comparison of gas and dust cooling rates in - Rencontres de Moriond
comparison of gas and dust cooling rates in - Rencontres de Moriond
comparison of gas and dust cooling rates in - Rencontres de Moriond
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E. Bayet<br />
OBSERVED LINES :<br />
CO = good tracer <strong>of</strong> H 2 molecular masses<br />
C l<strong>in</strong>ked with PDRs (mostly <strong>in</strong> the first layers)<br />
From Hollenbach & Tielens (1999)<br />
<strong>Moriond</strong> – March, 6th-12th 2005<br />
Study <strong>of</strong> the variation <strong>of</strong> C over CO<br />
<strong>de</strong>nsity ratio N(C)/ N(CO) <strong>in</strong> the<br />
molecular cloud<br />
Clouds are ruled by: heat<strong>in</strong>g<br />
- photoelectric effects on gra<strong>in</strong>s<br />
- collisionnal <strong>de</strong>excitation <strong>of</strong> H 2<br />
<strong>cool<strong>in</strong>g</strong> (con<strong>de</strong>nsation <strong>of</strong><br />
clouds = star formation)<br />
- neutral layer (Av < 5): CII, OI<br />
- molecular layer (Av > 5) : CO & C<br />
CO l<strong>in</strong>es refer to transitions between two<br />
rotationnal levels<br />
C l<strong>in</strong>es refer to transitions between two<br />
electronical levels
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