Dillmann, I

Heil, M

Käppeler, F

Plag, R

Rauscher, T

CERN Document Server

PoS(NIC-IX)090Present status of the KADoNiS databaseIris Dillmann∗†Forschungszentrum Karlsruhe, Institut für Kernphysik, Postfach 3640, D-76021 Karlsruhe andDepartement Physik und Astronomie, Universität Basel, Klingelbergstrasse 82, CH-4056 BaselE-mail: iris.dillmann@ik.fzk.deRalf Plag, Michael Heil, and Franz KäppelerForschungszentrum Karlsruhe, Institut für Kernphysik, Postfach 3640, D-76021 KarlsruheThomas RauscherDepartement Physik und Astronomie, Universität Basel, Klingelbergstrasse 82, CH-4056 BaselThe "Karlsruhe Astrophysical Database of Nucleosynthesis in Stars" (KADoNiS) project is anonline database for experimental cross sections relevant to the s process and p process. It isavailable under http://nuclear-astrophysics.fzk.de/kadonis and consists of two parts. Part 1 is anupdated sequel to the well-known Bao et al. compilations from 1987 and 2000, which is onlinesince April 2005. An extension of this s-process database to (n, p) and (n,α) cross sections at kT =30 keV, as in the first version of the Bao compilation, is planned. The second part of KADoNiSis a p-process library, which includes all available experimental data from (p,γ), (p,n), (α,γ),(α,n), (α,α), (n,α) and (γ,n) reactions in or close to the respective Gamow window. Despitethe great number of reactions required for a p-process reaction network, experimental data is stillscarce and up to now restricted to stable targets. Given here is a short overview about the presentstatus of the KADoNiS database.International Symposium on Nuclear Astrophysics — Nuclei in the Cosmos — IXJune 25-30 2006CERN, Geneva, Switzerland∗Speaker.†This work was supported by the Swiss National Science Foundation Grants 2024-067428.01 and 2000-105328.c© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/PoS(NIC-IX)090Present status of the KADoNiS database Iris Dillmann1. History of stellar neutron capture compilationsThe first collection of stellar neutron capture cross sections was published in 1971 by Allen andco-workers [1]. This paper reviewed the role of neutron capture reactions in the nucleosynthesisof heavy elements and presented also of a list of recommended (experimental or semi-empirical)Maxwellian averaged cross sections at kT = 30 keV (MACS30) for nuclei between carbon andplutonium (6≤Z≤94). The idea of an experimental and theoretical stellar neutron cross sectiondatabase was picked up again by Bao and Käppeler [2] for s-process studies. This compilationpublished in 1987 included cross sections for (n,γ) reactions (between 12C and 209Bi), some (n, p)and (n,α) reactions (33Se to 59Ni), and also (n,γ) and (n, f ) reactions for long-lived actinides. A(limited) updated compilation was published in 1992 by Beer, Voss and Winters [3].In the update of 2000 [4] the Bao compilation from 1987 was extended to isotopes between 1Hand 209Bi, and listed – like the original Allen paper – also semi-empirical recommended values fornuclides without experimental cross section information. These estimated values are