The problem of how to make H2 in Space E(r) H…H r (H-H) 

H + H E(r) H…H r (H-H) 

H + H E(r) Chemical Energies H…H r (H-H) 

H2 H + H E(r) Chemical Energies H…H r (H-H) 

D H2 H + H E(r) Chemical Energies H…H r (H-H) 

Nuclear Energies D H2 H + H E(r) Chemical Energies H…H r (H-H) 

To take away the excess energy there must be a 3-Body collision during the lifetime of the H…H collision complex ca 10-13 s H2 E(r) H…H r (H-H) 

A A A A G G G G H HHHHHHHHHHHHHHH E(r) H…..H H–H r (H-H) 

Total energy must be conserved and in a plant at snooker or billiards the blue ball takes away the energy and the white and red can thus remain in contact after collision

H2 H2  H2+  H3+ + e- + H

3 body collision t3B = 1023/ n2 yrs t3B = 1023/ 12 yrs Harry Kroto 2004

2-body collisions t2B = 103/n yrs A + B  AB*  A + B Harry Kroto 2004

H2 H2  H2+  H3+ + e- + H

At NTP gas-phase reactions NB At NTP gas-phase reactions are 3-body processes

3 body collision t3B = 1023/ n2 yrs

3 body collision t3B = 1023/ n2 yrs = 3x107x1023 /(1018)2 = 3x10-6 Harry Kroto 2004

3 body collision t3B = 1023/ n2 yrs A + B + M  [MAB]  AB + M Harry Kroto 2004

3 body collision t3B = 1023/ n2 yrs A + B + M  [MAB]  AB + M t(BIG U) ~ 1010 yrs Harry Kroto 2004

3 body collision t3B = 1023/ n2 yrs A + B + M  [MAB]  AB + M t(BIG U) ~ 1010 yrs n = atoms or mols per cm3 Harry Kroto 2004

3 body collision t3B = 1023/ n2 yrs Harry Kroto 2004

2-body collisions t2B = 103/n yrs (3x107)x103/1018 = 3x10-8 Harry Kroto 2004

3 body collision t3B = 1023/ n2 yrs t3B = 1023/ 12 yrs = 1023/ (1018)2 Harry Kroto 2004

The problem of how to make H2 in Space 3-Body collision during the lifetime of the collision complex ca 10-13 s E(r) H…H H…H r (H-H)  Harry Kroto 2004

E(r) H + H r  H2 Harry Kroto 2004

The problem of how to make H2 in Space 3 Body collision during the lifetime of the collision complex ca 10-13 s E(r) H……..H r  Harry Kroto 2004

E(r) H...H r  Harry Kroto 2004

t(BIG U) = 1010 yrs n = atoms/mols per cm3 Lifetimes (in yrs) Photo dissociation tPD = 103 AB + h  A + B 2-body collision t2B = 103/n A + B  AB*  A + B Radiative assocn tRA = 109/n A + B  AB*  AB + h Grain catalysis tGC = 109/n A + B + Gr  AB + Gr 3 body collision t3B = 1023/ n2 A + B + M  MAB  AB + M t(BIG U) = 1010 yrs n = atoms/mols per cm3

The problem of how to make H2 in Space E(r) A A A A G G G G H H H...H r  Harry Kroto 2004