1. Introductory remarks Takeshi Oka
Department of Astronomy and Astrophysics
and Department of Chemistry,
The Enrico Fermi Institute, the University of Chicago
Good morning. I am delighted that we are finally here together and begin the Royal Society Discussion Meeting on H3+. On behalf of the participants of the Meeting I wish to thank the Royal Society for their great help and support to this Meeting. We have two days of the Royal Society Discussion Meeting and one day of Satellite Meeting. They are equally important and exciting. The poster session too.
The Royal Society Discussion Meeting and Satellite Meeting
Kavli Centre, February 9, 2012

2. H3+
We are also celebrating the 100th anniversary of the discovery of H3+ by JJ Thomson, the 42 president of the Royal Society and the third Cavendish Professor. It is truly inspiring that H3+ initially discovered as a tiny dot here 100 years ago is now observed far away at the center of Galaxy and even outer Galaxy.
Thomson, J. J Rays of positive electricity. Phil. Mag. 21,
Thomson, J. J Further experiments on positive rays. Phil. Mag. 24,

3. Chemistry, astronomy and physics of H3+
Takeshi Oka
Mats Larsson
Steve Miller
Stephan Schlemmer
Secretary Ben McCall
In initiating these Meetings I was helped by Alex Dalgarno and Sir Harry Kroto. The Meetings have been organized with Mats Larsson, Steve Miller and Stephan Schlemmer. The Royal Society goes with the Britsh system and secretary’s name does not appear on the program, but we operate by the former Soviet system and the secretary Ben McCall had the supreme power. Also last but not least, we have been greatly helped by personnel at the Royal Society particularly by Tracey Wheeler who efficiently and cheerfully took care of the nitty-gritty of the Meetings.
Tracey Wheeler

4. Session 1, Spectroscopy and Theory
3n1+2n2
n1+ 4n24
6n22
2n1+3n2
6n20
n1+ 4n2
5n25
3n1+n2
5n23
5n21
2n1+2n2
4n24
n1+ 3n2
4n22
3n1
4n20
2n1+n2
n1+2n22
3n23
n1+2n20
3n21
2n1
n1+ n2
2n22
Morong et al. 2009
2n20
Gottfried et al. 2003
McCall et al. 2000 n1 n2
Xu et al. 1992
Bawendi et al. 1990
Majewski et al. 1987
Oka 1980

5. Session 1, Spectroscopy and Theory
10-8 Eh
non-adiabatic corr.
Jaquet SM
Polyansky RSDM
Adamowicz RSDM
Pavanello, et al. 2012, Phys. Rev. Lett. 108, ?
3ν1+ 4ν22
16000
ν1+ 6ν24
2ν1+ 5ν21
8ν22
ν1+ 6ν22
Ion counting
Petrignani, RSDM
Since these are inter-disciplinary Meetings by people with widely different background, I wish to count out some highlights of the subjects of discussions. The spectroscopy started in Together with the serendipitous discover of H3+ in Jupiter we observed higher transitions. Three years ago we terminated this brcause we ran out of the signal to noise ratio. The highest absorption is about million times weaker than the fundamental
to count Here I wish out some highlights of the Meetings so that you can all participate in the discussions.
This was pickeup up nicely by the action spectroscopy developed by Schlemmer, Gerlich and others. There has been a paradigm shift from photon counting spectroscopy to ion counting spectroscopy with much higher sensitivity and allowed to go deeply into the visible. This is just beginning and should allow us to do much deeper and to the ultraviolet. Alan Carrington’s spectrum is waiting at cm-1 still way up in the sky. The theoretical development has been even more spectacular.
< 10-6 Eh
Photon counting
Morong, Gottfried, Oka 2009, JMS, 255, 13
Sub-Doppler
Shy, Amano SM, P

