![]() ![]() In diffuse clouds H 3 + is destroyed via electron recombination, while in dense clouds destruction primarily occurs by charge tranfer with CO. ![]() It is generally assumed that a cosmic ray first ionizes H 2, which then collides with another H 2 molecule to form H 3 + and H. ![]() The reactions surrounding the formation and destruction of H 3 + are relatively simple. This is because H 3 + willingly donates its extra proton to a variety of collision partners, thus laying the foundation for a large network of ion-molecule reactions. H 3 + is extremely important to the chemistry of interstellar clouds. Arrows indicate the expected positions of the absorption features from previous measurements of the interstellar gas velocity. Spectra of three interstellar clouds showing absorption lines due to the R(1,1) u and R(1,0) transitions of H 3 +. ![]()
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