normalizedcross sections derived with the Hauser-Feshbach code NON-SMOKER [5], which account forknown systematic deficiencies in the nuclear input of the calculation. Additionally, the databaseprovided stellar enhancement factors and energy-dependent MACS for energies between kT= 5keV and 100 keV.2. The updated big bang and s-process databaseThe first update of the big bang and s-process database was finished in January 2006 [6]. Inthis stage, eight theoretical cross sections (74Se, 84Sr, 128−130Xe, 147Pm, 151Sm, and 180Tam) werereplaced with new experimental values. Further 20 cross sections were updated by the inclusionof new data. In order to make these updates reproducible, a full list of updated cross sections withreferences can be found on the KADoNiS homepage in the menu section "Logbook". Here will bealso a history of previous KADoNiS versions.The main future efforts in this part will be focussed on the re-evaluation of semi-empiricalcross sections and the re-calculation of cross sections for isotopes, where a recent change in physi-cal properties (e.g. t1/2, Iγ ...) leads to changes in already measured cross sections. Another modulewill be the extension to (n, p) and (n,α) cross sections at kT = 30 keV, as in the first version of theBao compilation [2].3. The new p-process databaseThe second part of KADoNiS is a collection of all experimental reaction rates relevant forp-process studies. The first stage is presented here and includes all available datasets of (α ,γ)(Table 1) and (p,γ) (Table 2) reactions within the respective Gamow window (see column EGamow).These tables are listed under http://nuclear-astrophysics.fzk.de/kadonis/pprocess, includinghyperlinks to the respective EXFOR files. In the present stage (July 2006) we have included 39(p,γ) datasets of 32 isotopes between 58Ni and 119Sn, and 9 (α ,γ) reactions. For these isotopeswe have created datasheets similar to those in the s-process database, which include tabulated crosssections data, from which the respective S factor and reaction rate is calculated. As additional in-formation, a graphical plot of the dataset(s) with the location of the Gamow window is given. A2PoS(NIC-IX)090Present status of the KADoNiS database Iris DillmannIsotope Reaction Eexp [MeV ] EGamow [MeV ] Reference EXFOR Entry56Fe (α ,γ) 3.90 - 6.50 3.21 - 6.86 [7] A030858Ni (α ,γ) 4.90 - 6.10 3.40 - 7.18 [8] C070362Ni (α ,γ) 5.10 - 8.60 3.40 - 7.19 [9] C066964Ni (α ,γ) 4.40 - 7.10 3.40 - 7.20 [9] C066963Cu (α ,γ) 5.90 - 8.70 3.49 - 7.34 [10] C105070Ge (α ,γ) 5.05 - 7.80 3.78 - 7.80 [11] O089796Ru (α ,γ) 7.03 - 10.56 4.85 - 9.51 [12] A0451112Sn (α ,γ) 8.30 - 9.97 5.32 - 10.30 [13] C0904144Sm (α ,γ) 10.50 - 13.40 6.26 - 11.78 [14] A0416Table 1: List of (α,γ) reactions within the Gamow window (EGamow), which are included in the p-processlibrary.graphical comparison with theoretical predictions from MOST [15] and NON-SMOKER [5] willalso be included.Up to the end of 2006 we plan to extend this database also to other available reactions, e.g.