We have shown that the dust amount is very small before ISM growth becomes active.
Many physical processes are related to the evolution of the dust amount.
If the dust-mass growth by material accretion in molecular clouds is active, the observed dust amount in the solar neighborhood is reproduced.
At a time around 4 Gyr, τac becomes shorter than τsn, and then the accretion growth becomes significant and the dust amount increases rapidly.
Thus, after dust mass growth becomes efficient, the dust amount in galaxies determines the balance between the effect of dust destruction and that of dust mass growth in the ISM (see also Inoue, 2011).
Percentage of marble dust, amount of glass fiber and degree of temperature were changed to explore their effects on the compressive strength and porosity values of specimens.
These have shown that it is difficult to explain the total dust amount in these QSOs only with stellar contributions, and the importance of dust mass growth in the ISM has been discussed.
Inoue and Kamaya (2003, 2004) discussed the effect of the photoelectric heating by the intergalactic dust on the thermal history of the IGM, obtaining an upper limit of the intergalactic dust amount.
Furthermore, the process of dust mass growth is expected to explain the dust amount in the Milky Way or dusty QSOs at high redshifts (e.g., Zhukovska et al., 2008; Draine, 2009; Michalowski et al., 2010a; Valiante et al., 2011).
for example, the present dust amount observed in the Milky Way cannot be explained if the source of dust was only stars, suggesting that we must consider the dust mass growth in the ISM in evolved galaxies (e.g., Liffman and Clayton, 1989; Dwek, 1998; Draine, 2009; Jones and Nuth, 2011).
