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T1 Ejecta

Extending the Results of the Spitzer-Deep Impact Experiment to Other Comets and Exo-Systems C.M. Lisse (JHU-Applied Physics Laboratory). (Typical JFC). T1 Ejecta. (Oort Cloud). 16 um Ejecta Imaging. GMC. ISM. Cometary Dust. ~1 um.

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T1 Ejecta

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  1. Extending the Results of the Spitzer-Deep Impact Experiment to Other Comets and Exo-Systems C.M. Lisse (JHU-Applied Physics Laboratory) (Typical JFC) T1 Ejecta (Oort Cloud) 16 um Ejecta Imaging

  2. GMC ISM Cometary Dust ~1 um Poorly Understood Process of Chemical and Gravitational Aggregation #1, occurring in T ≤ 1 Myr Proto-Solar Nebula 30 um • Ices - C, H, O, N • Dust - Mg, Si, Fe, S • Ca, O, Al, C, … P.U.P.C.G.A. #2, occurring in T ≤ 10 Myr Deep Impact ~5 km T<400K, P < 1kPa De-aggregation and Ejection of Sub-surface Fresh(?) PSN Material Icy Dirtball Comet Nucleus

  3. Parameters Derivable From the DI Experiment Bulk, Average Composition of Ejected Dust Obtained from features at set wavelengths Allows search for comparable species in other systems Temperature of Dust Components at 1.5 AU Obtained from short/long wavelength amplitude, feature No modeling required Yields location of dust in exo-systems from observed T’s Particle Size Distribution of Ejected Dust Obtained from feature/continuum ratio Unusual narrowly peaked distribution 0.1 - 10 um

  4. Spitzer IRS I+45 Min 344 Spectral Points SNR 5 - 30 (2 error bars) 95% C.L. = 1.13 Simultaneous 5- 35 um > 16 Sharp Features Best-Fit Linear Sum  (95% C.L. = 1.13) Carbonates (Chalk) (Pre-Post)/Pre = Ejecta/Pre-Impact Coma PAHs (Soot, Exhaust) Water Gas Amorphous Carbon (Soot) Water Ice Sulfides (Fool’s Gold) Phyllosilicates (Clay) Pyroxenes (Rock) Olivines (Rock) Lisse et al. 2006

  5. Fire, Mud, & Ice : Tempel 1 Contains Xtal Silicates, Annealed at T > 1000K + Carbonates & Clays- Formed via Interaction with Water + Ices - Stable Only Below 200 K Radial Mixing of PSN Material.From inside the orbit of Mercury to outside the orbit of Neptune (turn-off when giant planet cores form) Crystal Silicates Carbonates Clays Comets Parent Body Aqueous Alteration Over 4.5 Gyr (1) Impulsive Cratering (2) Long Term Water Vapor Processing

  6. SST-IRS P/Tempel 1 Ejecta Difference Spectrum vs. ISO-SWS C/Hale-Bopp, YSO HD100546 Silicates YSO with Rich Dusty Disk Input PAHs • Formed in Giant Planet Region • Resides in Outer Solar System Today Output Sulfides Carbonates • Formed in Kuiper Belt • Resides in Inner Solar System Sun

  7. SST-IRS P/Tempel 1 Ejecta Spectrum Compared to Comets, Exo-Systems. - -Similar Spectra Due to Presence of Silicates, PAHs, Water, Sulfides. - Differences Due to Relative Compositions, T, Particle Size Disk Systems HD100546, HD69830, HD113766 Comets Hale-Bopp, SW3, SW1 10 Myr Be9V YSO w/ Disk Cavity ~15 Myr F3/F5 YSO 2-10 Gyr K0V w/ 3 Neptunes

  8. 1.47 AU 1.5 AU JFC Tempel 1 Ejecta (SST; Lisse et al. 2006) JFC SW-3 B Fragment (SST; Sitko et al. 2007) Amorph Carbon PAHs Carbonates Sulfides Pyroxenes Olivines 2.8 AU 5.7 AU JFC/Centaur SW-1 Coma (SST; Stansberry et al. 2005) Oort Cloud Hale-Bopp Coma (ISO; Crovisier et al. 1997)) Carbonates Water Ice Smectite (clay) Pyroxenes Olivines Olivines Lisse et al. 2007 “Spectral Fingerprints” of Cometary IR Mineralogy T1 Spectral Model applied to other systems fits spectra well, extends results to Spitzer, ISO database. We can now dig down below the dominant silicate emissions to find other species. Hale-Bopp: No Fe-rich olivine. Much more water ice and amorphous carbon. Carbonates, clay. SW1, SW3 : Much amorphous silicates, Mg-rich olivine. Only water gas for SW3, ice for SW1.

