The ratio of cosmic ray source abundance to solar-system abundance was examined for individual elements. Correlations of these ratios with first-ionization potential (FIP) and the expected mass-to-charge ratio (A/Q) of the elements in a million-degree plasma are analyzed. The FIP correlation was examined and it is shown that the correlation is affected by the choice of C2 or C1 chondritic meteorites as the solar-system standard for comparison. An A/Q correlation is suggested as a consequence of the shock acceleration model in the hot interstellar medium. The correlations are presented

Binns, W. R.

Garrard, T. L.

Israel, M. H.

Klarmann, J.

Margolis, S. H.

Stone, E. C.

Waddington, C. J.

Caltech Authors - Main

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OG 7. 1-4 
IMPLICATIONS OF SOURCE ABUNDANCES OF ULTRAHEAVY COSMIC RAYS 
W.R. Binnsa, T. L. Garrardb, M. H. Israel 6 , J. Klarmann 6 , 
S. H. Margolisa, E. C. Stoneb, C. J. Waddingtonc, 
6 Washington University, St. Louis, MO, USA 
bCalifornia Institute of Technology, Pasadena, CA, USA 
cUniversity of Minnesota, Minneapolis, MN, USA 
1. Introduction. In this paper we will examine the ratio of cosmic-ray source 
abundance to solar-system abundance for individual elements. In particular we will 
look at correlations of these ratios with first-ionization potential (FIP) and also with 
the expected mass-to-charge ratio (A/Q) of the elements in a million-degree plasma. 
We have previously examined the FIP correlation and shown that the correlation is 
affected by the choice of C2 or Cl chondritic meteorites as the solar-system standard 
for comparison (Binns, et al., 1984). An A/Q correlation was suggested by Eichler and 
_lf~i_l!_~b~~h_j1_9~1), as a consequenc~ of their model of shock acceleration in the hot 
interstellar medium,- andhasmbe-en examTned-oy1sraellHJ8SJ,-1nese-co-rn~tat1ons a-re-
presented in the following four figures. 
2. Explanation of Figures. Figure 1 plots the ratio of cosmic-ray source to solar-
system abundances, normalized to unity for Fe, as a function of the first ionization 
potential. Error bars indicate the quadratic sum of the error on the solar-system 
abundance and that on the cosmic-ray source abundance. The element symbols for 
the various points have been transferred directly below the point. 
Cosmic-ray source abundances in all four figures are derived principally from 
observations on HEA0-3, except for H and He which come from balloon observations 
(Webber, 1982; Webber and Lezniak, 1974). Two H points are plotted; H(R) uses H 
abundances at the same rigidity as the other elements; H(E), at the same energy per 
nucleon. For 6 ~ Z < 27, and for Z = 29 and 31 (Cu and Ga), the results are from the 
Danish-French experiment on HEA0-3 (Lund, 1984). For Z = 28 and 30 (Ni and Zn) 
and for Z > 32 the results are from the Heavy Nuclei Experiment (Israel, et al., 1983). 
In each case experimental results were propagated back to the source. in a standard 
leaky-box model. 
In figures 1 and 3 the solar system abundances are from Anders and Ebihara 
(1982). These abundances are mainly from type Cl meteorites; except H, C, N, and 0 
are from photospheric measurements, He is from the solar wind H/He ratio, Ne is from 
the solar wind Ne/Ar ratio and from astronomical measurements of extra-solar-system 
nebulae, and Ar, Kr, and Xe are interpolated from nearby elements. In figures 2 and 4 
the Cl meteorite abundances are replaced by C2 meteorite abundances (Mason, 1979) 
in forming the solar-system values. 
Figures 3 and 4 have the same ordinates as figures 1 and 2 respectively, but the 
abscissa is A/Q120, where A is the atomic weight and Q120 is the charge state the 
element would have after removal of all electrons whose ionization potential is less 
than 120eV. Thus the abscissa is an estimate of the mass-to-charge ratio which the 
element would have in a million-degree interstellar gas. (The value 120 eV corresponds 
to a temperature of 1.4 x 106 K, but the correlation displayed here is insensitive to the 
precise value of ionization potential selected.) 
The implications of these figures will be discussed at the conference. 
© NASA/STI • Provided by the NASA Astrophysics Data System 
1985ICRC....3...13B
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3. References. 
Anders, E. and M. Ebihara, 1982, Geochim. Cosmochim. Acta, ,6,, 2363. 
Binns, et al., 1984, Adv. Space Rea. '' (no. 2-3), 225. 
Eichler, D. and K. Hainebach, 1981, Phya. Rev. Lett. 47, 1560. 
Israel, M.H., 1985, 1eth Tezaa Symp. Relativistic Aatrophya., in press. 
Israel, et al., 1983, 18th ICRC, 9, 305. 
Lund, N., 1984, Adv. Space Rea. ,, (no. 2-3), 5. 
Mason, B., 1979, Geol. Survey Prof. Paper 44~8-l. 
Webber, W.R., 1982, Ap. J., f55,, 329. 
Webber, W.R. and J.A. Lezniak, 1974, Ap. Space Sci., 90,, 361. 
OG 7.1-4 
© NASA/STI • Provided by the NASA Astrophysics Data System 