6. Session 2, Chemistry H3+ + O2 → H2 + HO2+ H3+ + N2 → H2 + HN2+p
H3+ + O2 → H2 + HO2+
Schlemmer RSDM
He-HO2+, Ne-HO2+
Nizkorodov et al CPL, 278, 26
Widucus Weaver et al ApJ, 697, 601
H3+ + N2 → H2 + HN2+
ortho-H3+, para-H3+
McCall RSDM
Crabtree, Tom, McCall, 2011, J. Chem. Phys. 134,
Crabtree et al. 2011, J. Chem. Phys. 134,
Crabtree et al. 2011, ApJ, 729:15 (12pp)
H+ + H2 → H3+ + hν
Plasil SM
H3+ trapping noble gas
Pauzat SM
Mousis SM

7.  L = 2 ke N(H3+) (nC/nH)SV RX / f(H2)
Session 3, Dissociative recombination
H3+ + e˗ → H + H + H, H2 + H
 L = 2 ke N(H3+) (nC/nH)SV RX / f(H2)
Oka et al. 2005, ApJ, 632, 882
Cloud length
Cosmic ray ionization rate
Larsson RSDM
Johnsen SM
104 → 3
20 – 30 K
McCall et al. 2004, PR A70,
380 K
Petrignani et al. 2011, PR A83,
ortho-H3+, para-H3+
Kreckel RSDM
Glosik SM
Cation + anion
Thomas SM
H3O+ CH3+ NH4+
Douguet P
D3+
Dohnal P
Help!!! Theory for H3+ Recombination Badly Needed
Oka 2001
Kokooline, Greene, Esry, 2001, Nature, 412, 891
Kokooline, Greene, 2003, Phys. Rev. Lett. 90,
Kokooline, Greene, 2003, Phys. Rev. A68,
Jungen, Pratt, 2009, Phys. Rev. Lett. 102,
Jungen RSDM

8. Session 4, H3+ as best Probe for Cosmic Rays
H → H HD, OH
H+ + e- → H + hν
H2 → H H3+
H3+ + e- → H + H + H
ζ 7 × s-1
Spitzer Tomasko 1968
Dense cloud ζL = (0.32 – 1.50) × 102 cm s-1
3 × s-1
McCall et al. 1999, ApJ, 522, 338
Diffuse cloud ζL = (0.48 – 4.40) × 104 cm s-1
5 × s-1
Indriolo et al ApJ, 671,1736
Indriolo, McCall, 2012, ApJ, 745, 91
Galactic center ζL > (1.2 – 6.3) × 105 cm s-1
> 2 × s-1
Black RSDM Indriolo RSDM

9. Session 5, Galactic center
H3+ warm diffuse cloud
Oka et al. 2005, ApJ, 632, 882
Goto et al. 2008, ApJ, 688, 306
Geballe, Oka, 2010, ApJ, 709, L70
T ~ 250 K
n < 100 cm-3
Geballe RSDM Goto SM
Lis RSDM
H3O+ hot dense cloud
T ~ 700 K
n ~ 104 cm-3
Active Galactic Nucleus
Meijerink SM

10. Session 6, Interstellar Chemistry
Gerin RSDM
Schilke SM
H3+ R(1,1)l
H2O+ 111← 000
H2O+ 110← 101
Schilke et al. 2011, A&A, 521, L11
Geballe & Oka, 2010, ApJ, 709, L70
H2+
H3+
H3+ + HD → H2 + H2D K
H2D+ + HD → H2 + HD K
HD2+ + HD → H2 + D K H2
Van der Tak RSDM
Pagani RSDM H-
(H2-)
Robert, Herbst, Millar, 2003, ApJL 591, L41

11. Session 7, Planetary ionosphere
H3+ aurora
H3+ aurora
Stallard RSDM
Io, Volcano
Oka, Rev. Mod. Phys. 1992, 64, 1141

12. Other hydrogenic species
H2+ H3
Black RSDM
H3˗
Kokoouline SM
H5+
Prosmiti SM Valdes P
H7+
Prosmiti P
H4+ in solid Ne
Correnti P
H6+ in solid H2
Kumagai P