Physics, Chemistry and Astronomy of H 3 + Royal Society Discussion Meetin And the Satellite Meeting January 16-18, 2006
Dec 21, 2015
Physics, Chemistry and Astronomy of
H3+
Royal Society Discussion MeetingAnd the Satellite Meeting
January 16-18, 2006
Theoretical Spectroscopy
Rigorous calculation
Triplet excited state
Asymptotic vibrational states
Sub-microhartree PES
Hyperspherical coordinate1975 H2
Laboratory spectroscopy
Near-infrared to visible, above the barrier
Action spectroscopy
H2D+, HD2+, D3
+
Ultra-cold H2+, H3
+ and isotopomers mK Spectroscopy using quantum logic
25 vibrational bands
13676 cm-1
Dissociative recombination
Rotationally cooled H3+
CRYRING, TSR
Theoretical calculation
Full dimentional calculationJahn-Teller effect
Surprise in diffuse cloud
Same column density in dense and diffuse clouds
N(H3+)dense ~ 3.6 ×1012 cm-2 AV
N(H3+)diffuse ~ 4.4 ×1013 cm-2 AV
Ntotal(H3+)diffuse≈ 100 Ntotal(H3
+)dense
ζdiffuse≈ 10ζdense
Grain neutralization and cosmic ray ionization
The Galactic center
The Central Molecular Zone (CMZ)The treasure house of H3
+
Discovery of metastable H3
+
Revelation of warm and diffuse gas
Cold30 K>104 cm-3
Hot104 K~102 cm-3
Ultrahot107-8 K~0.3 cm-3
Warm250 K~102 cm-3
metastable
Deuterium fractionation
Destroyers of H3+: CO, O……
HD
N(H2) =1.5 ×106 cm-3 T = 10 K
n(H2D+) ≤ n(HD2+) « n(D3
+)
HD2+ in prestellar core
H2D+ in protoplanetary disks
Planetary ionospheres
Powerful probe of plasmas in planetaryIonosphere from ground based observatories
Active driver of thermosphere and ionosphere
H3+ thermostat effect
Ion-neutral coupling