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Star Formation(Compare: Solar System Formation)
Where Stars come from: the Interstellar Medium
• Gas– Single atoms and molecules– Mostly hydrogen (90%), 9% helium; deficient in heavier
elements
• Dust– Microscopic clumps of atoms/molecules– Size ~ 107 m, similar to the wavelength of visible light– Composition is not well known
• Temperature depends on the proximity of stars, typically ~100 K
• Density is very low!– Gas: about 1 atom/cm3 D; Dust: even less dense
How do we know it’s there?
• Cold gas or dust doesn’t glow– they are dark
– We might “see” them blocking light of other objects (Dark Nebulae)
• Gas & Dust clouds are very dilute– they might not be blocking other
object’s light totally
– Usually they will reduce (redden) the light of other objects
Reminder: Kirchhoff’s Laws
Cool gas absorbs light at specific frequencies
Dark Lines: “fingerprints of the elements”
Looking Through Dust Clouds
Seeing Through Gas and Dust• EM radiation is appreciably
scattered or absorbed only by particles with size comparable to its wavelength (or larger)
• Gas– Emission and absorption
lines
– Doesn’t block EM radiation
• Dust– Grain size is comparable to the wavelength of visible light
– Dims visible light and high frequency EM radiation
– Transparent to longer wavelength radio and infrared radiation, though
Scattering in Earth’s Atmosphere
The Interstellar Medium
• Dust dims and reddens the light from distant stars
Dust Clouds• What happens to the blue light scattered by the
dust clouds?• It’s still there, and sometimes can be seen
M20 Pleiades
Nebulae
• Any irregularly shaped cloud of gas and dust• May be bright or dark, depending on temperature• Types:
– Emission (bright) Nebulae
– Dark Nebulae
– Reflection Nebulae
• Historic Remark: Only some of the 109 “nebulae” catalogued by Charles Messier in 18th Century are actual nebulae; most are star clusters and galaxies
Dark Nebulae
• Classic Example: Horsehead Nebula in Orion
Can’t see what’s behind a dark nebula, that’s why we see it!
Dark Nebulae
• Dark Nebulae do emit light of their own, though
• Temperatures ~ 10 to 100 K; black body radiation peaks in the radio to infrared frequencies
fpeak in infrared frequencies
Dark Nebulae• Now you see it Now you don’t
• (infrared frequencies) (visible frequencies)
Rho Ophiuchi (visible light) Rho Ophiuchi (infrared)
Emission Nebulae
• Regions of hot glowing gas– Temperatures ~ 8000K
• Made to glow by ultraviolet radiation emitted by new O- or B-type (hot) stars located inside
• Emission lines from the nebula are easily distinguished from the continuous spectrum and absorption lines of stars within
• Color predominantly red, the color of a particular hydrogen emission line (the “H line”)
Trifid Nebula (M20)
Good example for dark dust lanes in front of an emission nebula
Emission Nebulae Example: Orion Nebula (M 42)
• hot glowing gasTemperatures ~ 8000K
• Made to glow by ultraviolet radiation emitted by young O- or B-type (hot)
stars located inside
• Color predominantly red, the color of a particular hydrogen
emission line (“H”)