-
2
-
-
34547323848
-
-
R. S. Lewis, M. Tang, J. F. Wacker, E. Anders, E. Steel, ibid. 326, 160 (1987).
-
(1987)
Nature
, vol.326
, pp. 160
-
-
Lewis, R.S.1
Tang, M.2
Wacker, J.F.3
Anders, E.4
Steel, E.5
-
5
-
-
0025207083
-
-
S. Amari, E. Anders, A. Virag, E. Zinner, Nature 345, 238 (1990).
-
(1990)
Nature
, vol.345
, pp. 238
-
-
Amari, S.1
Anders, E.2
Virag, A.3
Zinner, E.4
-
7
-
-
0028562260
-
-
L. R. Nittler, C. M. O. Alexander, X. Gao, R. M. Walker, E. K. Zinner, Nature 370, 443 (1994).
-
(1994)
Nature
, vol.370
, pp. 443
-
-
Nittler, L.R.1
Alexander, C.M.O.2
Gao, X.3
Walker, R.M.4
Zinner, E.K.5
-
11
-
-
11944268259
-
-
D. D. Clayton, B. S. Meyer, C. I. Sanderson, S. S. Russell, C. T. Pillinger, Astrophys. J. 447, 894 (1995).
-
(1995)
Astrophys. J.
, vol.447
, pp. 894
-
-
Clayton, D.D.1
Meyer, B.S.2
Sanderson, C.I.3
Russell, S.S.4
Pillinger, C.T.5
-
14
-
-
0026274326
-
-
_, Science 254, 1188 (1991).
-
(1991)
Science
, vol.254
, pp. 1188
-
-
-
17
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3543018006
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note
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For TEM we used a Philips Biotwin instrument operated at 120 kV and a Topcon EM-002B operated at 200 kV.
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-
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19
-
-
0030427120
-
-
T. L. Daulton, D. D. Eisenhour, T. J. Bernatowicz, R. S. Lewis, P. R. Buseck, Geochim. Cosmochim. Acta 60, 4853 (1996).
-
(1996)
Geochim. Cosmochim. Acta
, vol.60
, pp. 4853
-
-
Daulton, T.L.1
Eisenhour, D.D.2
Bernatowicz, T.J.3
Lewis, R.S.4
Buseck, P.R.5
-
21
-
-
0009666457
-
-
I. P. Wright, S. R. Boyd, I. A. Franchi, C. T. Pillinger, J. Phys. E 21, 865 (1988).
-
(1988)
J. Phys. E
, vol.21
, pp. 865
-
-
Wright, I.P.1
Boyd, S.R.2
Franchi, I.A.3
Pillinger, C.T.4
-
22
-
-
0000741086
-
-
A. B. Verchovsky, A. V. Fisenko, L. F. Semjonova, C. T. Pillinger, Meteoritics Planet. Sci. 32, A131 (1997).
-
(1997)
Meteoritics Planet. Sci.
, vol.32
-
-
Verchovsky, A.B.1
Fisenko, A.V.2
Semjonova, L.F.3
Pillinger, C.T.4
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23
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3543006650
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note
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13C = -32.7 per mil), also has considerably higher total and lower pyrolysis carbon yields. Apart from that, these data are also in agreement with ED-9 being the coarsest fraction.
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24
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0032504272
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D. A. Shelkov, A. B. Verchovsky, H. J. Milledge, C. T. Pillinger, Chem. Geol. 149, 109 (1998).
-
(1998)
Chem. Geol.
, vol.149
, pp. 109
-
-
Shelkov, D.A.1
Verchovsky, A.B.2
Milledge, H.J.3
Pillinger, C.T.4
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25
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3543010275
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note
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When considering N and noble gas abundances released by stepped combustion, it is necessary to normalize the yields of these species to the overall C content of each sample. This has been done for each step of the four extractions, and the results are presented as element-to-C ratios versus proportion of total C removed (Fig. 3).
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26
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3542996950
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We cannot exclude the possibility that the primary ion energies could be modified because of ion collisions with dust particles and gas, present along with diamonds in the place where implantation has occurred, making the ion energies just enough to stop within diamond grains.
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27
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3543045660
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36Ar ratios decrease with increasing grain size). This is clearly not compatible with preferential noble gas losses from smaller grains (as may accompany postformational heating, for instance) but is in agreement with an implantation mechanism at which small, light ions have a shorter projected range (31).
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29
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3543012658
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14N would be required at the same time, and that is not predicted in any of the supernova shells (32).
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33
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3543046245
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note
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Supported by the Particle Physics and Astronomy Research Council and by Russian Foundation of Basic Science grant 96-05-64546 (A.V.F. and L.F.S.). We thank J. Findlay and J. R. Fryer for assistance with TEM.
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