Dust in SNR 1E 0102.2−7219

1. Dust in SNR 1E 0102.2−7219 Karin M. Sandstrom et al. 2009

2. Dust, a crucial component • for interstellar chemistry • regulates thermal balance • A Shield for dense clouds

3. Mid-IR emission from Newly Formed Dust • ∼ 400 and 800 days after the explosion • SN 1987A ∼ 10^-4 Msun of dust produced by 775 days after the explosion • SN 1990I (Elmhamdi et al. 2004) • SN 2006jc (Smith et al. 2008; Nozawa et al. 2008) • (other source: IR light echoes) • Reverse shock reheats the newly formed dust

4. Introduction to 1E 0102.27219 • Young(adopt a value 2000yr) • 190,000 ly • R.A. 01h04m02.s1 decl. −72◦0152.5(J2000) • oxygen-rich • Type Ib/Ic or IIL/b SN (Blair et al. 2000; Chevalier 2005) • Blast wave radius ∼ 22’’ • Reverse shock radius ∼ 15’’ T. J. Gaetz, 2000 APOD, April ,14, 2000

5. Mid-IR spectrum of E 0102

6. cartoon cross-section of E 0102

7. SCSM • “forward-shocked CSM/ISM” • outer radius at∼ 6.6 pc, inner radius at the contact discontinuity • Radio & outer part of X-ray • Te ~ 1keV (10^7 K)

8. NRSE • “nonradiative shocked ejecta” • outer radius at the contact discontinuity, inner radius at ∼ 4.5 pc • Te ~0.4 keV (5×10^6 K)

9. RSE • “radiative shocked ejecta” • reverse shock encounters dense clumps of ejecta • the brightest optical emission lines from these shocks is the [O iii] line at 5007 Å

10. USE • ?

11. Results of the decomposition • All of the line emission is found to come from the radiative shocked ejecta (RSE) • NRSE shows dust continuum but no emission lines • SCSM spectrum also has a small dust emission component that peaks around 20 μm.

12. Modeling the Dust Emission • Unmixed • Model in Nozawa et al. (2003) amorphous carbon in the He-rich layers Mg2SiO4(forsterite) and MgO in the O–Mg–Si layer MgSiO3 and SiO2 in the O–Si–Mg layer silicon and iron rich species in the deeper nucleosynthetic layers • how deeply into the ejecta the reverse shock has propagated • what species of dust we should include.

13. Dust model in E 0102 • magnesium is ∼ 2 times more abundant than silicon (Flanagan et al. 2004). • the primary species : • amorphous carbon • Al2O3 • forsterite • MgO

14. Dust Model Fit Results • involves the four grain species discussed above with a fixed size of 0.1 μm. (For dust grains in the Rayleigh limit the dust mass is independent of the grain size)? • Parameter: the mass of dust in each species and its temperature

15. Dust Model Fit Results

16. (b)from Laor & Draine (1993).

17. Implications for Dust Production in CCSN andComparison with Previous Results • With Cas A • Mixedunmixed • Species S, Ar, Ca, Fe O, Ne, Mg • Mass and temperatureof dust • For Cas A , Rho et al. (2008) find on the order of 0.02−0.05 Msun of dust. two temperature components of Am.carbon at ∼ 80 and ∼ 200 K totaling ∼ 1–2 × 10^-3 Msunand ∼ 0.6–1.4 ×10^-2 Msun of FeO at ∼ 60 K. • For E 0102, 3 × 10^-3 Msunam.carbon at 70K, 2 × 10^−5 Msun Mg2SiO4 at 145K • An ejecta knot in N 132D •  CCSN and newly dust formation

18. Problem • find substantially less amorphous carbon dust than predicted by dust condensation models.(outermost layers of the ejecta) • have no constraints on the initial grain size, so it is difficult to estimate how much of the dust in the remnant has been destroyed up to this point • The contribution to the IR continuum from MC or other kind of dust • The mid-IR observations are not sensitive to cold dust present in the remnant

19. SUMMARY AND CONCLUSIONS • Fine-structure emission lines of oxygen and neon on top of emission from warm dust. • Decomposition of the spectrum. Emission and continuum… • Best fit model：3 × 10^-3 Msunam.carbon at 70K, 2 × 10^−5 Msun Mg2SiO4 at 145K

20. Thanks