What force keeps a bunch of hot gas molecules from dissipating in star formation process?
Gravity dominates electromagnetism over large distances. Get enough gas in a large space (say 10 parsecs across), and there will be enough gravitational pressure to crush the particles near the center. This has been seen in simulation.
From "Universe" 5ed by Kaufmann and Freedman, p. 498, "Protostars form in cold, dark nebulae":
"In order for a star to condense, gravity ... must overwhelm the pressure pushing it apart. This means stars will most easily form in regions where the interstellar material is relatively dense, so that atoms and dust grains are close together and gravitational attraction is enhanced.
"To assist star formation, the pressure of the interstellar medium should be relatively low. This means that the interstellar medium should be as cold as possible...
"The only parts of the interstellar medium with high enough density and low enough temperature for stars to form are the dark nebulae. Many of these ... were discovered and catalogued around 1900 by Edward Barnard and are known as Barnard objects... The density of the gas and dust within a Barnard object ... is indeed quite high by cosmic standards... [Their] temperatures are very low, only about 10K...
"Within these clouds, the densest portions can contract under their own mutual gravitational attaction and form clumps called protostars."
It later goes on to describe calculations in the 50's have predicted that protostars, which begin as much larger than our solar system, slowly collapse and build up internal temperatures. These calculations, though it doesn't describe them, probably involve the use of Green's functions to compute forces by integration; if you're interested in reproducing the work yourself, you'll need to read up on multivariate calculus and Green's functions. Also, see the work of Louis Henyey (U.S.) and C. Hayashi (Japan), both from the 1950's.
I understand that the last bit, "the densest portions can contract under their mutual gravitation attraction", effectively dodges your question. But I hope you can at least see that it doesn't have to start out very hot, and that 10 parsecs of gas will generate quite a lot of gravitational attraction. Lastly, you should remember that for objects far from the center of mass C of an complex body, you may treat the complex body as a point mass located at C for the purposes of calculating both gravitational and electromagnetic forces.
Hope this helps.
Then how come Polonium halos are found in granite all over the world? Wouldn't the atom decay waaay before even getting to Earth? Check out work of Robert Gentry on polonium halos for more specific information.
I am ignorant on the subject of polonium halos. However, a possible quick answer to the question, "Why do we find polonium at all, wouldn't it decay before it reaches the Earth from the nearest supernova?" is that while its travelling through space, it isn't polonium yet, but decays some time after its arrival here. Polonium is one of the stages of uranium decay, and uranium has a very long half life. As long as uranium arrives here from someplace, it will eventually turn into polonium, which may then be found in halo form -- whatever that is -- in granite.
I will seek out more information on polonium halos.
-Erasmus