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0 1 32 54jina/Proceedings/Cowan/cowantalk.pdf · 60 80 100 120 140 160 180 200 220 MASS NUMBER...
Transcript of 0 1 32 54jina/Proceedings/Cowan/cowantalk.pdf · 60 80 100 120 140 160 180 200 220 MASS NUMBER...
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P. M
öller, J. R. N
ix, and K.-L
. Kratz/N
uclear Properties
56
− 2.5 − 2.0 − 1.5 − 1.0 − 0.5
0.0 0.5 1.0
log(Tβ /s)
FRDM (1992)
80
100 120
140
Mass Number A
r-Process abundance
160 180
200
10−2
10−1
100
101
0 20 40 60 80 100 120 140 160 Neutron Number N
0
20
40
60
80
100
120 P
roto
n N
umbe
r Z
Nr,
(Si
= 10
6)
Figure 16
60 80 100 120 140 160 180 200 220MASS NUMBER
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−1.00
−0.50
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2.00
2.50
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log
εSolar System Abundances
s−Process and r−Process
SS s−ProcessSS r−Process
Se Sr
Te
Xe
Ba
Eu
PbOs
PtAu
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Observed HST-STIS and synthetic (computed) spectra in the region surrounding the gold spectral line at a wavelength of2675.94 Angstroms. (One Angstrom = 1/100 millionth of a centimeter).
(Top) The observed spectrum of BD +17 3248, shown in blue, is compared to that of another old halo star in our Galaxyknown as HD 122563, shown in red. The atomic gold spectral line is seen in BD +17 3248, but not in HD 122563. Thisdetection could only be made using space telescopes such as the Hubble Space Telescope.
(Bottom) The observed BD +17 3248 spectrum, shown in blue dots, is compared to four synthetic spectra to determine theabundance of gold. The computed values, shown in order of increasing abundance of goldby dotted, short-dashed, solid,and long-dashed lines computed for these abundances are: log epsilon (Au) = -infinity, -0.80, -0.30, +0.2. The best fit isseen to be for log epsilon = -0.3, which indicates that gold in this star is less than a trillion times as abundant as hydrogen.
50 60 70 80 90ATOMIC NUMBER
−2.50
−2.00
−1.50
−1.00
−0.50
0.00
0.50
1.00
1.50
2.00
log
εr−Process Abundances in BD+17 3248
(Cowan et al. 2002)
Ground−Based DataSS r−Process AbundancesHST Data
Th U
Ba
La
Ce
Pr
Nd
Sm
Eu
Gd
Tb
Dy
Ho
Er
Tm
Os Pt
Ir
Au
Pb
50 60 70 80 90Atomic Number
−6.50
−5.50
−4.50
−3.50
−2.50
−1.50
−0.50
0.50
Rel
ativ
e lo
g ε
r−Process Abundances in Halo Stars
HD 115444CS 22892−052SS r−Process AbundancesBD +173248
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0.00
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1.00
1.50
2.00
log
εr−Process Abundances in BD+17 3248
Ground−Based DataModel SS r−AbundancesHST DataSS r−process Abundances
Ba
Th
Nd
Pt
Pb
Ag
Pr
Y
Sr
ZrOs
Ir
Tb
La
Er
Eu
Ho
Tm
Nb
Pd
Ge
U
Ce
Gd
Dy
Au
Sm
30 40 50 60 70 80 90ATOMIC NUMBER
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−2.00
−1.50
−1.00
−0.50
0.00
0.50
1.00
log
ε
Stellar DataSS r−Process AbundancesSS s−Process Abundances U
Th
Pb
Os
Pt
Ce
Nd
Sm
Dy
La
Ba
Pr Eu
Tb
Sr
Y
Zr
Ru
Nb
MoAg
Pd
Ho
Tm
Hf
Yb
ErGd
Ge
CdGa
Au
Ir
Lu
Rh
Sn
NEW DETECTIONS OF NEUTRON-CAPTURE ELEMENTS IN
CS 22892–052, HD 115444 & BD +17 3248
• Elements with atomic number Z = 40-50,including niobium, ruthenium, rhodium, pal-ladium, silver and cadmium have been de-tected now in CS 22892–052, HD 115444 andBD +17◦3248.
A SECOND R-PROCESS?
• Abundances of the neutron-capture ele-ments Z ≥ 56 (i.e. Ba and above) are con-sistent with the scaled solar system r-processcurve (blue line) indicating that the rela-tive elemental r-process abundances have notchanged over the history of the Galaxy andfurther suggests that there is one r-processsite in the Galaxy, at least for elements Z ≥56. Robust.• Abundances of the newly determined ele-ments from Z=40-50 in general fall below thescaled solar system r-process curve. Thesedata seem to support the suggestion (Wasser-burg, Busso & Gallino 1996, Wasserburg &Qian 2000) that there may be two r-processsites, with one responsible for the heavier ele-ments (occurring on a more rapid time-scale)and a less frequently occurring synthesis pro-ducing the elements below Ba.
• Strong and a Weak r-Process?
• Alternative explanations: one supernovasite with two different epochs in the explo-sion/ejection process or different regions ofthe same neutron-rich jet of a core-collapsesupernova (Sneden et al. 2000; Cameron2001).
−4 −3 −2 −1 0 1[Fe/H]
−1.00
−0.50
0.00
0.50
1.00
1.50
2.00
2.50
[Eu/
Fe]
ABUNDANCE SCATTER IN THE GALAXY
−2 −1 0 1 2[Ba/Fe]
−2
−1
0
1
2
[Sr/
Ba]
r−process poorBurris et al.McWilliam et al.r−process rich
100% r−process
Radioactive-Decay Age Estimates
The measured abundance of Th presents the op-
portunity to determine the age of CS 22892–052, by
use of the known Th half-life (14.05 Gyr):
NTh(t) = NTh(t0)exp(−t/τTh)
Where
τTh =14.05
ln2= 20.27Gyr
=⇒ Solar System Th/Eu (at formation) = 0.463
=⇒ Solar System Th/Eu (today) = 0.344
=⇒ Observed Th/Eu in CS 22892-052 = 0.219
It is important to note, that since the solar-
system Th/r ratio is larger than the observed ratio
in CS 22892–052 then CS 22892–052 must be older
than the solar system r-process material.
30 40 50 60 70 80 90ATOMIC NUMBER
−2.50
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log
ε
r−Process Abundances in CS 22892−052
Stellar DataSS r−Process Abundancesr−Process Theory U
Th
Pb
Os
Pt
Ce
Nd
Sm
Dy
La
Ba
Pr EuTb
Sr
Y
Zr
Ru
Nb
Mo Ag
Pd
Ho
Tm
Hf
Yb
ErGd
Ge
CdGa
Au
Ir
Lu
Rh
Sn
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