A&A 463, 261-264 (2007)
DOI: 10.1051/0004-6361:20065689
M. Q. Liu - J. Zhang - Z. Q. Luo
Institute of Theoretical Physics, China West Normal University, Nanchong 637002, PR China
Received 25 May 2006 / Accepted 12 October 2006
Abstract
Aims. With the new electron capture results from the improved GT resonance distribution, we analyzed the electron screening effect on electron capture at the presupernova stage.
Methods. The relativistically degenerate electron liquid screening potential derived from the linear response theory are adopted. The calculation of the electron capture rates is based on the shell-model. Both the change of electron energy and the shift in the threshold for electron capture in screening are taken into account.
Results. The results indicate that the influence of electron screening on the electron capture is prominent in high-density matter. As the improved electron capture rate is considered, screening effect on the electron capture rate increases by about 1 percent at
g/cm3.
Conclusions. The influence of screening on the electron capture reaction is about 10 percent for 56Co at
g/cm3. Screening may affect the structure and evolution of presupernova and should be included in any precise simulation.
Key words: supernovae: general - nuclear reactions, nucleosynthesis, abundances - methods: numerical
The electron capture process plays a large role in astrophysics because it is a key process in the evolution of presupernova star and the explosion of supernova (SN, Woosley et al. 2002). In this process, the electron number density decreases, and the electron degenerate pressure decreases accordingly. One of the products in the capture process, the neutrinos, escape and take plenty of energy away from the star when the density is below the trapped density of the neutrino. Both the decrease in degenerate pressure and the loss of energy accelerate the collapse (Bethe et al. 1979, 1990) of the star.
The weak interaction processes, including the electron capture and
decay, in dense matter have been investigated extensively in
last decades. Based on the simple shell model, Fuller et al. (1982, hereafter FFN) accomplished pioneering work,
in which they discussed the location and the strength of the
Gamow-Teller (GT) resonance transition and made detailed calculations
of 226 nuclei with mass number A ranging from 21 to 60. Auferheide
et al. (1994) pointe out that the nuclei with A>60 should
also be taken into account in the theoretical analysis because the core
region of presupernova is mainly composed of neutron-rich nuclei.
They extended FFN's work to some nuclei with A>60 and provided the
weak interaction rates of the 150 most abundant isotopes with some
key temperatures and densities at the presupernova stage. In recent
years, the large-scale shell-model calculations and the shell-model
Mont Carlo calculations (SMMC) of the GT strength distribution were
done by Langanke & Martinez-Pinedo
(1997, 2000, hereafter LMP). Their results indicate
that the improved electron capture rates are significantly lower
than usually adopted in core collapse calculation.
People have also addressed the effect of the electron screening in a
weak interaction. In the 1950s, Reitz (1950) analyzed the
effect of screening on
decay by solving the Dirac equation
and concluded that the screening slightly decreases the
decay rate. After that, the screening effect on Fermi function and
Coulomb correction in
decay were considered (Chen et al. 1966; Matese et al. 1966). Gutierrez
(1996) suggested that the decrease in electron Fermi energy is equal
to the shift in the chemical potential of nuclei before and after
the capture reaction. Luo et al. (1996, 2001) argue
that the screening also affects the phase space distribution of the
electron besides the Fermi energy. The calculation showed that the
screening can reduce the rate of change of electron fraction by
.
With the same method as Gutierrez, Bravo (1999) solved
the nuclear statistical equation and found that the neutronization
rate is higher than
at some temperatures and densities.
Numerical simulations show that the SN explosion depends on the persupernova structure and the evolution mode, which is especially sensitive to the physical parameters' input. The parameters are closely related to the electron fraction and the weak interaction rates at the presupernova stage (Heger et al. 2001). Therefore, it is imperative to calculate the electron capture rates with high precision. In this paper, the screening effects on the electron capture rates for the improved results from Langanke et al. (1999) are evaluated.
For the convenience of explaining the results, it is necessary to
briefly introduce the formulae of our calculations. The capture rate
for the kth nucleus (Z, A) in thermal equilibrium at
temperature T is given by a sum over the initial parent states i and the final daughter states f (Pruet et al. 2003),
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(1) |
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(2) |
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(3) |
The screening mainly affects the electron capture in three facets.
(1) The screening changes the Coulomb in-wave function of the
electron, which, however, can be neglected because the screening
potential D is much less than the average energy of the electrons.
(2) The screening decreases the electron energy
in
the capture reaction to
.