(p,n), (p,α), (α ,n), (α , p), (n,α) and (n, p) reactions. A further step will be the inclusion ofphotodissociation rates, and the calculation of those rates from (n,γ) reactions via detailed balance.Although KADoNiS is thought to be a "dynamic" database, which is updated regularly, a paperversion will be published in 2007.References[1] B. Allen, J. Gibbons, and R. Macklin, Adv. Nucl. Phys., 4, (1971) 205.[2] Z. Bao, and F. Käppeler, At. Data Nucl. Data Tables 36, (1987) 411.[3] H. Beer, F. Voss, and R. Winters, Ap. J. Suppl. 80, (1992) 403.[4] Z. Bao, H. Beer, F. Käppeler, F. Voss, K. Wisshak, and T. Rauscher, At. Data Nucl. Data Tables 76,(2000) 70.[5] T. Rauscher and F.-K. Thielemann, At. Data Nucl. Data Tables 79, (2001) 47.[6] I. Dillmann, M. Heil, F. Käppeler, R. Plag, T. Rauscher, and F.-K. Thielemann, AIP Conf. Proc. 819,(2006) 123.[7] M.R. Anderson, S.R. Kennett, Z.E. Switkowski, D.G. Sargood, Nucl. Phys. A 316, (1979) 471.[8] F.K. MacGowan, P.H. Stelson, W.G. Smith, Phys. Rev. B 133, (1964) 907.[9] J.L. Zyskind, J.M. Davidson, M.T. Esat, M.H. Shapiro, R.H. Spear, Nucl. Phys. A 331, (1979) 180.[10] M.S. Basunia, E.B. Norman, H.A. Shugart, A.R. Smith, M.J. Dolinski, and B.J. Quiter, Phys. Rev. C71, (2005) 035801.[11] Zs. Fülöp, A.Z. Kiss, E. Somorjai, C.E. Rolfs, H.P. Trautvetter, T. Rauscher, and H. Oberhummer, Z.Phys. A 355, (1996) 203.[12] W. Rapp, M. Heil, D. Hentschel, F. Käppeler, R. Reifarth, H.J. Brede, H. Klein, and T. Rauscher,Phys. Rev. C 66, (2002) 015803.3PoS(NIC-IX)090Present status of the KADoNiS database Iris Dillmann[13] N. Özkan, A.S.J. Murphy, R.N. Boyd, A.L. Cole, M. Famiano, R.T. Gray, M. Howard, L. Sahin, J.J.Zach, R. de Haan, J. Görres, M.C. Wiescher, M.S. Islam, and T. Rauscher, Nucl. Phys. A 710, (2002)469.[14] E. Somorjai, Zs. Fülöp, A.Z. Kiss, C.E. Rolfs, H.P. Trautvetter, U. Greife, M. Junker, S. Goriely, M.Arnould, M. Rayet, T. Rauscher, and H. Oberhummer, Astron. Astrophys. 333, (1998) 1112.[15] S. Goriely, Hauser-Feshbach rates for neutron capture reactions (version 08/26/05),http://www-astro.ulb.ac.be/Html/hfr.html (2005).[16] G.A. Krivonosov, B.A. Nemashkalo, O.I. Ekhichev, A.P. Klucharev, A.I. Popov, V.E. Storizhko, andV.K. Chirt, 24th Conference on Nuclear Spectroscopy and Nuclear Structure, Kharkov (USSR), 1974,p. 352.[17] C.W. Cheng and J.D. King, Can. Journ. of Physics 58, (1980) 1677.[18] G.A. Krivonosov, B.A. Nemashkalo, O.I. Ekhichev, V.E. Storizhko, and V.K. Chirt, Izv. RossiiskoiAkademii Nauk, Ser. Fiz. 41, Issue 10, (1977) 2196.[19] C.W. Tingwell, L.W. Mitchell, M.E. Sevior, D.G. Sargood, Nucl. Phys. A 439, (1985) 371.[20] M.E. Sevior, L.W. Mitchell, M.R. Anderson, C.W. Tingwell, D.G. Sargood, Austr. Journ. of Physics36, (1983) 463.[21] S. Qiang, Ph.D. thesis, University of Kentucky, Lexington/ USA, (1990).[22] M.T. Esat, R.H. Spear, J.L. Zyskind, M.H. Shapiro, W.A. Fowler, and J.M. Davidson, Phys. Rev. C23, (1981) 1822.[23] Gy. Gyürky, Zs. Fülöp, E. Somorjai, M. Kokkoris, S. Galanopoulos, P. Demetriou, S. Harissopulos, T.Rauscher, and S. Goriely, Phys. Rev. C 68, (2003) 055803.[24] Gy. Gyürky, E. Somorjai, Zs. Fülöp, S. Harissopulos, P. Demetriou, and T. Rauscher, Phys. Rev. C 64,(2001) 065803.