Sentence examples for grain disruption from inspiring English sources

The processes considered are (i) "grain growth"—grain growth by accretion and coagulation in a dense medium, (ii) "shock destruction"—destruction by sputtering in SN shocks, and (iii) "grain disruption"—grain disruption by shattering in interstellar turbulence.

The 0.22 μm bump created by small graphite grains in this model becomes also prominent by grain disruption.

Grain disruption steepens the extinction curve because of the production of a large number of small grains.

Grain motions driven by interstellar turbulence lead to grain disruption (shattering) in the diffuse ISM (Yan et al, 2004; Hirashita and Yan, 2009).

We have shown that the grain size distributions after (i) grain growth, (ii) shock destruction, and (iii) grain disruption can synthesize the MRN size distribution.

This means that the fitting is practically dominated by the balance between the decreased small grains in shock destruction and the increased small grains in disruption (shattering).

In other words, these two quantities show the relative importance of grain growth and disruption.

Since they focus on the early stage, they did not include other processes such as grain growth and disruption (shattering), which are important in solar-metallicity environments such as in the Milky Way (Hirashita and Yan, 2009).

Controllable changes in the energy of incident particles adjusted by bias voltages ranging from −40 to −120 V affect the competitive growth of grains with different orientations, induce disruption of grain growth and thus give rise to structural variations across the film thickness.

In our previous papers (Nozawa et al., 2006; Hirashita and Yan, 2009; Hirashita, 2012), we showed that dust grains are quickly processed by shock destruction, disruption, and grain growth.

We denote the grain size distribution after disruption as ndisr a, tdisr), where tdisr is the duration of shattering in the WIM.