How Does Stellar Radiation Clear Dust from a Proto-Planetary Disc?

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SUMMARY

Radiation from a star effectively clears dust from a proto-planetary disc by exerting radiation pressure that pushes smaller dust particles outward, transitioning the area from opaqueness to transparency. The force of radiation pressure is proportional to the radius squared, while gravitational force is proportional to the radius cubed, which explains why smaller particles are more affected by radiation than larger, more massive objects. This differential scaling illustrates fundamental principles in astrophysics regarding the interaction between radiation and matter.

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  • Understanding of radiation pressure and its effects on small particles
  • Basic knowledge of gravitational forces and mass distribution
  • Familiarity with the concepts of proto-planetary discs in astrophysics
  • Awareness of scaling laws in physics
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  • Research the role of radiation pressure in astrophysical processes
  • Explore the dynamics of proto-planetary disc formation and evolution
  • Study the mathematical relationships between force, mass, and radius in astrophysics
  • Investigate the implications of differential scaling in various physical systems
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Astronomers, astrophysicists, and students of cosmology interested in the mechanisms of dust clearing in proto-planetary discs and the effects of stellar radiation on small particles.

RJ Emery
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How does radiation from a star clear dust from a proto-planetary disc, changing the area from one of opaqueness to one of transparency?

Please note that I am a retired engineer with an interest in astronomy, cosmology and particle physics but very much a layman..
 
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Thanks for answering my question.
 
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RJ Emery said:
Thanks for answering my question.

Thanks for asking your question. :wink:
 
RJ Emery said:
How does radiation from a star clear dust from a proto-planetary disc,
I'd like to add to the contribution from @Drakkith . You might ask why the radiation affects just the dust and not all the bigger stuff. It's because the area that the radiation acts on an object (and hence the force) is proportional to the radius squared (A = πr2) BUT the gravitational force on an object is proportional to its Mass, which is proportional to the radius cubed. (Mass = density times 4πr3/3). For small objects the radiation pressure wind and for large (massive) objects, the gravitational force wind.
This is just an example of how things don't scale in a simple way - why fleas can jump much higher than elephants - in terms of the animals' own height - and why a mouse can jump of the Empire State Building and land safely but one of us . . . . . . . .
 

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