Selected Questions - Answers From All Experts Astronomy Forum (Giant Molecular Clouds)

Question: I have been reading about "giant molecular clouds" what are they and what are they made of? - Benji, Portland OR

Answer:  Giant molecular clouds - such as that shown (Rosette Nebula) consist mainly of molecular hydrogen (H2) but other molecules can also be present including:

OH  Hydroxyl radical

CO carbon monoxide

HCN   Hydrogen Cyanide

H2O   water

NH3  Ammonia

H2 CO  Formaldehyde

HC2 H   Acetylene

CH4   Methane

HCOOH   Formic acid

CH2 OH   Methyl alcohol

CH2 CN   Methyl cyanide

CH3 NH2  Methylamine

CH2 CH2 CN Ethyl cyanide

HCOOCH3  Methyl formate

This is just to give you an idea of how many different molecules can be found in these molecular clouds, usually associated with a type of nebula containing what we call HI regions (neutral hydrogen) as well as H II regions (single ionized hydrogen)   Most of the 'exotic' molecules listed tpo be sure, make up only a relatively small proportion of the total mass of such clouds, and were discovered through radio observations beginning in the 1960s.

We acknowledge here that optical observation alone aren't the most practical for detecting such component molecules given different energy states can arise depending on how the atom vibrates or the molecule spins.

Here we can think of the internal energy (U) of a given molecule - say hydrogen H2- and note there are three degrees of freedom or parts: translational, rotational and vibrational

U = U(transl.) + U(rotational) + U (vibrational)
On average then, the available energy is equally shared by each independent degree of freedom, acknowledging at once that molecules can not only move from point a to point b in space (translation), but also rotate and vibrate. Each of these contributes (½ kT) of energy on average. For the different translational velocity directions, i.e. in 3 space directions x, y, and z (v_x, v_y and v_z ) we than have a total contribution of 3((½ kT) = 3kT/2. To obtain the rotational energy contributions we can use the "dumbbell" model shown in the graphic:


 where the system can rotate either in the z-plane (e.g. about the x-axis) or in the x-plane (about the z-axis). Since there is (½ kT) of energy for each of these then the total contributed to internal energy U is: 2((½ kT)= kT.  If we finally add in the possible vibrations (visualizing the dumbbell atoms connected via 'springs') we get on more kT contribution to make: 5kT/2 + kT = 7kT/2, so U = 7kT/2.

Having stated he relative abundance of most molecules in giant molecular clouds are small relative to hydrogen, it is also useful to note that the most common of those other molecules are carbon monoxide, ethyl alcohol and water.   Again, in order to remain as molecules these need to be localized in dark, denser cold regions - which, however, often lie close to H II regions.  (One of the nearest molecular clouds is situated behind the Orion Nebula)

In terms of density, the typical  molecular cloud region has average densities ranging from  10^{8  -}  10¹²    molecules per cubic meter.  This compares to a density of   10⁸  molecules per cubic meter for the interstellar medium and about 1,000 atoms per cubic meter near the edge of our solar system.   The total mass of these giant ,molecular clouds generally ranges from   10^{4  -}  10⁷ solar masses and 10 ⁵   solar masses is typical.  Typical low density molecular clouds can extend 30 light years across with a "core" of perhaps 0.5 Ly.    These "cores" are generally at a low temperature of 10 K  and are where densities can attain 10¹²  molecules per cubic meter.

Interestingly, giant HII regions, i.e. those surrounding young, massive stars, often connect to giant molecular clouds. In some cases - like the Rosette nebula-  models show a "co-moving" HII shell with an Hi molecular cloud.

If you are up to it you can read about this model for the Rosette in this paper from the Monthly Notices of the Royal Astronomical Society.

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