Tables and Preprints

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 Astrophysical Reaction Rates

Fits of all reaction rates calculated with the Hauser-Feshbach code NON-SMOKER 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 on-line 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.

  1. 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 e-print 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 1010 K. Partition functions for higher temperatures can be found below.)

  2. Machine readable files containing reaction rate fits

    Machine readable files can be downloaded from the on-line 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, ETFSI-Q), 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 e-mail to me if you have further questions.

Tables of Nuclear Cross Sections and Reaction Rates

On public request, the original statistical model (Hauser-Feshbach) 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 NON-SMOKER 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 on-line.

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.

  1. Preprint

    The preprint is locally available in PostScript or PDF and also from the arXiv.org e-print archive.

  2. Machine processable files of cross sections and reaction rates

    Machine readable files can be downloaded from the on-line 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, ETFSI-Q) - 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.

Nuclear Partition Functions For T9>10

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 T9=10.

The extended set of partition functions presented here was calculated for a grid of temperatures from 1.2x1010 K to 2.75x1011 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.

  1. 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 e-print archive.

  2. Machine processable files of high-T partition functions

    Machine readable files are available from the on-line version of Astrophys. J. Suppl. 147 (2003) 403. In case you have problems accessing the Ap. J. site, try to download from here.

Predicted Cross Sections for Photon-Induced Particle Emission

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 180Ta (i.e. 180mTa) 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 r-processes in heavy element nucleosynthesis and therefore warrant further study). The results were obtained with the same NON-SMOKER 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.

  1. Preprint

    The preprint is available from the arXiv.org e-print archive.

  2. Machine processable files of photon-induced cross sections for targets in their ground state

    Machine readable files are available at the on-line version of the paper. In case you have problems accessing the ADNDT site, try to download from here.

Core-Collapse Supernova Yields

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.

  1. Preprint

    The preprint is available from the arXiv.org e-print archive.

  2. Machine processable tables

    All tables in the paper are also available in ASCII format in the on-line 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.

  3. 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!

Parity ratios in the nuclear level density

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 NON-SMOKERWEB code and will be used in the future treatment of direct capture reactions.

  1. Preprint

    The paper has been published as Physical Review C 75 (2007) 045805. The preprint is available at the arXiv.org e-print archive.

  2. 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.

Effective energy windows

The relevant energy windows (sometimes called Gamow windows) for the calculation of astrophysical reaction rates. The energy windows are derived with the use of NON-SMOKER 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!

  1. Preprint

    The paper appeared in Physical Review C 81 (2010) 045807. The preprint is available at the arXiv.org preprint archive.

  2. 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.

Ground state contributions to stellar rates

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 X-factor) 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 X-factors is provided for nuclei and temperatures relevant for the s-process. (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.

  1. Preprint

    The paper appeared in The Astrophysical Journal 738 (2011) 143. The preprint is available at the arXiv.org preprint archive.

  2. Machine processable table

    An ASCII table with the X-factors, 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.

Sensitivity of astrophysical reaction rates to nuclear uncertainties

Sensitivities of nuclear reaction rates to a variation of nuclear properties are studied. Target nuclei range from proton- to neutron-dripline for 10<=Z<=83. Reactions considered are nucleon- and alpha-induced 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 gamma-induced 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 gamma-widths and of the nuclear level density. The sensitivities are given for particle- and photon-induced cross sections and rates. The details and relevant definitions and formulae are given in the full paper.

  1. Preprint

    The paper appeared in The Astrophysical Journal Supplement 201 (2012) 26. The preprint is available at the arXiv.org preprint archive.

  2. 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.

Monte Carlo Study of the νp Process

The νp process appears in proton-rich, hot matter which is expanding in a neutrino wind and may be realised in explosive environments such as core-collapse 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 Ye.

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 p-nuclei and their uncertainties can be found here.

Revised s-process neutron capture rates including uncertainties

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 s-process 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.

  1. Preprint

    The paper appeared in The Astrophysical Journal Letters 755 (2012) L10. The preprint is available at the arXiv.org preprint archive.

  2. 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.

  3. 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.

Stellar Reactivities for THEXO

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.
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© Dr. Thomas Rauscher (email), last change 2019-Nov-29