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Yamasawa et al. (2011) have recently calculated the evolution of the grain size distribution in the early stage of galaxy evolution by considering the ejection of dust from SNe and subsequent destruction in SN shocks.
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But that doesn't explain what is causing those random ejections of dust.
Numerical modeling of dust ejection indicates radiation pressure may also be responsible and suggests that planets further than about 1 AU from the star cannot directly cause the dust stream.
Perhaps these ejections are like little avalanches of dust falling off the asteroid's surface before the thing finally breaks up entirely.
More recently, Nesvorný and co-workers have developed a zodiacal cloud model which starts with the orbital properties of comets and asteroids and follows the dynamical evolution of dust particles after ejection from these sources.
Solid, dotted, dashed and dot-dashed lines represent the rates of dust injection into stars, dust ejection by stars, dust destruction by SN shocks and dust mass growth in a galaxy, respectively.
After ejection the dust drifts in the direction of the planet under the action of Poynting Robertson drag forming a ring inward of the moon.
From the first stages of star and galaxy formation, non-gravitational processes such as ram pressure stripping, SNs, galactic winds, AGNs, galaxy galaxy mergers, etc. lead to the enrichment of the IGM in stars, metals as well as dust, via the ejection of galactic material into the IGM.
"They get full of dust.
One atom of dust?
A speck of dust?
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Justyna Jupowicz-Kozak
CEO of Professional Science Editing for Scientists @ prosciediting.com