Interstellar dust

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H 2 formation rate: Photo-dissociation Regions ISOCAM MAP (in the LW2 filter) Rotational transitions of H 2 and PAHs emission ISO SWS Rotational transitions of H 2 ISO LWS ISOCAM- CVF Spectro- imaging Rotational transitions of H 2 Abergel et al. 1996 Habart et al. 2003 Gas temperature Photodissocation of H 2 Formation rate of H 2 Grain temperature
H 2 formation rate: Photo-dissociation Regions Observations of several PDRs (Abergel et al. 1996; Habart et al. 2003) T <strong>dust</strong> = 15 - 90K T gas = 60 - 620K R(H 2 )= 3 10 -17 - 1.5 10 -16 cm 3 s -1 H 2 formation @ high T<strong>dust</strong> and Tgas → para sites properties Other factors: R(H 2 )=(1/2) n H v H n d S H abundances PAHs/very small grains (AC) (Compiegne et al. 2008, Joblin et al ) Gry et al. 2002 Habart et al. 2004
Page 1 and 2: Interstellar dust: The hidden prota
Page 3 and 4: Dust as catalyst/ reservoir H 2 in
Page 5 and 6: Dust as a reservoir: interstellar i
Page 7 and 8: Interstellar dust grains Grain size
Page 9 and 10: Interaction atom/surface: experimen
Page 11 and 12: Model: Interaction and mobility phy
Page 13 and 14: Formation of H 2 on dust
Page 15 and 16: Interaction atom/surface: Density f
Page 17 and 18: Interaction atom/surface: experimen
Page 19: H 2 formation rate in the ISM R(H 2
Page 23 and 24: Experiment H 2 formed on PAHs L. Bo
Page 25 and 26: More complex species Star form in c
Page 27 and 28: Grain surface chemistry: Monte carl
Page 29 and 30: Grain surface chemistry: Monte carl
Page 31 and 32: Grain surface Results Gas phase Tes
Page 33 and 34: Diffuse clouds Diffuse clouds: H at
Page 35 and 36: UV and X-rays star forming regions
Page 37 and 38: Dust grains as catalyst Formation s
Page 39 and 40: Impact of dust on gas: experiments
Page 41 and 42: Dust in Flash Flash + cooling at di

Interstellar dust

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