Implications of Source Abundances of Ultraheavy Cosmic Rays

NASA Technical Reports Server

13
OG 7. 1-4
IMPLICATIONS OF SOURCE ABUNDANCES OF ULTRAHEAVY COSMIC RAYS
W. R. Binns a, T. L. Garrard b, M. H. Israel a, J. Klarmann a,
S. H. Margolis a, E. C. Stone b, C. J. Waddington c,
aWashington University, St. Louis, MO, USA
bCalifornia Institute of Technology, Pasadena, CA, USA
¢University of Minnesota, Minneapolis, MN, USA
1. Introduction. In this paper we will examine the ratio of cosmic-ray source
abundance to solar-system abundance for individual elements. In particular we will
look at correlations of these ratios with first-ionization potential (FIP) and also with
the expected mass-to-charge ratio (A/Q) of the elements in a million-degree plasma.
We have previously examined the FIP correlation and shown that the correlation is
affected by the choice of C2 or CI chondritic meteorites as the solar-system standard
for comparison (Binns, et al., 1984). An A/Q correlation was suggested by Eichler and
Hainebach (1981), as a consequence of their model of shock acceleration in the hot
interstellar medium, and has been examined by Israel (1985). These correlations are
presented in the following four figures.
2. Explanation of Figures. Figure 1 plots the ratio of cosmic-ray source to solar-
system abundances, normalized to unity for Fe, as a function of the first ionization
potential. Error bars indicate the quadratic sum of the error on the solar-system
abundance and that on the cosmic-ray source abundance. The element symbols for
the various points have been transferred directly below the point.
Cosmic-ray source abundances in all four figures are derived principally from
observations on HEAD-3, except for H and He which come from balloon observations
(Webber, 1982; Webber and Lezniak, 1974). Two H points are plotted; H(R) uses H
abundances at the same rigidity as the other elements; H(E), at the same energy per
nucleon. For6< Z < 27, and for Z =29and 31 (Cu and Ga), the results are from the
Danish-French experiment on HEAO-3 (Lund, 1984). For Z = 28 and 30 (Ni and Zn)
and for Z > 32 the results are from the Heavy Nuclei Experiment (Israel, et al., 1983).
In each case experimental results were propagated back to the source, in a standard
leaky-box model.
In figures 1 and 3 the solar system abundances are from Anders and Ebihara
(1982). These abundances are mainly from type C1 meteorites; except H, C, N, and O
are from photospheric measurements, He is from the solar wind H/He ratio, Ne is from
• the solar wind Ne/Ar ratio and from astronomical measurements of extra-solar-system
nebulae, and Ar, Kr, and Xe are interpolated from nearby elements. In figures 2 and 4
the C1 meteorite abundances are replaced by C2 meteorite abundances (Mason, 1979)
in forming the solar-system values.
Figures 3 and 4 have the same ordinates as figures 1 and 2 respectively, but the
abscissa is A/QI20, where A is the atomic weight and QI20 is the charge state the
element would have after removal of all electrons whose ionization potential is less
than 120eV. Thus the abscissa is an estimate of the mass-to-charge ratio which the
element would have in a million-degree interstellar gas. (The value 120 eV corresponds
to a temperature of 1.4 × 108 K, but the correlation displayed here is insensitive to the
precise value of ionization potential selected.)
The implications of these figures will be discussed at the conference.
https://ntrs.nasa.gov/search.jsp?R=19850026553 2020-03-20T16:59:34+00:00Z
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FIRST IONIZATION POTENTIAL (eV) FIRST IONIZATION POTENTIAL (eV) ..j
Figure 1 Figure 2
_v=.,-, , , , , , , .... 5.0 , , , , , ,' , , , , ,
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MASS/CHARGEAT kT~ 120eV (A/Q,zo) MASS/CHARGEAT kT~ 120eV (A/Q_zo)
c)
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Figure 3 Figure 4 .,4
!
OG 7.I-4
16
3. References.
Anders, E. and M. Ebihara, 1982, Geochim. Cosmochim. Acta, 46, 2363.
Binns, et al., 1984, Adv. Space Res. 4, (no. 2-3), 225.
Eichler, D. and K. Hainebach, 1981, Phys. Rev. Left. 47, 1560.
Israel, M.tt., 1985, l'2th Texas Syrup. Relativistic Astrophys., in press.
Israel, et al., 1983, 18th ICRC, 9, 305.
Lund, N., 1984, Adv. Space Res. 4, (no. 2-3), 5.
Mason, B., 1979, Geol. Survey Prof. Paper 440-[3-1.
Webber, W.R., 1982, Ap. J., 255, 329.
Webber, W.R. and J.A. Lezniak, 1974, Ap. Space Sci., 80, 361.


English

Implications of source abundances of ultraheavy cosmic rays

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Implications of Source Abundances of Ultraheavy Cosmic Rays

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