[25] S. Galanopoulos, P. Demetriou, M. Kokkoris, S. Harissopulos, R. Kunz, M. Fey, J.W. Hammer, Gy.Gyürky, Zs. Fülöp, E. Somorjai, and S. Goriely, Phys. Rev. C 67, (2003) 015801.[26] P. Tsagari, M. Kokkoris, E. Skreti, A.G. Karydas, S. Harissopulos, T. Paradellis, and P. Demetriou,Phys. Rev. C 70, (2004) 015802.[27] C.E. Laird, D. Flynn, R.L. Hershberger, and F. Gabard, Phys. Rev. C 35, (1987) 1265.[28] F.R. Chloupek, A.S.J. Murphy, R.N. Boyd, A.L. Cole, J. Görres, R.T. Gray, G. Raimann, J.J. Zach, T.Rauscher, J.V. Schwarzenberg, P. Tischhauser, and M.C. Wiescher, Nucl. Phys. A 652, (1999) 391.[29] S. Harissopulos, E. Skreti, P. Tsagari, G. Souliotis, P. Demetriou, T. Paradellis, J.W. Hammer, R.Kunz, C. Angulo, S. Goriely, and T. Rauscher, Phys. Rev. C 64, (2001) 055804.[30] T. Sauter and F. Käppeler, Phys. Rev. C 55, (1997) 3127.[31] J. Bork, H. Schatz, F. Käppeler, and T. Rauscher, Phys. Rev. C 58, (1998) 524.4PoS(NIC-IX)090Present status of the KADoNiS database Iris DillmannIsotope Reaction Eexp [MeV ] EGamow [MeV ] Reference EXFOR Entry58Ni (p,γ) 1.32 - 2.74 1.14 - 3.22 [16] A069658Ni (p,γ) 1.00 - 4.91 1.14 - 3.22 [17] C088658Ni (p,γ) 0.51 - 3.09 1.14 - 3.22 [18] A004858Ni (p,γ) 1.14 - 4.09 1.14 - 3.22 [19] A031160Ni (p,γ) 0.61 - 2.94 1.14 - 3.22 [18] A004861Ni (p,γ) 1.11 - 2.94 1.14 - 3.22 [18] A004864Ni (p,γ) 1.11 - 2.94 1.14 - 3.22 [20] A019863Cu (p,γ) 1.11 - 4.69 1.17 - 3.29 [20] A019863Cu (p,γ) 1.99 - 4.52 1.17 - 3.29 [21] C073965Cu (p,γ) 1.03 - 3.22 1.17 - 3.29 [20] A019865Cu (p,γ) 1.99 - 4.52 1.17 - 3.29 [21] C073964Zn (p,γ) 1.47 - 2.73 1.21 - 3.35 [18] A004867Zn (p,γ) 1.47 - 2.92 1.21 - 3.35 [18] A004868Zn (p,γ) 1.67 - 4.97 1.21 - 3.35 [22] C065074Se (p,γ) 1.60 - 3.00 1.34 - 3.61 [18] A004874Se (p,γ) 1.46 - 3.55 1.34 - 3.61 [23] O084976Se (p,γ) 1.46 - 3.55 1.34 - 3.61 [23] O084977Se (p,γ) 1.55 - 2.97 1.34 - 3.61 [18] A004884Sr (p,γ) 1.67 - 2.96 1.47 - 3.85 [24] A042686Sr (p,γ) 1.48 - 2.96 1.47 - 3.85 [24] A042687Sr (p,γ) 1.58 - 2.96 1.47 - 3.85 [24] A042688Sr (p,γ) 1.38 - 4.94 1.47 - 3.85 [25] O105489Y (p,γ) 1.76 - 4.83 1.51 - 3.91 [26] O118290Zr (p,γ) 1.97 - 5.70 1.54 - 3.97 [27]96Zr (p,γ) 3.50 - 6.00 1.54 - 3.97 [28] C055693Nb (p,γ) 1.42 - 4.80 1.57 - 4.03 [29] O091892Mo (p,γ) 1.48 - 3.00 1.60 - 4.08 [30] A065394Mo (p,γ) 1.48 - 2.49 1.60 - 4.08 [30] A065395Mo (p,γ) 1.70 - 3.00 1.60 - 4.08 [30] A065398Mo (p,γ) 1.48 - 3.00 1.60 - 4.08 [30] A065396Ru (p,γ) 1.65 - 3.37 1.66 - 4.20 [31] A065498Ru (p,γ) 1.65 - 3.37 1.66 - 4.20 [31] A065499Ru (p,γ) 1.46 - 3.37 1.66 - 4.20 [31] A0654100Ru (p,γ) 1.46 - 3.37 1.66 - 4.20 [31] A0654104Ru (p,γ) 1.65 - 3.37 1.66 - 4.20 [31] A0654102Pd (p,γ) 2.53 - 4.17 1.72 - 4.31 [13] C0904112Sn (p,γ) 3.00 - 8.50 1.84 - 4.52 [28] C0556116Sn (p,γ) 2.63 - 4.18 1.84 - 4.52 [13] C0904119Sn (p,γ) 2.80 - 6.00 1.84 - 4.52 [28] C0556Table 2: List of (p,γ) reactions within the Gamow window (EGamow), which are included in the p-processlibrary.5

Present status of the KADoNiS database

Abstract

Similar works

Full text

Available Versions

CERN Document Server