Library format:
STARLIB is a nextgeneration library of thermonuclear reaction and decay
rates. Additional information is available in our publication in the Astrophysical Journal Supplement Series.
STARLIB incorporates the results of the Monte Carlo based thermonuclear reaction rate evaluation
of Iliadis et al., Nucl. Phys. A841, 31 (2010). Unlike other libraries,
STARLIB also provides factor uncertainties and probability density functions of reaction rates at
each temperature grid point.
For each nuclear reaction, the experimental or theoretical rates listed here refer to "stellar" rates, that is, rates that take into account the
thermal population of the interacting nuclei. The "stellar" rates are computed from
"laboratory" rates by using a correction factor, called stellar enhancement factor
(SEF), which is obtained from HauserFeshbach theory [Goriely, Hilaire, and Koning,
Phys. Rev. C 78, 064307 (2008)]. Reverse stellar rates are computed from the
corresponding forward stellar rates by using normalized partition functions of the
nuclei involved in the reaction [Goriely, Hilaire, and Koning,
Phys. Rev. C 78, 064307 (2008)], i.e., the tabulated reverse rates already contain the ratio of partition functions. For weak interactions, the tabulated values correspond to "laboratory"
rates, i.e., they do not take the thermal population of excited states in the
decaying nucleus into account. The decay rates are either adopted from experiment or from theory.
For the modeling of stellar environments that are exposed to elevated temperatures and densities, the rates listed in STARLIB
need to be supplemented by information pertaining to (i) "stellar" weak interactions, and (ii) plasma screening.
Header and column format:
STARLIB lists for each reaction a header and three columns.
Header:
spaces 135: interaction label, where each nuclide label is rightaligned in
a field of 5 characters; the first 15 spaces contain nuclides of the incoming
channel, the following 20 spaces contain nuclides in the outgoing channel. The chapter number is listed in the first space, following the convention of JINA REACLIB .
 Example 1: the reaction ^{3}He+^{7}Be → 2p+^{4}He+^{4}He is denoted by:
he3 be7 p p he4 he4
 Example 2: the reaction ^{4}He+^{104}Rb → ^{107}Y+n is denoted by:
he4rb104 n y107
 Example 3: the photodisintegration ^{49}Ti → ^{48}Sc+p is denoted by:
ti49 p sc48
 Example 4: the betadecay ^{99}As → ^{99}Se is denoted by:
as99 se99
Next in the header is the source label indicating the source of the rates. This label
occupies spaces 4447. The labels and the associated references are listed at the
end of this page. Space 48 is reserved for a special label: (i) The character "v" denotes a reverse rate that was
calculated from the corresponding forward rate; the tabulated values already contain the ratio of partition functions; (ii) "w" denotes a weak interaction; (iii) "g" denotes a
gammaray transition, see below. The characters
"ec" in spaces 4647 are used for three interactions: the pep reaction; ^{3}He → t; ^{7}Be → ^{7}Li. In these three
cases the
tabulated rates need to be corrected for the electron density, i.e., multiplied by
rho*Ye; this is a legacy from the Caughlan and Fowler compilation.
Next in the header is the nuclear energy release (Qvalue) for the interaction
in units of MeV. The energy occupies spaces 5364.
Columns:
column 1 lists the temperature in units of GK (10^{9} K). The lowest and highest
temperatures given are 1 MK and 10 GK, respectively.
column 2 lists the thermonuclear rate of a reaction (in units of cm^{3} mol^{1} s^{1}),
or the decay constant of a photodisintegration or a betadecay (in units of s^{1}).
column 3 lists the factor uncertainty of the rate at the given temperature.
In most
cases it can be assumed that the rate probability density function is described
by a lognormal distribution [Longland et al., Nucl. Phys. A841, 1 (2010) Sec. 5.4].
Thus the values of the rate in column 2 and of the corresponding factor uncertainty
in column 3 allow an estimation of the lognormal parameters mu and sigma of the
rate probability density function at each temperature. They are simply given by:
mu = ln(rate)
sigma = ln(factor uncertainty)
where "ln" denotes the natural logarithm.
Notes:
 In one case, the same interaction label appears twice in STARLIB,
but the source label is different:
both the p+p reaction and the p+e+p reaction have the interaction label
" p p d".
In the first case, the source label is "nacr" (indicating that the rate is adopted from the NACRE evaluation), while in the second case the source label is "ec" (indicating that
the rate tabulated here needs to be multiplied by rho*Ye before use in
a reaction network calculation).

