OGLE-2002-BLG-360: A dusty anomaly among red nova remnants

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Table 2

Input parameters for RADMC-3D models.

Model	R_⋆ (R_⊙)	T_eff (K)	Silicate type^a	Sil:Al₂O₃:mFe:amC	r_in (AU)	r_out (AU)	$r_{i n}^{c a v}$ $\[\mathrm{r}_{i n}^{c a v}\]$ (AU)	$r_{o u t}^{c a v}$ $\[\mathrm{r}_{out}^{cav}\]$ (AU)	r_bound (AU)	f_ρ
cd1dl	150	3000	dl-sil	3:2:7:0	10	9500	1000	8500	8500	60
cd2dl	150	3500	dl-sil	3:2:7:0	10	9500	1000	8500	8500	60
cd3dl	150	3500	dl-sil	3:2:7:0	10	9500	1000	8500	8500	100
cd4dl	150	3000	dl-sil	3:2:0:7	10	9500	1000	8500	8500	60
cd1os	150	3000	oss-sil	3:2:7:0	10	9500	1000	8500	8500	60
cd1py	150	3000	Pyroxene	3:2:7:0	10	9500	1000	8500	8500	60
cd1ol	150	3000 ^c	Olivine	3:2:7:0	10	9500	1000	8500	8500	60
s1dl	150	3000	dl-sil	3:2:7:0	10	9500	−	−	−	1^b
d1dl	150	3000	dl-sil	3:2:7:0	10	9500	−	−	8500	60

Notes. ^aReferences for different silicate grains are: dl-sil: Draine & Lee (1984), oss-sil: Ossenkopf et al. (1992), pyroxene: Dorschner et al. (1995), olivine: Dorschner et al. (1995). ^bf_ρ=1 is implemented to remove the outer shell. ^cReproducing the cd1ol model with a synthetic stellar spectrum indicates that the central star is more likely to have a temperature of 3500 K. See Sect. 5.

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