Astrophysics (index)about

cosmic dust

(cosmic dust is dust in space such as interstellar dust)

Cosmic dust is a general term for dust in space, which includes intergalactic dust, interstellar dust, and interplanetary dust. Dust leads to extinction, making observation of stars and other astronomical bodies more difficult, but is also observed both for itself and for the conclusions that can be drawn from reradiation and scattering.

Though termed dust, it can be orders-of-magnitude smaller than everyday dust: in the interstellar medium, what are termed dust particles (or referred to as particles, or dust grains or grains) are a few molecules, though in the interplanetary medium, presumably all sizes particles exist, from micrometeoroids down. Essentially, once two molecules stick together, dust is the term used. They are presumed to have the opportunity to grow larger in molecular clouds, and clearly grow further in protoplanetary disks, a necessary stage in planet formation. In such disks, the term dust is used for that which gathers from the cloud, on the order of a micron in diameter, up to what are termed pebbles, on the order of a few millimeters or a centimeter in diameter.

Infrared can be used to see through dust, and extinction, scattering, absorption, and polarization reveal information about the dust itself.

Much dust is thought to be formed by stars toward the end of their main sequence, such as red giants. It is also formed or scattered by novae and supernovae. The term nebula has come to be most commonly used for clouds that include sufficient interstellar dust to be opaque to visible light.

The best means of discerning dust particle size is the effects of the scattering of electromagnetic radiation via diffraction as well as the particles' emission and absorption.

Dust maps of the Milky Way are of interest to aid in interpretation of photometry of Milky Way stars as well as basically every other galactic or extragalactic observation. A means of creating them is through analysis of stellar distance and photometric survey data.


Referenced by:
Baade's Window
Bok globule
Bondi radius
carbon star
circumgalactic medium (CGM)
cosmic infrared background (CIB)
circumstellar disk
infrared cirrus
dark nebula
debris disk
disk galaxy
dwarf spheroidal galaxy (dSph)
elliptical galaxy
extra-solar planet
far infrared (FIR)
galactic center
galactic halo
galaxy merger
Gould's Belt Distances Survey (GOBELINS)
helium runaway shell
hot DOG
Hubble Ultra-Deep Field (HUDF)
hydrogen (H)
IC 342
intergalactic medium (IGM)
infrared (IR)
interplanetary medium (IPM)
interstellar medium (ISM)
James Clerk Maxwell Telescope (JCMT)
kilometer size barrier
light echo
luminous infrared galaxy (LIRG)
mass spectrometer
meter size barrier
Morgan classification
Milky Way chemical evolution
near infrared (NIR)
New Horizons (NF1)
Spindle Galaxy (NGC 5866)
OH/IR source
1.3mm observation
Orion Nebula (M42)
passive dust
planetary embryo
planet formation
Poynting-Robertson effect
protoplanetary disk (PPD)
reflection nebula
spectral energy distribution (SED)
star formation rate (SFR)
star-forming region (SFR)
submillimeter galaxy (SMG)
supernova (SN)
solar nebula
solar system
spiral galaxy
starburst galaxy
star formation (SF)
star system
21cm line
Toomre Q parameter (Q)
Trapezium Cluster
Wide-field Infrared Survey Explorer (WISE)
zone of avoidance (ZOA)
zodiacal light