The nucleus ^{8}Be does not occur in STARLIB. Since its halflife is very short, the breakup into
two alpha particles is explicitly included in the tabulated rates. For example, for the triple alpha reaction the total 3a → ^{12}C rate is
listed, but not the individual rates for the two steps a+a → ^{8}Be and ^{8}Be+a → ^{12}C.

When a rate was estimated using the Monte Carlo procedure [Longland et al., Nucl. Phys. A841, 1 (2010)], the "median rate" is listed here, not the rate
calculated from the parameter mu of the lognormal approximation of the rate probability density.

For the Monte Carlo based rates, the factor uncertainty given here is calculated
from f.u. = exp(sigma), where sigma is the spread parameter of the lognormal
approximation of the rate probability density.

When incorporating experimental reaction rates published in the literature that
were not obtained using the Monte Carlo procedure, we explicitly assume that the
rate probability densities are lognormally distributed and find the recommended
rate (column 2) and factor uncertainty (column 3) from Eq. (39) of [Longland et al., Nucl. Phys. A841, 1 (2010)].

For experimental betadecays and competing betadelayed particle decays, we assume
that the rate probability densities are lognormally distributed. Values of the rate and factor
uncertainty are computed from the following input: total halflife; uncertainty in halflife;
branching ratio, uncertainty in branching ratio.
Beta decays:
Many experimental halflives in G. Audi's 2003 evaluation were "symmetrized", i.e., they must have been
obtained from widths, giving rise to asymmetric uncertainties, and the deduced halflife uncertainties
were then made symmetric [the procedure is described in Audi et al., Nucl. Phys. A 729, 3 (2003)].
As a reasonable thing to do, we interpret the reported values of the experimental halflife and its
uncertainty
(or the derived partial halflife and uncertainty) as the expectation value, E[x], and standard
deviation, sqrt(V[x]), of a lognormal distribution. For the decay constant, lambda = ln 2/T_{1/2}, we obtain
the "median" value from lambda = exp(ln(ln 2)  mu) and the factor uncertainty from f.u. = exp(sigma), where
mu and sigma are found from Eq. (27) of Longland et al., Nucl. Phys. A841, 1 (2010).
Above we assume that the decay constant, lambda, is lognormally distributed. We suspect that
the probability densities of very precisely measured halflives are distributed according to a difference
of two Poissonians (i.e., counting statistics limited). One may argue, however, that for not too small sample
sizes a Poissonian is well approximated by a Gaussian, which in turn can be approximated by a
lognormal distribution if the uncertainty is relatively small.
When a betadelayed particle decay competes with a beta decay, the "partial" halflives for these
competing interactions are found from t_{1/2} = T_{1/2} / BR, while the associated uncertainty is found by
quadratically adding the individual relative uncertainties.
Isomeric states:
For the special case of ^{26}Al, six different labels are used: al26, al6, al*6, al01, al02, al03.
The first refers to ^{26}Al in thermal equilibrium. The second and third refer to the
ground state (J^{π} = 5^{+}) and isomeric state (E_{x} = 228 keV; J^{π} = 0^{+}), respectively. The last three denote
the excited ^{26}Al levels at E_{x} = 417 keV, 1058 keV, and 2070 keV.
At high temperatures, the ground and isomeric state in ^{26}Al will be in thermal equilibrium.
In that case, the label "al26" (but none of the other ^{26}Al labels!) may be used when constructing
the reaction network. At low temperatures, the ground and isomeric state are not in
thermal equilibrium and may be considered as separate species. In that case, the labels
"al6" and "al*6" (but not "al26"!) may be used when constructing the reaction network.
The temperature boundary above (below) which ^{26}Al is (is not) in thermal equilibrium is
about T = 400 MK [Ward and Fowler, Astrophys. J. 238, 266
(1980)]. These are
extreme assumptions and a more consistent procedure is to take the equilibration
of the ^{26}Al ground and isomeric state explicitly into account (via excitations of higher lying
^{26}Al levels, of which those at E_{x} = 417 keV, 1058 keV, and 2070 keV are most important).
In the latter case, the labels "al6", "al*6", "al01", "al02" and "al03" (but not "al26"!) may be
used when constructing the reaction network.
The necessary gamma and betadecay transition strengths were computed by Coc, Porquet
and Nowacki, Phys. Rev. C 61, 015801 (1999); Runkle, Champagne and Engel, Astrophys.
J. 556, 970 (2001); Gupta and Meyer, Phys. Rev. C 64, 025805 (2001). Values of the decay
constants are listed in App. A of Iliadis et al., Astrophys. J. Suppl. 193, 16 (2011).
Rate reference labels (links present):
 REACTION RATES BASED ON EXPERIMENT
cf88   Caughlan & Fowler, At. Data Nucl. Data Tab. 40, 283 (1988) [CF88] 
de04   Descouvemont et al., At. Data Nucl. Data Tab. 88, 203 (2004) 
mc10   Iliadis et al., Nucl. Phys. A 841, 31 (2010) [Monte Carlo rates] 
mc13   Sallaska et al., ApJ Supp. Ser. 207, 18 (2013) [updated Monte Carlo rates] 
nacr   Angulo et al., Nucl. Phys. A 656, 3 (1999) [NACRE] 
taex   experimental neutron induced rates, extrapolated using TALYS 

