![]() | Annu. Rev. Astron. Astrophys. 1994. 32:
153-90 Copyright © 1994 by Annual Reviews. All rights reserved |
3.2. The Secondary r-Process
A system that does not achieve equilibrium may also produce r-process
elements. As we have seen, as the bulk of the nuclei strive to reach
the iron group, the reactions that carry them in this direction may
release neutrons that then capture on pre-existing seed nuclei. If the
number of neutrons released is sufficiently large, a solar system
r-process abundance distribution may result. The nuclear reactions
that would be the dominant producers of neutrons are
(, n)
reactions, and in particular the reactions
13C(
,
n)16O,22Ne(
, n)25Mg,
and 25Mg(
,
n)28Si.
A crucial feature of a secondary r-process is that it does not achieve
(n,)
- (
,
n) equilibrium. Such equilibrium occurs
when the flows from (n,
) and
(
,
n) reactions come into balance. The most
abundant isotope of some element in such equilibrium is then the one
for which the rate for that isotope (Z, A) to capture a
neutron is equal to the rate for the resultant isotope
(Z, A + 1) to suffer a disintegration
(
,
n) reaction. The neutron-separation energy
Sn, that
is, the binding energy of the least tightly bound neutron, of this
nucleus is, upon neglect of the A dependence of nuclear partition
functions (e.g.
Sato 1974, see also
Howard et al 1993,
and Meyer 1994),
![]() | (5) |
where nn is the neutron number density in units of
cm-3. In secondary
r-process sites, the neutron number density is typically ~ 1019
cm-3
and T9 ~ 1; thus, the dominant nuclei in
(n, )
- (
,
n) equilibrium have
Sn
3.0 MeV. Figure 8 shows the neutron-separation
energies for the isotopes of neodymium (Z = 60). We see that the
dominant isotope in
(n,
)
- (
,
n) equilibrium should be the one with neutron number
N
110. The
most neutron-rich beta-stable isotope of neodymium is 150Nd
(N = 90). The neutron sources in a secondary r-process would have to
supply and maintain some 20 neutrons per seed nucleus in order to
establish (n,
)
- (
,
n) equilibrium. This is something they cannot do.
![]() |
Figure 8. Neutron-separation energies for the isotopes of neodymium. The data are derived from Möller & Nix (1988). |
Let us now consider possible secondary r-process sites. One possible
site is the helium shell of an exploding massive star
(Truran et al 1978,
Thielemann et al 1979;
see also
Cowan et al 1980,
1983,
1985;
Blake et al 1981;
Klapdor et al 1981).
As the supernova shock wave
traverses this shell, it heats up the material to a temperature
T9
1. Although this temperature is not high enough to force the
material into NSE, it is high enough to drive material strongly in that
direction. Among the main nuclear reactions that occur are
(
, n)
reactions that liberate neutrons which can then capture on the
pre-existing seed nuclei.
Truran et al (1978)
found that neutron
captures could modify an s-process seed abundance distribution into an
r-process distribution. Later work indicated that a seed distribution
that is enhanced with respect to the solar system heavy-element
distribution is required to produce the solar r-nuclei. Such an
enhanced distribution could result from s-processing prior to shock
passage if protons were to mix down into the helium shell to make
13C
from the abundant 12C [via 12C(p,
)
13N(
+)13C].It is apparent today,
however, that the amount of 13C required is unrealistically large
(Cowan et al 1985,
Cameron et al 1985).
Lee et al (1979)
considered supernova shock passage through the carbon shell. Here the
22Ne(,
)25Mg reaction produces the
neutrons. 25Mg is also a neutron poison, however; it absorbs
many of the liberated neutrons before they have a chance to capture on
heavier seed nuclei.
Wefel et al (1981)
found that some heavy nuclei could be
synthesized, but not the bulk of the r-nuclei.
Another intriguing secondary site is again the helium burning shell, but now the effects of neutrino inelastic scattering on 4He nuclei are included. The neutrinos come from the cooling nascent neutron star resulting from the core-collapse event. These neutrinos spall neutrons from the 4He (and other light) nuclei. The neutrons can then capture on the seed nuclei and drive an r-process (Epstein et al 1988). A detailed study of this "v-process" showed that some interesting nucleosynthesis may occur in such an event, but it could not have been a major contributor to the solar system r-process abundances (Woosley et al 1990).
All of the secondary r-process models studied to date have had profound difficulties which have rendered them implausible. Moreover, as shown in the next section, there are other reasons for favoring a primary over a secondary r-process. Nevertheless, the study of secondary r-process models has been valuable because they may have important applications to isotopic anomalies in meteorites (e.g. Clayton 1989, Howard et al 1992, Cameron et al 1993).