C Domingo-Pardo et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014020 doi:10.1088/0954-3899/35/1/014020
C Domingo-Pardo1, U Abbondanno2, G Aerts3, H Álvarez4, F Alvarez-Velarde5, S Andriamonje3, J Andrzejewski6, P Assimakopoulos7, L Audouin3, G Badurek8, P Baumann9, F Bečvář10, E Berthoumieux3, S Bisterzo11, F Calviño12, M Calviani13, D Cano-Ott5, R Capote14,15, C Carrapiço16, P Cennini17, V Chepel18, N Colonna19, G Cortes12, A Couture20, J Cox20, M Dahlfors17, S David9, I Dillmann1, W Dridi3, I Duran4, C Eleftheriadis21, M Embid-Segura5, L Ferrant22, A Ferrari17, R Ferreira-Marques18, K Fujii2, W Furman23, R Gallino11, I Goncalves18, E Gonzalez-Romero5, F Gramegna13, C Guerrero5, F Gunsing3, B Haas24, R Haight25, M Heil1,26, A Herrera-Martinez17, M Igashira27, E Jericha8, Y Kadi17, F Käppeler1, D Karadimos7, D Karamanis7, M Kerveno9, P Koehler28, E Kossionides29, M Krtička10, C Lamboudis21, H Leeb8, A Lindote18, I Lopes18, M Lozano15, S Lukic9, J Marganiec6, S Marrone19, C Massimi30, P Mastinu13, A Mengoni14,17, P M Milazzo2, M Mosconi1, F Neves18, H Oberhummer8, S O'Brien20, J Pancin3, C Papachristodoulou7, C Papadopoulos31, C Paradela4, N Patronis7, A Pavlik9, P Pavlopoulos32, L Perrot3, M T Pigni8, R Plag1, A Plompen33, A Plukis3, A Poch12, C Pretel12, J Quesada15, T Rauscher34, R Reifarth25, C Rubbia35, G Rudolf9, P Rullhusen33, J Salgado16, C Santos16, L Sarchiapone17, I Savvidis21, C Stephan22, G Tagliente19, J L Tain36, L Tassan-Got22, L Tavora16, R Terlizzi19, G Vannini30, P Vaz16, A Ventura37, D Villamarin5, M C Vincente5, V Vlachoudis17, R Vlastou31, F Voss1, S Walter1, M Wiescher20 and K Wisshak1
Show affiliationsThe neutron capture cross section of 206Pb has been measured at the CERN n\TOF spectrometer using a setup of two C6D6 detectors. In the energy interval from 1 eV to 600 keV the cross section is dominated by resonances, which were analyzed via the R-matrix analysis code SAMMY. In the relevant energy ranges for stellar nucleosynthesis, i.e., at thermal energies of kT = 8 keV and kT = 23 keV, the present Maxwellian average cross section differs by 20% and 9% from the recommended values of Bao et al respectively. From the new cross section the s-abundance of 206Pb could be reliably determined as 70(4)%. This result is of importance in order to test and constrain r-process abundance calculations in the actinide region, because the r-process portion of 206Pb is dominated by α-back decays of short-lived transbismuth isotopes.
97.10.Cv Stellar structure, interiors, evolution, nucleosynthesis, ages
27.80.+w 190(less-than-or-equal-to)A(less-than-or-equal-to)219
Issue 1 (January 2008)
Received 29 June 2007
Published 13 December 2007
C Domingo-Pardo et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014020
Ashoke Sen JHEP05(2005)059
John M. Cannon et al. 2003 The Astronomical Journal 126 2806
H P Trautvetter et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014019
J Marganiec et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014022
Dale C. Jackson et al. 2004 The Astronomical Journal 128 1219
A Wallner et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014018
John A Sidles et al 2009 New J. Phys. 11 065002
C. W. Engelbracht et al 2006 ApJ 642 L127
Daniel R. Weisz et al. 2008 ApJ 689 160