Cold dust in three massive evolved stars in the LMC

Table 2:

SED fit parameters and results.
	T_*	L_*	$T_{\rm in}$	R_*	$R_{\rm out}/R_{\rm in}$	$R_{\rm in}$	$\dot{M}_{\rm total}$	$T_{\rm dust}^{\rm sub-mm}$	$M_{\rm dust}^{\rm sub-mm}$
	(10⁴ K)	( $10^5~L_\odot$ )	(K)	( $R_\odot$ )		(km)	( $M_\odot~{\rm yr}^{-1}$ )	(K)	( $M_\odot$ )
R71 (inner/outer shell)	1.5	4.6	490/120	100	2/1.6	$\sim$ 10¹¹/10¹²	$\sim$ 10^-6 / $\sim$ 10^-4	$9 \pm 1$	$\gtrsim$ 10^-1
IRAS05280-6910	0.3	2.2	250	1700	30	$\sim$ 10¹¹	$\sim$ 10^-3	...	...
HD 36402	18	4.6	960	15	300	$\sim$ 10¹⁰	$7\times10^{-6}$	...	...
HD 36402 IR1 (YSO2)	...	...	...	...	...	...	...	64/15 ( $\pm 1$ )	10^-12/> $1.5 \pm 0.4$

Notes. Fitting results from 2-D UST. DUSTY fits for R71 and IRAS05280-6910 estimate outer shell MLRs 2 $\times$ to 4 $\times$ less than the 2-D UST results. IR1/YSO2 was fit with two modified blackbodies (64 K and 15 K). For R71, we use O-deficient silicate optical constants (Ossenkopf et al. 1992) at long wavelengths and astronomical silicate optical constants (Draine & Lee 1984) at $\lambda < 0.18$ $\mu$ m. For IRAS05280-6910, we use Ossenkopf et al. (1992) O-deficient silicates and for HD 36402, we use amorphous carbon grains from Zubko et al. (1996). The 2-D UST models use a KMH grain size distribution (Kim et al. 1994) with $a_{\rm min}=0.01~\mbox{$\mu$ m}$ and $a_0=0.1~\mbox{$\mu$ m}$ ( $a_0=1~\mbox{$\mu$ m}$ for IRAS05280-6910). Stellar parameters for R71 are consistent with those from Lennon et al. (1993). $T_{\rm dust}^{\rm sub-mm}$ is the temperature of the coldest dust component. For IRAS5280-6910, $\upsilon_{\rm wind}$ is measured from the maser emission (20 km s^-1; Marshall et al. 2004). For R71, we use 10 km s^-1, but the velocity measured from the H $\alpha$ profile indicates the inner shell velocity may be >10 $\times$ larger (Stahl et al. 1986). For HD36402, a typical velocity for a WC4 star is assumed (3000 km s^-1; Willis et al. 2004).

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