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Isotope fractionation in the photochemical escape of O from Mars
The production of energetic and escaping neutral O atoms at the current epoch in the martian thermosphere is thought to be dominated by the O 2 + dissociative recombination process: O 2 + + e → O ∗ + O ∗ + Δ E In this equation, O ∗ represents a fast O atom and Δ E is the energy released. There are f...
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| Published in: | Icarus (New York, N.Y. 1962) N.Y. 1962), 2010-07, Vol.208 (1), p.176-191 |
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| Main Authors: | , |
| Format: | Article |
| Language: | English |
| Subjects: | |
| Citations: | Items that this one cites Items that cite this one |
| Online Access: | Get full text |
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| Summary: | The production of energetic and escaping neutral O atoms at the current epoch in the martian thermosphere is thought to be dominated by the
O
2
+
dissociative recombination process:
O
2
+
+
e
→
O
∗
+
O
∗
+
Δ
E
In this equation,
O
∗
represents a fast O atom and
Δ
E
is the energy released. There are five energetically allowed channels of this reaction, with exothermicities, and thus O kinetic energies, that depend on the electronic energies of the O atoms produced, on the vibrational and rotational states of the initial
O
2
+
ions, and on the ion and electron velocities. We have recently reported the escape probabilities and rates for
16
O
produced in dissociative recombination of
16
O
16
O
+
for 60° solar zenith angle low and high solar activity models of the martian thermosphere/ionosphere (Fox, J.L., Hać, A. [2009]. Icarus 204, 527–544). Because the isotope ratios of atmospheric species, including
18
O
/
16
O
, contain information about the evolution of the atmosphere, we investigate here the probabilities for escape of energetic
18
O
produced in dissociative recombination of the isotopomer
18
O
16
O
+
. We first predict the altitude dependent vibrational distribution of
18
O
16
O
+
(
v
)
, and we compute the nascent energy distributions of the fast
18
O
atoms as functions of vibrational excitation, of the electron and ion temperatures, and of the rotational distributions of the ions; we compare these energy distributions to those of
16
O
produced in DR of
16
O
16
O
+
(
v
)
. We then use a 1-D spherical Monte Carlo code to determine escape probabilities for
18
O
as functions of energy and altitude. In this code, energetic atoms are followed in spherical geometry from their altitude of production from one collision to the next through the background atmosphere until their energies fall below the escape energy, or they reach an altitude of 700
km with energies above the escape energy. We convolve these escape probabilities with the nascent energy distributions to determine the probabilities of escape of
18
O
produced in DR of
18
O
16
O
+
. We find that there is a substantial altitude dependent isotope effect, which operates in addition to the effects of diffusive separation of the neutral species from which the
O
2
+
ions are created. |
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| ISSN: | 0019-1035 1090-2643 |
| DOI: | 10.1016/j.icarus.2010.01.019 |