**Table 1:** Model parameters.
Id	Time (yr)	$M_\star (M_{\odot})$	$R_{\rm S}$ (AU)	$Z_{\rm S}$ (AU)	$M_{\rm S} (M_{\odot})$	$\dot{M}_\star (M_{\odot}$ yr^-1)	$L_{\rm TOT} ({L}_{\odot})$	$T_\star$ (K)	Description
`t`0	0	-	-	-	-	-	-	-	initial conditions
`t1`	$5.3\times10^{4}$	-	-	-	-	-	-	-	before sink formation
`t2`	$5.3\times10^{4}$	0.01	4.0	3.4	0.04	$5\times10^{-5}$	5.7	5150	a protostar has formed
`t3`	$6.0\times10^{4}$	0.20	4.0	0.4	0.09	$1\times10^{-5}$	27.2	7650
`t4`	$6.8\times10^{4}$	0.49	4.0	0.4	0.05	$2\times10^{-6}$	12.3	6250
`t5`	$6.9\times10^{4}$	0.53	4.0	0.4	0.01	$4\times10^{-7}$	2.5	4200	protostar is off centre

$Z_{\rm S}$ , $R_{\rm S}$ : Smartie dimensions (Fig. 1). $M_{\rm\star}$ : Stellar mass. $T_\star$ : Star temperature. $M_{\rm S}$ : Smartie mass.
$\dot{M}_\star$ : Accretion rate onto the central star. $L_{\rm TOT}$ : Total star luminosity (intrinsic + accretion).

Source LaTeX | All tables | In the text

	1 Introduction
	2 The SPH simulation
	3 The radiative transfer simulation
	4 The evolution of the dust temperature field, SED and isophotal maps in a star-forming core
	5 Summary
	References