This is the portal to access online tables and preprints of various data
(results of theoretical calculations) interesting in different aspects of
astrophysical application. Please select your area of interest in the navigation
bar on the left. Please quote this webpage and the original publication
when making use of these results. Further preprints can be accessed through
my publication list.
Fits of all reaction rates calculated with the HauserFeshbach code
NONSMOKER are published in
Atomic
Data Nuclear Data Tables 75 (2000) 1.
The printed version is only a subset of all the available fits. The
complete sets of rates are available online from the
ADNDT web site (see
below).
Please note the following copyright information regarding the
paper and
the reaction rate fits:
This
material has been published in Atomic
Data and Nuclear Data
Tables 75 (2000) 1, the only definitive repository of the content that
has been certified and accepted after peer review. Copyright and all
rights therein are retained by Academic Press. This material may not be
copied or reposted without explicit permission.

Preprint
All files are gzipped PostScript:
 Main
text, including explanation of tables and Table A (therein
referred to as Table 1). [22 pages]
(Also available at the
arXiv.org eprint archive.)
 Table I (prepared by the Editorial Office of ADNDT and
not
available
here)
 Table
II [135 pages]
 Table
III [48 pages]
 Table
IV [43 pages]
 Table
V [109 pages] (tabulated
partition functions up to a temperature of 10^{10}
K. Partition
functions for higher temperatures can be found below.)

Machine readable files containing reaction rate fits
Machine
readable files can be downloaded from the online version of the original publication.
If you have problems with downloading from the ADNDT web site, try
here.
There are two sets of reaction rate fits, using
microscopic information
from two mass formulae (FRDM, ETFSIQ), and two tables with the
respective partition functions.
For further details on contents and file formats consult the README
file.
Note: For (n,γ)
reactions, the reaction
rates (obtained with FRDM input)
should be renormalized to the recommended theoretical and experimental
values given in Atomic Data
Nuclear Data Tables 76 (2000) 70!
That paper also gives a theoretical correction of the rates correlated
with the neutron number which can also be applied to nuclei further off
stability.
Please send email to me
if you have further questions.
On public request, the original statistical model (HauserFeshbach)
results used to
generate the above reaction rate fits are also published in a data
repository. The data sets consist of theoretical cross sections and
reaction rates calculated with the NONSMOKER code. In order to
facilitate comparison to other calculations, the input set of nuclear
level information is also given.
The tables have appeared in
Atomic
Data Nuclear Data Tables 79 (2001) 47.
The
printed version only contains a detailed explanation and 3 sample
tables. The full tables are only available online.
Please note the following copyright information regarding the
paper and
the cross section and reaction rate tables:
This material has been
published in Atomic
Data and Nuclear Data
Tables 79 (2001) 47, the only definitive repository of the content that
has been certified and accepted after peer review. Copyright and all
rights therein are retained by Academic Press. This material may not be
copied or reposted without explicit permission.

Preprint
The preprint is locally available in PostScript
or PDF
and also from the arXiv.org
eprint archive.

Machine processable files of cross sections and reaction
rates
Machine
readable files can be downloaded from the online version of
the ADNDT article.
In case you have problems accessing the ADNDT site, try to download
from here.
The full article is available at IDEAL.
The files contain nuclear cross sections and reaction
rates 
calculated
with microscopic information from two mass models (FRDM, ETFSIQ) 
and nuclear level information used in the computation of the above
astrophysical reaction rate fits.
For further details on contents and file formats consult the README
file.
Note: For (n,γ)
reactions, the cross sections and reaction
rates (obtained with FRDM input)
should be renormalized to the recommended theoretical and experimental
values given in Atomic
Data
Nuclear Data Tables 76 (2000) 70!
That paper gives a theoretical correction of the rates correlated
with the neutron number which can also be applied to nuclei further off
stability.
For certain applications it is necessary to have partition functions
available beyond the temperature range considered in the
above
ADNDT paper. The
above
paper contains tables of
partition functions up to a maximal temperature of T
_{9}=10.
The extended set of partition functions presented here was calculated
for a grid of temperatures from 1.2x10^{10} K to
2.75x10^{11} K (1<=kT<=24 MeV). At
such high
energies/temperatures additional continuum corrections have to be
applied which lead to a suppression of the "bare" partition function.

Preprint
The paper appeared in Astrophys. J. Suppl. 147 (2003) 403.
The preprint is locally available in PostScript
or PDF
and also from the arXiv.org
eprint archive.

