dust in snr 1e 0102.2−7219
DESCRIPTION
Dust in SNR 1E 0102.2−7219. Karin M. Sandstrom et al. 2009. Dust, a crucial component. for interstellar chemistry regulates thermal balance A Shield for dense clouds. Mid-IR emission from Newly Formed Dust. ∼ 400 and 800 days after the explosion - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/1.jpg)
Dust in SNR 1E 0102.2−7219
Karin M. Sandstromet al. 2009
1
![Page 2: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/2.jpg)
Dust, a crucial component
• for interstellar chemistry• regulates thermal balance• A Shield for dense clouds
2
![Page 3: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/3.jpg)
Mid-IR emission from Newly Formed Dust
• ∼ 400 and 800 days after the explosion– SN 1987A 10^-4 ∼ M sun 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
3
![Page 4: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/4.jpg)
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, 2000APOD, April ,14, 2000 4
![Page 5: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/5.jpg)
Mid-IR spectrum of E 0102
5
![Page 6: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/6.jpg)
cartoon cross-section of E 0102
6
![Page 7: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/7.jpg)
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)
7
![Page 8: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/8.jpg)
NRSE
• “nonradiative shocked ejecta”• outer radius at the contact discontinuity, inner
radius at 4.5 pc∼• Te ~0.4 keV (5×10^6 K)
8
![Page 9: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/9.jpg)
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
9
![Page 10: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/10.jpg)
USE
• ?
10
![Page 11: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/11.jpg)
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.
11
![Page 12: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/12.jpg)
Modeling the Dust Emission
• Unmixed• Model in Nozawa et al. (2003)
amorphous carbon in the He-rich layersMg2SiO4(forsterite) and MgO in the O–Mg–Si layerMgSiO3 and SiO2 in the O–Si–Mg layersilicon 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.
12
![Page 13: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/13.jpg)
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
13
![Page 14: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/14.jpg)
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
14
![Page 15: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/15.jpg)
Dust Model Fit Results
15
![Page 16: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/16.jpg)
(b)from Laor & Draine (1993).
16
![Page 17: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/17.jpg)
Implications for Dust Production in CCSN andComparison with Previous Results
• With Cas A– Mixedunmixed– 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 ∼ ∼ ∼ Msun and 0.6–∼1.4 ×10^-2 Msun of FeO at 60 K.∼
• For E 0102, 3 × 10^-3 Msun am.carbon at 70K, 2 × 10^−5 Msun Mg2SiO4 at 145K
• An ejecta knot in N 132D• CCSN and newly dust formation
17
![Page 18: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/18.jpg)
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
18
![Page 19: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/19.jpg)
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 Msun am.carbon at 70K, 2 × 10^−5 Msun Mg2SiO4 at 145K
19
![Page 20: Dust in SNR 1E 0102.2−7219](https://reader034.vdocument.in/reader034/viewer/2022051403/568148a8550346895db5bb0e/html5/thumbnails/20.jpg)
Thanks
20