REACTION RATES BASED ON HAUSERFESHBACH THEORY

DECAY RATES BASED ON EXPERIMENT

DECAY RATES BASED ON THEORY
bkmow   Klapdor, Metzinger & Oda, At. Data Nucl. Data Tab. 31, 81 (1984) [betaminus decay] 
btykw   Takahashi, Yamada & Kondo, At. Data Nucl. Data Tab. 12, 101 (1973) [betaplus decay] 
ec   pep reaction; ^{3}He → t; ^{7}Be → ^{7}Li (*) 
il11g   Iliadis et al., Astrophys. J. Suppl. 193, 16 (2011) 
ka88w   Kajino et al., Nucl. Phys. A 480, 175 (1988) [betadecay of excited 26Al levels] 
mo92w   Moeller et al. (1992) [betaminus decay] 
mo03w   Moeller, Pfeiffer, and Kratz, Phys. Rev. C 67, 055802 (2003) 

INDIVIDUAL RATES, MAINLY BASED ON EXPERIMENT
an06   Ando et al., Phys. Rev. C 74, 025809 (2006) 
ar12   Arnold et al., Phys. Rev. C 85, 044605 (2012) 
bb92   Rauscher et al., Astrophys. J. 429, 499 (1994) 
be01   Beaumel et al., Phys. Lett. B 514, 226 (2001) 
ce14   Cesaratto et al., Phys. Rev. C 88, 065806
(2013)

cy08   Cybert & Davids, Phys. Rev. C 78, 064614 (2008) 
fu90   Fukugita & Kajino, Phys. Rev. D 42, 4251 (1990) 
ha10   Hammache et al., Phys. Rev. C 82, 065803 (2010) 
il11   Iliadis et al., Astrophys. J. Suppl. 193, 16 (2011) 
im05   Imbriani et al., Eur. Phys. J. A 25, 455 (2005) 
ku02   Kunz et al., Astrophys. J. 567, 643
(2002) 
mafo   Malaney and Fowler, Astrophys. J. 345, L5 (1989) 
nk06   Nagai et al., Phys. Rev. C 74, 025804 (2006) 
po13   Pogrebnyak et al., Phys. Rev. C 88, 015808 (2013) 
re98   Rehm et al., Phys. Rev. Lett. 80, 676 (1998) 
rolf   C. Rolfs and collaborators 
se04   Serpico et al., J. Cosm. Astropart. Phys. 12, 010
(2004) 
ta03   Tang et al., Phys. Rev. C 67, 015804 (2003) 
wies   M. Wiescher and collaborators 
Notes: * Values listed need to be multiplied by rho*Y_{e}.