Machine processable files of highT partition
functions
Machine
readable files are available from the online version of Astrophys. J. Suppl. 147 (2003) 403.
In case you have problems accessing the Ap.
J. site, try to download
from here.
Recently there has been increased interest in testing reaction cross
section predictions of photodisintegration reactions by using real
photons from Bremsstrahlung or lasers. In principle,
photodisintegration
rates can be inferred from
the
data given above.
However, those are not
applicable to the reactions studied in the laboratory where the target
usually is in its ground state. Therefore, here we calculate
photodisintegration cross sections for targets in their naturally
occuring excitation states, which is the first excited state for
^{180}Ta (i.e.
^{180m}Ta)
and the ground state for all other nuclei. More
specifically, the (γ,n), (γ,p), and
(γ,α) cross
sections
for naturally occuring isotopes from Ti to Bi are given (those are
considered to be relevant for the γ, p, s, and
rprocesses
in heavy element
nucleosynthesis and therefore warrant further study). The results
were obtained with the same NONSMOKER code with the same inputs as for
the papers above.
It should be noted that these cross sections cannot
be applied to
nucleosynthesis calculations as the thermal excitation of the target is
not considered. However, this becomes important for photodisintegration
reactions already at moderate temperatures. For such applications, use
the rates from the
above paper instead.
The tables have been published in
Atomic
Data Nuclear Data Tables 88 (2004) 1.
Please note the following copyright information regarding the paper and
the cross sections:
This material has been
published in Atomic
Data and Nuclear Data
Tables 88 (2004) 1, the only definitive repository of the content that
has been certified and accepted after peer review. Copyright and all
rights therein are retained by Academic Press. This material may not be
copied or reposted without explicit permission.

Preprint
The preprint is available from the arXiv.org
eprint archive.

