In. Tolstikhin et B. Marty, THE EVOLUTION OF TERRESTRIAL VOLATILES - A VIEW FROM HELIUM, NEON, ARGON AND NITROGEN ISOTOPE MODELING, Chemical geology, 147(1-2), 1998, pp. 27-52
In this contribution, we have developed an evolutionary model in order
to identify and quantify processes which were able to reproduce rare
gas and nitrogen isotopic abundances in the main terrestrial reservoir
s. The following processes appear to have played an important role in
the history of terrestrial volatiles. During accretion, impact degassi
ng could have released approximate to 95% of the initial rare gas abun
dances, which were quite similar to those typical of solar wind-implan
ted gases. After the major phase of accretion and core segregation (4.
50 Ga ago), some parts of the upper mantle were partially melted by gi
ant impact(s) and experienced vigorous convection and solubility-contr
olled degassing. More than 99% of the volatile species initially prese
nted in the upper mantle-atmosphere reservoirs were lost during this p
eriod (from 4.50 to 4.30 Ga ago). This loss was accompanied by element
al and isotopic fractionation of residual atmospheric constituents. Th
e atmosphere became retentive for Xe at 4.40 Ga but degassing, loss an
d fractionation of lighter rare gases and nitrogen might have taken pl
ace some time afterwards. Therefore each gas might have undergone frac
tionation to various extent at different times. After closure of the a
tmosphere (at approximate to 4.30 Ga) for all but the lightest (H, He)
constituents, the lower mantle supplied the upper mantle with minute
amounts of parent incompatible elements, rare gases and nitrogen, betw
een similar to 1% (4.3 Ga ago) and similar to 0.2% (at present) of the
ir total amount in the lower mantle per Ga. The post-atmosphere closur
e flux of Liquid silicates from the upper mantle, analogue to the pres
ent-day MOR flux of basaltic melts, decreased by a factor of similar t
o 100, from similar to 5.10(18) (4.3 Ga ago) to 6.10(16) g a(-1) (at p
resent). The ratio of Ar-36(now)/Ar-36(4.3 Ga)(um) similar to 10(-4) i
llustrates the total degree of upper mantle degassing yielded by this
flux. This rate of degassing corresponds to a present-day ratio of Ar-
40/Ar-36(um) > 10(6), if no fluxes from the lower mantle and the crust
al-atmospheric reservoirs had operated, and the ratios of radiogenic o
ver primordial species could have been higher in the past than those a
t present. The model postulates that nitrogen trapped in the Earth-Atm
osphere system was initially depleted in N-15 relative to present-day
atmospheric composition (ATM). Atmospheric escape enriched the ancient
atmosphere in N-15, resulting in a delta(15)N isotopic composition of
+2.5 parts per mil (ATM) 4 Ga ago. Subsequent degassing of mantle nit
rogen allowed this element to reach its present-day composition in air
. Because the upper mantle is extremely depleted in volatile elements,
their transfer from the lower mantle is sufficient to maintain primor
dial rare gases and nitrogen abundances in the upper mantle approximat
ely at a steady state. Decays of parent radioactive elements, U-um, Th
-um, and K-um,, contribute radiogenic nuclides. Recycling fluxes of (s
ub)surface materials into the upper mantle transfer surface volatiles,
similar to 6% of surface-derived (atmosphere + sediments) N and simil
ar to 0.03% of atmospheric Ar-36(ah), per Ga. Consequently, the isotop
ic composition of mantle nitrogen varied from its initial delta(15)N v
alue of - 30 parts per mil to its present-day upper mantle value of -5
parts per mil. The consequence of nitrogen recycling in the Earth-Atm
osphere system is therefore partial re-homogenisation of N-isotopes, b
ut this process was not efficient enough to have erased early heteroge
neity. Thus the present contribution proposes early formation of the E
arth's atmosphere by a combination of degassing, dissipation, and frac
tionation processes. Primordial rare gases and nitrogen were set in th
is reservoir around 4.3 Ga ago and further mantle outgassing has contr
ibuted less than 3% of these species since that time. (C) 1998 Elsevie
r Science B.V. All rights reserved.