HII regions slides

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ISM: average properties• Mean density of ISM (in our Galaxy) ~ 10 6 particles/m 3 (1 particle/cm 3 )but is HIGHLY CLUMPED: filling factor ~3%.• The GAS is mainly:Hydrogen (90%)Helium (10%)metals (C,N,O, ... Fe)
A global model:the 3+1 phases of the ISM• Cold, neutral medium (CNM)n ~ 110 3 /cm 3 , T < 100 K, volume fraction: ~15%• Hot, ionized medium (HIM)n ~ 10 -4 10 -2 /cm 3 , T ~ 10 6 10 7 K, volume fraction: ~3070%• Warm interface media• Warm ionized medium (WIM)n ~ 0.01 /cm 3 , T ~ 1000 K, volume fraction: ~2050%hydrogen ionization fraction (X H ) ~ 70%• Warm neutral medium (WNM)n ~ 0.110 /cm 3 , T ~ 10005000 K, volume fraction: ~1020%hydrogen ionization fraction (X H ) ~ 10% Dark neutral (molecular) cloudsn ~ 10 3 10 6 /cm 3 , T ~ 10 50 K, volume fraction:
Page 1: Today:Recap on 1 st lecture:- Basic
Page 6 and 7: Distance = 450 pcDiameter ~ 1° (si
Page 8 and 9: Dark CloudsBok globules• relative
Page 14: A global view
Page 18 and 19: Cold, neutral medium (CNM)• domin
Page 20 and 21: www.milkywayproject.org
Page 22 and 23: Lagoon nebula
Page 25 and 26: PhotoionisationPhotoionisation: the
Page 27 and 28: Photoionisation: the removal of ele
Page 29 and 30: Balmer seriesLyman series(UV)Recomb
Page 31 and 32: Optical SpectrumPlanetary Nebula: N
Page 33 and 34: AtomsThe Maxwellian DistributionVel
Page 35: cross sectionse nucleuselectric fie
Page 39 and 40: For a typical O-star (e.g. the O6V
Page 42 and 43: M43Real examples1. no. of ionising
Page 44 and 45: However, Q per ionization is: (3/2)
Page 46 and 47: excitation/de-excitation of bound e
Page 48 and 49: Collisionally excited lines (CELs)B
Page 50 and 51: O +CELs (forbidden lines) are writt
Page 52 and 53: compare energy level diagrams1S 05.
Page 54 and 55: Forbidden line coolingtransition ra
Page 56 and 57: www.jodcast.netTopical podcast with
Page 59: DensitiesObservations n e ~ 100 cm
Page 62 and 63:
Fraction of O2+ ions able to emit 4
Page 64 and 65:
End of last lecture
Page 66 and 67:
Today:HII regions: Practical method
Page 68 and 69:
compare energy level diagrams1S 05.
Page 70 and 71:
DensitiesObservations n e ~ 100 cm
Page 72 and 73:
Practical methods and examples
Page 74 and 75:
eal example
Page 76 and 77:
• End of stellar existence for lo
Page 78 and 79:
Optical Recombination Lines• ORLs
Page 80 and 81:
Possible solutions?• Possibility
Page 82 and 83:
Any other ideas?• Possibility 3:
Page 84 and 85:
Knots: Abell 30• Results of empir
Page 86:
Conclusions• Cold H-deficient kno
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HII regions slides

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