  9. Abundance of Cometary Water Ice vs. Gas Follows Water Ice Stability in Solar System (water ice stable) (rapidly ejected Interior material) (water ice rapidly sublimating)

  10. Relative amount of crystalline pyroxene increases from SW1, SW3 to Tempel 1. Tempel 1 appears most ”processed”. Hale-Bopp probably formed early, but why SW3 so “fresh”? Deep interior material, or bodies formed in PSN at different times 1- 10(?) Myr and places (4 - 50 AU)? Silicate Trends?(work in progress) asteroidal cometary Pyroxene content is high for comets and HD100546, low for asteroidal debris disks

  11. K0V, 12 pc • K0V, T = 5400 K, 2 - 10 Gyr old, 12 pc distant • 3 Neptune Sized Planets @ 0.08, 0.16, 0.63 AU Lovis et al. 2006 “Mature” HD69830 B C D Asteroidal Dust Belt Lisse et al. 2007 T~ 400 K Super Comet or Asteroid? Carbonates PAHs absent Carbon attenuated Water Ice Sulfides absent Pyrox all crystalline Olivine Super-rich Lisse et al. 2007 Beichman et al. 2005 “Near-solar” star. Small, icy, ephemeral dust replenished by ongoing fragmentation. S.S. analogue : ~30 km radius P/D asteroid disrupted @ 1 AU. Karins/Veritas 5-8 Mya?

  12. Comparative IR Mineralogy of Young Stellar Objects HD100546 : Comet-like. Especially rich in Mg-rich olivine and amorphous pyroxene, water ice. We find the dust to be at ~13 AU, consistent with the inner disk cavity edge of Grady et al. 2005. HD113766: Mainly has Mg-rich olivine, Fe-rich sulfides, and xtal pyroxene. Little carbonates, clays, PAHs, or amorphous carbon present. Similar to S-type asteroid. NOT an older HD100546. Amorph Carbon HD100546 Disk Herbig Be9V >10 Myr X PAHs HD113766 Disk F3/F5 ~16 Myr Carbonates Water Ice Sulfides Clays Sulfides Pyroxenes Pyroxenes Olivines Olivines Lisse et al. 2007

  13. Comets r(AU) Water Ice/Gas Silicates Carbonates Clays PAHs Sulfides Tempel 1 1.51 Ice & O:P = 1 Magnesite & Yes Yes Yes JFC Gas fxtalo = 0.7 Siderite (SST, 5-35um) (Impact) fxtalp = 0.9 SW3 1.47 Abundant O:P = 1.6 Some No Yes Yes JFC Water Gas fxtalo = 0.3 Siderite (SST, 5-35um) (Near-Sun) fxtalp = 0.6 HaleBopp 2.8 Abundant O:P = 1.3 Abundant Yes Yes Yes Oort Cloud Water Ice fxtalo = 0.7 Magnesite & (ISO, 5-40um) (Beyond Ice fxtalp = 0.7 Siderite Line) SW1 5.8 Abundant O:P ~ 3.2 Some No Yes? Some Centaur/JFC Ice (BYI) fxtalo = 0.3 Siderite (SST, 7-35um) fxtalp = 0.5 Exo-systems r(AU) Water Ice/Gas Silicates Carbonates Clays PAHs Sulfides HD100546 ~13 AU Abundant O:P = 0.8 Magnesite Yes YES Yes Be9V, ≥ 10 My (103pc) Ice & Water fxtalo = 1.0 (ISO, 5-40um) fxtalp = 0.3 HD113766 ~1.8 AU Some O:P = 2.4 None ~None No Yes F3/F5, ~16 My (131pc) Ice fxtalo = 0.7 (SST, 5-35um) fxtalp = 1.0 HD69830 ~1 AU Some O:P = 2.8 ??? None No? No K0V, 2 - 10 Gy (12pc) Ice fxtal = 0.8 (SST, 7-35um) fxtalp = 0.8

  14. Conclusions • We have obtained good fits to the 5- 35 um mid-IR spectra of comets HaleBopp, SW3, and SW1 using the Deep-Impact -T1 ejecta model. • Silicates, PAHs, water, and sulfides are found in abundance in all studied systems. • We find the water content of the comets is gaseous inside the ice line, solid outside it, following the solid ice stability in the solar system. • The relative amount of pyroxene decreases as the systems become processed into asteroidal material. In the comets, crystal pyroxene may increase with time of formation. • We find emission from HD69830 (K0V, 2-10 Gy, ~0.5 Lsolar) dominated by highly processed dust from disruption of a ~ 30 km P or D-type body. • We find emission from HD100546 (Be9V, > 10 My, 22-26 Lsolar) dominated by primitive nebular material at ~13 AU, at the disk inner cavity wall of Grady et al. • We find emission from HD113766 (F3/F5, ~15 My, 4.4 Lsolar) dominated by processed dust from disruption of an ~S-type, terrestrial planet forming?) body at 2.2 AU. => Disks can be either primordial nebulae (cometary?) or due to stochastic collisions of coherent small bodies (asteroidal?).

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