(3) The
screening relatively decreases the number of the high energy
electrons whose energy is more than the threshold energy of electron
capture. Thus, the threshold energy will increase from w to
,
where
represents the change in binding
energy of the final and initial nuclei due to the presence of the
electron gas. In the plasma, a nucleus has its binding energy
increased due to interactions with the dense electron gas. In the
Wigner-Seitz approximation, the extra binding of an atom can be
written as
MeV (Salpeter et al. 1969). Because of the charge
dependence of this binding, the effective nuclear Q-value changes
at high density. In general, the average Q-value for each electron
will increase by (FFN 1982)
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(4) |
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(5) |
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Figure 1:
D and ![]() ![]() |
Open with DEXTER |
Table 1:
The effect of electron screening on 56Co
Fe. (
K,
,
C1 denotes the screening factor in the fiducial GT resonance distribution, C2 denotes the screening factor with the improved GT resonance distribution.
Table 2:
The effect of electron screening on 56Co
Fe, where the left panel is the results of
g/cm3,
,
D=0.095 MeV,
MeV and the right panel
is the results of
g/cm3,
,
D=0.208 MeV,
MeV). The other notes are the same as that in Table 1.
Provided the excited state distribution of nucleus is known, the electron capture rates can be obtained with high precision. Unfortunately, the nuclei in the presupernova environment are usually unstable, and the distribution of the high excited states are almost continuous (particularly for the heavier nuclei), so it is difficult to get an explicit distribution for each nucleus. Following the technique of Auderheide et al. (1994), we employed the so-called Brink hypothesis and assumed that the distribution of the parent excited states is similar to that of the ground state and that the location of the GT resonance moves upward in the daughter nucleus by the same amount.
People can split the sum of final states of daughter nuclei into two
parts for convenience. One is the contribution
from the
low-energy region near the ground state and the other is the
contribution
from the resonance region dominated by
the GT resonance transition. The GT strength distribution is similar
to a Gaussian distribution (Kar et al. 1994) and the GT
resonance energy
,
where
is the energy difference between
the new occupied neutron orbital and the ground state;
is the repulsion energy that should be supplied to pull the
neutron out of the daughter ground state;
is the
cost of breaking a neutron pair in daughter nucleus with an even
number of neutrons. The resonance transition matrix element
can be derived from the model calculation, such as the
simple shell-model calculation (FFN 1982). With Auderheide's
method, we take
MeV,
(quenching factor
is 0.5) for 56Co in this paper.
LMP adopted the shell-model diagonalization in the pf shell
with modified KB3 interaction to calculate the electron capture
rates of six important odd-odd nuclei in LMP (1999). They
find that the GT centroids
is typically 2 MeV higher and the
resonance transition matrix element decreases more than the previous
estimation. These changes make the electron capture rates 1 order
of magnitude too low compared to the fiducial results (Aufderheide
et al. 1994; FFN 1982) except for 58Mn. More
detailed large-scale shell-model calculations by LMP show that the
electron capture rates are significantly lower for nuclei with the
mass number ranging from 45 to 65 in the presupernova environment.
For example, the electron capture rate of 56Co is
s-1 by FFN and is
s-1 by
LMP at temperature T=109 K and density
g/cm3 (FFN 1982b; LMP
2000). However, the effect of screening on the electron
capture is ignored in these calculations.
We here calculate the electron capture rates with screening for
capture reaction of 56Co, which is one of the most important
electron capturing nuclei in presupernova. We take
as 8.2 MeV and
as 7.7 in the improved method derived by LMP (1999). In addition, the quenching factor changes from 0.5 to 0.55. For a comparison,we define a screening factor, a ratio C between the electron capture rates with (
)
and
without (
)
screening,
.
We show the influence of electron screening on the reaction
56Co
Fe at different temperatures,
densities, and electron fraction in Tables 1 and 2, where
is the electron capture rate in the
fiducial GT resonance distribution and
the electron
capture rate with the improved GT resonance distribution. Although
the modified rates obviously decrease, they are not as low as LMP's
results. The reason is that LMP handle the ground state (J=4) and
the first excited states (J=3, 5 and 1) of parent nucleus,
respectively. Their calculation adopts 33 Lanczos iterations and
each state (
)
in the parent nucleus is connected to 99
states in the daughter nucleus. Such treatment is more precise and
complicated. But we found the electron capture rate by adopting
LMP's GT resonance transition location and strength is close to
their detailed results, so here we can estimate the effect of
screening by the Brink hypothesis.
Acknowledgements
This work was supported by the National Natural Science Foundation of China under Grant No. 10347008. One of the authors (Menquan Liu) would like to thank Bin Wang at Peking University for useful discussions and help with preparing this paper.