some chemistry in assorted star-forming regions
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Some Chemistry in Assorted Star-forming Regions
Eric Herbst
Some Regions Associated with Star-Formation
pre-stellar cores (L1544)
low mass protostars (IRAS 16293) protoplanetary disks Hot cores PDR’s
A pre-stellar core (cold but with a dense center)
H2D+ - detected by Caselli et al. (2003)
D/H =
1.5 x 10-5
“H2D+ is the main molecular ion in the central..”
L1544 – a prestellar coreCCS – gray scale
Dust emission peak
The model:
multiply deuterated species are now observed in the ISM
observations support the link between high fractionation and CO depletion
we present a pseudo-time-dependent model of deuterium chemistry, including all analogues of H3
+, NH3, CH3OH HD2
+ and D3+ may be important even in
modeling singly deuterated species
Fractionation in the gas-phase….
H3+
CO, N2, O
HCO+
N2H+
OH+
H2D+e-
HD
DCO+, HCO+
N2D+, N2H+
OD+, OH+
CO, N2, O
e-
H2
H H HH2 H
H H D
HD H
H2 D
When species are depleted….
H3+
CO, N2, O
HCO+
N2H+
OH+
H2D+e- HD
DCO+, HCO+
N2D+, N2H+
OD+, OH+
CO, N2, O
e-
H2
H H HH2 H
H H D
HD H
H2 D
At higher densities….
H3+
CO, N2, O
HCO+
N2H+
OH+
H2D+e- HD
DCO+, HCO+
N2D+, N2H+
OD+, OH+
CO, N2, O
e-
H2
H H HH2 H
H H D
HD H
H2 D
Accretion model without HD2+
and D3+:
n(H2) 104 (cm-3) 106 (cm-3)
H2D+/H3+ 0.938 27.37
DCO+/HCO+ 0.217 0.492
N2D+/N2H+ 0.215 0.484
D/H 0.075 0.355
NH2D/NH3 0.313 1.208
HDCO/H2CO 0.133 0.381
Times of peak D/H ratios: 10(6) yr and 2 x 10(4) yr
Deuterium fractionation:
H3+ + HD H2D+ + H2
H2D+ + CO HCO+ + HD 2/3
DCO+ + H2 1/3
• Maximum DCO+/HCO+ ratio is 0.5
Deuterium fractionation:
H2D+ + HD HD2+ + H2
HD2+ + CO HCO+ + D2 1/3
DCO+ + HD 2/3
• DCO+/HCO+ ratio reflects the total degree of deuteration of H3
+
HD2+ + HD D3
+ + H2
D3+ + CO DCO+ + D2 1
Fractional abundances:
Molecular D/H ratios:
A comparison of the homogeneous model with observations of CO and D2CO:observations
model
(Observations from Bacmann et al. 2002; 2003)
Heterogeneous shell model does much better!
Fractionation on Grains
One of the strongest predictions of the pre-stellar core model is that the abundance ratio of D to H atoms in the gas becomes quite high (0.1 – 1.0). In reality, these atoms strike dust particles and react to form both normal and deuterated species!! These species stay on the grains until star formation begins to occur and temperatures rise!
Accretion and Diffusion
DUST
HD
CO
Surface reactions produce
the following molecules:
H2CO, HDCO, D2COCH3OH, CH3OD
CH2DOH, CHD2OH
CH2DOD, CHD2OD
CD3OH, CD3OD
O
H2O, HDO, D2O, CO2, H2, HD, D2
The Protostar IRAS 16293-2422 Temperatures have warmed up to near 100 K
close to the budding star and 50 K somewhat farther removed. The following methanol isotopomers have been detected:
CH3OH, CH3OD, CH2DOH, CHD2OH, CD3OH in addition to HDCO and D2CO.
The belief is that these species have very recently come off grains.
Dust continuum – IRAS 16293
Methanol fractionation from a grain surface chemistry model:
Abundance CH3OH 1 x 10-7
Fractionation CH3OD 0.22
CH2DOH 0.8
CH2DOD 0.16
CHD2OH 0.2
CHD2OD 0.048
CD3OH 0.02
CD3OD 0.004Accreting D/H ratio = 0.4 (Stantcheva & Herbst 2003)
IRAS
0.04
0.9
0.2
0.03
Methanol fractionation from a protostellar model. T=50 K; n(H2)=106cm-3
What happens as the evaporated material ages?
After methanol desorbs from the grains:
CH3OD
CH2DOH
CH3ODH+
CH2DOHH+
CH3OD
CH3OH
CH2DOHH3
+e-
e-
H3+
e-
Osamura et al. 2004
Compared with the observations:
Observations of IRAS 16293-2422 from Parise et al. 2002; 2003
HOT MOLECULAR CORES
Hot cores are regions of warm, quiescent gas near high-mass star-forming regions. Temperatures are 100-300 K and densities are typically 107 K. They are associated with a variety of saturated gas-phase organic molecules: methanol, ethanol, acetaldehyde, methyl formate, acetic acid, glycolaldehyde, ethylene oxide, dimethyl ether, and possibly diethyl ether, glycine, and ethylmethyl ether.
OMC: KL
HOT CORES
HOT MOLECULAR CORES II As in protostellar sources, the chemistry is
associated with evaporation from the dust, although the post-evaporation gas-phase chemistry may be crucial in producing larger species from the precursor methanol.
Key reactions in chain to form methyl formate:
HHCOOCHeOCHHHCO
HOCHHHCOCOHOHCH
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23223
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)(
Ab Initio Calculations
TWO EXPERIMENTS
1) SIFT AT HANSCOM AF BASE dominant product cluster ion (high density) 2) ICR AT WATERLOO, CANADA dominant product CH3OCH2
+ (low density) CONCLUSION: no major channel to produce
protonated methyl formate We don’t know how it is made in hot cores.
There is work left for you to do!!!!!
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