1. Dust Models for the Extinction of Type IIn SN 2010jl Jian Gao, Jun Li, B. W. Jiang Beijing Normal University , 昆明

2. Why Type IIn SN Dust 很重要！ 起源：SNe, AGBs SNe
Large amount of dust in very young universe
Dust mass formed in a SN < 10-2 to 10-3 M⊙, much smaller than predicted.
超新星到底能产生多少尘埃？
affects the physical and chemical conditions in ISM, star formation etc.
Figure 4 | Temporal evolution of the dust mass. Carbon dust masses and
standard deviation derived from the extinction (green band) and the NIR
emission (red bars and band; see Methods) including a literature data point at
553 days (ref. 12) The light-grey shaded area illustrates the evolution of the early
(Md / t0.8 at t,250 days) and late (Md / t2.4 at t.250 days) stages of dust
formationwhen SN2010jl switches fromcircumstellar to ejecta dust formation.
The grey and blue symbols correspond to literature data for SN2005ip
(triangles), SN 2006jd (dots), and other supernovae (bars)1,5,6,9,10,27,30. The length
of the symbols for SN 1995N and SN1987A correspond to the quoted dust
mass range. For other supernovae the standard deviation is either smaller than
the size of the symbols or has not been reported.
Gall et al Nature

3. Why SN 2010jl Target：Type IIn SN 2010jl
Cool dense shell
Dust formed: IR excess
Host in UGC5189A, 49Mpc
Extinction: Gall et al Nature
Derived from the attenuation of emission lines
Gray+MW/SMC extinction
Larger Rv:
Larger dust grain size: a ~ 1.3 mm
Target: SN 2010jl
ü Type IIn, named after narrow H spectral lines.
ü Cool dense shell
ü Significant infrared excess
ü Host in UGC 5189A, 49Mpc
Gall et al Nature
Gall Nature

4. The Dust around SN 2010jl Al increase, new dust formed
Larger grain size a ≈ 1.3 mm
MRN
Larger Rv = 6.4
We fitted
several dust models to the extinction curve using amorphous carbon
dust characterized by a power-law grain size distribution20 with slope
a, and minimumandmaximumgrain radii (amin,amax) in the interval
[0.001, 5.0] mm
Gall+ 2014
Gall et al Nature

5. The Dust around SN 2010jl Al increase, new dust formed
NIR excess dust emission
Larger Rv = 6.4
Gall+ 2014
Gall et al Nature

6. More stricts dust model + MIR emission
The Dust around SN 2010jl
Dust Mass:
M⊙ (MIR emission) v.s to 10-4 M⊙ (Gall+ 2014)
Gall+ 2014的缺陷:
尘埃成分单一： amorphous carbon or silicate
消光曲线拟合不好
没有结合MIR emission，质量估计方法简单：
Some interpret as evidence of newly formed dust (Smith et al. 2012; Maeda et
al. 2013; Gall et al. 2014), while others suggest a pre-existing and unshocked CSM dust (Andrews et
al. 2011; Fox et al. 2013; Fransson et al. 2014). Using a standard Mathis-Rumpl-Nordsieck (hereafter
MRN) grain size distribution of a􀀀3:5 between and 0.05 m (Mathis et al. 1977), Andrews et al.
(2011) estimated a dust mass between 0.03 and 0.35 M by tting the photometric data of Spitzer
at 3.6 m and 4.5 m and of WIYN in the JHK bands on day 90. Maeda et al. (2013) derived a dust
mass of (7:5 􀀀 8:5) 10􀀀4M from an optical to near-infrared (NIR) spectrum around 1.5 years
after the explosion. They also inferred that carbon grains are the main dust component and the
typical grain size is 0:1 m, and even likely 0:01 m. Because of the non-detection at 11.1 m
by SOFIA on 2014 May 5-6, Williams & Fox (2015) ruled out the presence of silicate dust around
SN2010jl. They also estimated an upper limit of M carbonaceous dust with a single grain
size of 0.1 m, with the photometric data at Spizter 3.6 m, 4.5 m, and the upper limit at SOFIA
11.1 m.
More stricts dust model + MIR emission

7. Dust Models of Dust around SN 2010jl
Rv = 2.1
尘埃模型 成分
Silicate+Graphite
Silicate+Amorphous Carbon
尺寸分布：
Rv = 7.0

8. Dust Models of Dust around SN 2010jl
MRN
KMH

9. Prior Mass Ratio: MSilicate/MGraphite
Williams & Fox 2015
No evidence for strong
9.7 μm feature
a ≈ 1.3 mm, 20% sil.
No evidence for the strong
9.7 µm feature
MC Simulation
15%, 50%, 85%
0.07, ,
Williams & Fox 2015
 Silicate
20%, 40%

10. The Best Dust Model
40% sil. + 60% gra.
MSilicate/Mgraphite = 0.4:0.6

11. Best-fitted Results MSilicate/Mgraphite = 0.4:0.6
Nielsen+(2018) found Rv of SN 2005ip increase with time, from

13. Dust Mass from MIR Emission
49 Mpc
mid-infrared photometry of SN 2010jl
D is the luminosity distance to the observers (49 Mpc).

14. Discussion: Dust mass from extinction
Zhao et al. (2018)
WD01
effective surface area
rCDS ~ 1016cm (Gall+2014, Sarangi+2018)
 Mdust ~ 10-4 M⊙ < ~ 10-2 M⊙
Too small?

15. Summary for Dust around SN 2010jl
Size Distribution:
Small Silicate Dust + Large Carbonaceous Dust
MSilicate/Mgraphite = 0.4:0.6
Rv~3.0 < 6.4 (Gall+,2014)
Mdust~ 0.05M⊙ at 1741 day

16. Thanks!