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Study of Planet forming Systems Orbiting Intermediate-mass Stars

Study of Planet forming Systems Orbiting Intermediate-mass Stars. Sweta Shah Ithaca College Advisor: Dr. Luke Keller In collaboration with the NASA Spitzer Space Telescope I nfra R ed S pectrograph Disk’s Team. Image credit: Caltech. Theory of Planet formation Adapted from Hogerheide 1998.

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Study of Planet forming Systems Orbiting Intermediate-mass Stars

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  1. Study of Planet forming Systems Orbiting Intermediate-mass Stars Sweta ShahIthaca College Advisor: Dr. Luke Keller In collaboration with the NASA Spitzer Space Telescope InfraRed Spectrograph Disk’s Team Image credit: Caltech

  2. Theory of Planet formation Adapted from Hogerheide 1998

  3. Why intermediate mass (Herbig Ae Be) stars ? • Hot and massive 12,000 - 18,000 K • 2-10 solar mass • Excess thermal (IR) radiation • ‘e’ Emission line spectra Circumstellar disks in Orion Nebula (Hubble Space Telescope Image: McCaughrean & O’Dell 1995)

  4. Spectral characteristics of the Accretion Disk • Thermal IR excess • PAH • Dust -silicates UV mm Spectral Energy Distribution (Malfait et al. 1998)

  5. Correlation of SED and disk geometry(Malfait et al. 1998)

  6. IRS SL IRS SL IRS SL IRS SL Physical structure of the disks: SEDs (UV-mm) LL LL LL LL (Malfait et al. 1998)

  7. H H H H H H H H H H H H Spectral features - PAH? • Polycyclic Aromatic Hydrocarbon • Excited by UV radiation Sloan, Keller, Leibensperger et al. 2005 very stable

  8. What is the shape of the disk? How do we test this hypothesis?

  9. Measuring the strength of “bumps” in Infrared continuum 13 6 25

  10. Dust grain growth and settling Flared disks Increasing 13-25 m SED slope Flat disks Star with no disk Increasing 6-13 m SED slope Keller, Shah et al. 2006, paper in preparation

  11. Ultimate Goal ?! IPAH Disk evolution in time

  12. Thanks!(Any ?)

  13. SpitzerInfraRedTelescopeFacility • Background-limited sensitivity 3 – 180 m • 85 cm f/12 beryllium R-C telescope, T < 5.5K • Three scientific instruments provide: • Imaging/photometry, 3-180 m • Spectroscopy, 5-40 m (R = 90 & 600) • Spectrophotometry, 50-100 m • 5.5 yr lifetime • Launched on 25 August 2003 • Birth stone: forsterite IRS

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