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Interstellar reddening occurs because interstellar dust absorbs and scatters blue light waves more than red light waves, making stars appear redder than they are. This is similar to the effect seen when dust particles in the atmosphere of Earth contribute to red sunsets. [6]
For submicron-sized dust particles this force becomes significant and for particles < 0.1 microns it exceeds solar gravity and the radiation pressure force. For example, interstellar dust particles of ~0.3 microns in size that pass through the heliosphere are either focused or defocused with respect to the solar magnetic equator.
The main physical processes "affecting" (destruction or expulsion mechanisms) interplanetary dust particles are: expulsion by radiation pressure, inward Poynting-Robertson (PR) radiation drag, solar wind pressure (with significant electromagnetic effects), sublimation, mutual collisions, and the dynamical effects of planets (Backman, D., 1997).
Fugitive dust is an environmental air quality term for very small particles suspended in the air, primarily mineral dust that is sourced from the soil of Earth's pedosphere.A significant volume of fugitive dust that is visible from a distance is known as a dust cloud, and a large dust cloud driven by a gust front is known as a dust storm.
Dust particles are charged and the plasma and particles behave as a plasma. [1] [2] Dust particles may form larger particles resulting in "grain plasmas". Due to the additional complexity of studying plasmas with charged dust particles, dusty plasmas are also known as complex plasmas. [3]: 2 Dusty plasmas are encountered in: Space plasmas
House dust under a microscope Domestic dust on a ribbon A video on reducing dust exposure in the workplace. Dust control is the suppression of solid particles with diameters less than 500 micrometers (i.e. half a millimeter). Dust poses a health risk to children, [12] older people, and those with respiratory diseases. House dust can become ...
This causes dust that is small enough to be affected by this drag, but too large to be blown away from the star by radiation pressure, to spiral slowly into the star. In the Solar System, this affects dust grains from about 1 μm to 1 mm in diameter. Larger dust is likely to collide with another object long before such drag can have an effect.
[19]: 341 In particular, it is still not clear how these objects grow to become 0.1–1 km (0.06–0.6 mi) sized planetesimals; [5] [20] this problem is known as the "meter size barrier": [21] [22] As dust particles grow by coagulation, they acquire increasingly large relative velocities with respect to other particles in their vicinity, as ...