Machine processable files of photoninduced cross
sections for targets in their ground state
Machine
readable files are available at the online version of the paper.
In case you have problems accessing the ADNDT site, try to download
from here.
The stellar evolution of massive stars with masses between 15 and 25
solar masses and initial solar metallicity has been calculated with
updated stellar and nuclear physics. The original paper appeared in
The Astrophysical Journal 576 (2002) 323. The printed
version contains abbreviated tables whereas the electronic version
includes the full tables.
Preprint
The preprint is available from the arXiv.org
eprint archive.
Machine processable tables
All tables in the paper
are also available in ASCII format in the online version of
The Astrophysical Journal 576 (2002) 323.
You have to click on the table and then on "ASCII" in the first line on the top.
If you cannot access the journal, ASCII versions of Tables 5, 8, 9 can be
downloaded locally.
Additionally, the elemental yields can also be
downloaded.
This table was not published before.
Additional material
Additional, previously unpublished and more detailed data are also available. These include yields obtained with different reaction rates,
pre and postsupernova structure and composition data, as well as some
movies. Check it out!
The ratio of the nuclear level densities for even and odd parity states as
a function of excitation energy has been calculated for all nuclides
between Ne and Bi. These ratios are used in the calculation of
astrophysical reaction rates in the newer versions of the
NONSMOKER^{WEB} code and will be used
in the future treatment of direct capture reactions.
Preprint
The paper has been published as Physical Review C 75 (2007) 045805.
The preprint is available at the arXiv.org
eprint archive.
Machine processable tables
ASCII tables with the parity ratios for all considered nuclei are
available
with the original publication.
They are also available locally from this server. Please cite the paper and that page when
making use of the files.
The relevant energy windows (sometimes called Gamow windows) for
the calculation of astrophysical reaction rates. The energy windows
are derived with the use of
NONSMOKER cross
sections. It is found that the usual approximation formulae for the
Gamow windows are not applicable in many cases.
It is important to note that the relevant energy windows are not just derived
from 1/e widths of the integrand's peak. Rather, they were numerically
determined to yield 10% accuracy in the rate when completely covered!
Preprint
The paper appeared in Physical Review C 81 (2010) 045807. The preprint is available at the arXiv.org preprint archive.
Machine processable table
An ASCII table with the relevant energy windows and the errors in the standard
formulae is available as supplemental material to Phys. Rev. C 81 (2010) 045807. It is also available
locally from this server. Please cite the paper and that page when
making use of the results.
Currently it is only possible to measure reactions proceeding on nuclei in the ground state. In stellar plasmas, however, reactions also occur on nuclei in excited states. The population of excited states depends on the plasma temperature but also on the nuclear spectroscopy. The ground state contribution to a stellar rate (the Xfactor) is important to determine how well an astrophysical rate can be constrained by a measurement and how strong it is affected by theoretical uncertainties.
A table of Xfactors is provided for nuclei and temperatures relevant for the sprocess. (A full table for all reactions in a wider range of stellar temperatures can be found in the paper below!) The details and relevant definitions and formulae for the calculation of the uncertainty factors are given in the full paper.
Preprint
The paper appeared in The Astrophysical Journal 738 (2011) 143. The preprint is available at the arXiv.org preprint archive.
Machine processable table
An ASCII table with the Xfactors, partition functions, and stellar enhancement factors are available as Electronic Table. It is also available
locally from this server. Please cite the paper when making use of the results.
Sensitivities of nuclear reaction rates to a variation of nuclear properties are studied. Target nuclei range from proton to neutrondripline for 10<=Z<=83. Reactions considered are nucleon and alphainduced reactions mediated by the strong interaction. The contribution of reactions proceeding on the target ground state to the total stellar rate is also given. General dependences on various input quantities are discussed. Additionally, sensitivities of laboratory cross sections of nucleon, alpha, and gammainduced reactions are shown, allowing to estimate the impact of cross section measurements. Finally, recommended procedures to explore and improve reaction rate uncertainties using the present sensitivity data are outlined.
Several tables of sensitivities are provided. These include sensitivities to variations of the neutron, proton, alpha, and gammawidths and of the nuclear level density. The sensitivities are given for particle and photoninduced cross sections and rates. The details and relevant definitions and formulae are given in the full paper.
Preprint
The paper appeared in The Astrophysical Journal Supplement 201 (2012) 26. The preprint is available at the arXiv.org preprint archive.
Machine processable table
The ASCII tables with the sensitivities are available along with the original paper. They are also available
locally from this server. There you can also find sample programs extracting data directly from the formatted tables. Please cite the paper when making use of the results.
The νp process appears in protonrich, hot matter which is expanding in a neutrino wind and may be realised in
explosive environments such as corecollapse supernovae or in outflows from accretion disks. The impact of uncertainties in nuclear
reaction cross sections on the finally produced abundances has been studied by applying Monte Carlo variation of all astrophysical
reaction rates in a large reaction network. As the detailed astrophysical conditions of the νp process still are unknown, a
parameter study was performed, with 23 trajectories covering a large range of entropies and Y
_{e}.
The results, including tables with uncertainties and key reactions, have been published in Nishimura et al., MNRAS 489 (2019) 1379 (arXiv:1907.13129).
Additional tables with isotopic abundance ratios of light pnuclei and their uncertainties can be found here.
A general formalism to include experimental reaction cross sections into calculations of stellar rates is presented. It also allows to assess the maximally possible reduction of uncertainties in the stellar rates by experiments. As an example for the application of the procedure, stellar neutron capture reactivities from
KADoNiS v0.3 are revised and the remaining uncertainties shown. Many of the uncertainties in the stellar rates are larger than those obtained experimentally. This has important consequences for sprocess models and the interpretation of meteoritic data because it allows the rates of some reactions to vary within a larger range than previously assumed.
The paper contains a large table with the revised stellar rates, their uncertainties, and also the excited state contributions (a generalization of the g.s. contribution concept) and their uncertainties.
Preprint
The paper appeared in The Astrophysical Journal Letters 755 (2012) L10. The preprint is available at the arXiv.org preprint archive.
Machine processable table
The ASCII table with the newly derived reactivities and uncertainties is available in the original paper. It is also available
locally from this server. Please cite the paper when making use of the results.
Erratum to the above paper:
The original uncertainties given for the revised stellar rates were incorrectly calculated in some cases. An erratum was published giving the corrected uncertainty calculation and also a complete version of Eq. (6), which was incomplete in the original paper.
The erratum appeared in The Astrophysical Journal Letters 864 (2018) L40. The preprint is available at the arXiv.org preprint archive.
The ASCII table with the corrected uncertainties is available in the original publication. It is also available locally from this server.
THEXO (Theoretical tools in support of Infrastructures) is a JRA within ENSAR. During the ENSAR programme tables of stellar reactivities have been produced with an updated model calculation. It is accessible from the
THEXO portal.