The star formation factory revisited - I. The impact of metallicity on collapsing star-forming clouds

Open Access

Fig. 3

Time evolution of the shell radius (top left), shell mass (top right), stellar mass (bottom left), and thermal energy (bottom right) for the low metallicity (IZw18) models, which were performed for three different values of ϵ_ff (the first three models listed in Table 1). The colour map shows the average initial gas number density of the clouds, ${\bar{n}}_{c l} = 3 M_{g a s, 0} / (4 π μ m_{H} R_{c l, 0}^{3})$ $Mathematical equation: $\[\bar{n}_{\mathrm{cl}}=3 M_{\mathrm{gas}, 0} /\left(4 \pi \mu m_{\mathrm{H}} R_{\mathrm{cl}, 0}^{3}\right)\]$$ .

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