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

2. H + H
E(r)
H…H
r (H-H) 

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

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

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

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

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

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

9. 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

10. H2
H2  H  H3+
+ e H

11. 3 body collision t3B = 1023/ n2 yrs t3B = 1023/ 12 yrs
Harry Kroto 2004

12. 2-body collisions
t2B = 103/n yrs
A + B  AB*  A + B
Harry Kroto 2004

15. H2
H2  H  H3+
+ e H

16. At NTP gas-phase reactionsNB
At NTP gas-phase reactions
are 3-body processes

17. 3 body collision
t3B = 1023/ n2 yrs

18. 3 body collision t3B = 1023/ n2 yrs = 3x107x1023 /(1018)2 = 3x10-6
Harry Kroto 2004

19. 3 body collision t3B = 1023/ n2 yrs A + B + M  [MAB]  AB + M
Harry Kroto 2004

20. 3 body collision t3B = 1023/ n2 yrs A + B + M  [MAB]  AB + M
t(BIG U) ~ 1010 yrs
Harry Kroto 2004

21. 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

22. 3 body collision
t3B = 1023/ n2 yrs
Harry Kroto 2004

23. 2-body collisions t2B = 103/n yrs (3x107)x103/1018 = 3x10-8
Harry Kroto 2004

24. 3 body collision t3B = 1023/ n2 yrs t3B = 1023/ 12 yrs
= 1023/ (1018)2
Harry Kroto 2004

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

26. E(r)
H + H
r  H2
Harry Kroto 2004

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

28. E(r)
H...H
r 
Harry Kroto 2004

29. t(BIG U) = 1010 yrs n = atoms/mols per cm3
Lifetimes (in yrs)
Photo dissociation tPD = 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/ n A + B + M  MAB  AB + M
t(BIG U) = 1010 yrs n = atoms/mols per cm3

30. 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