 335 Pei et al., 1999, ApJ, 522, 604 Sargent, B. A., et al., 2010, ApJ, 716, 878 Sargent, B. A., et al., 2011, ApJ, 728, 93 Schaefer, B. E., 2008, AJ, 135, 112 Skrutskie, M., et al, 2006, AJ, 131, 1163 Srinivasan, S., et al., 2009, AJ, 137, 4810 Srinivasan, S., et al., 2010, A&A, 524, A49 Srinivasan, S., et al., 2011, A&A, 532, A54 Szewczyk, O., et al., 2009, AJ, 138, 1661 Ueta, T., & Meixner, M., 2003, ApJ, 586, 1338 Zaritsky, D., Harris, J., & Thompson, I., 1997, AJ, 114, 1002 Zubko, V. G., et al., 1996, MNRAS, 282, 1321 References

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