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And, in particular, when does dust mass growth become dominant as a source of dust mass?
Time evolution of the ratio of dust mass produced by stars to metal mass ejected by stars.
In this paper, we investigate what is the main driver of dust mass growth in the ISM.
Fig. 3. Left: Percentage of dust mass carried by Fe as a function ol the gas-to-dust mass ratio Rg/d (from Frisch and Slavin, 2003).
After dust mass growth has taken place, the effect of dust destruction by SN shocks approaches that of dust mass growth.
Inoue (2011) defined a critical metallicity to compare the contribution of dust destruction by SN shocks with that of dust mass growth.
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Time-Of-Flight dust mass spectrometer and Hybrid dust detector which are under development in Japan have been investigated using HIT dust accelerators.
In addition, we also observe that the increase of the contribution of the dust mass growth (dot-dashed line) has a peak, after which, the increase slows down.
A third characteristic of the depletion pattern appears when depletions in tenuous and translucent clouds are combined to display the gas-to-dust mass ratio, Rg/d, as a function of the percentage of the dust mass carried by Fe (Fig. 3, left, and Frisch and Slavin (2003)).
One reason for this may be that most of the dust mass input consists of relatively small particles (radius <100 μm) entering the atmosphere in a near prograde orbit with low velocity (<15 km s 1, as predicted by the zodiacal cloud model of Nesvorný et al).
Inoue (2011) showed that the convergence value of δ is determined by the balance between the contribution of dust destruction by SN shocks and that of the dust mass growth (for details, the product of τacc, 0 and ϵmswept).
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