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The \u3csup\u3e33\u3c/sup\u3eS(p,γ)\u3csup\u3e34\u3c/sup\u3eCl reaction in classical nova explosions
Authors
Vinzenz Bildstein
Shawn Bishop
+31 more
Lothar Buchmann
Alan A. Chen
Jason A. Clark
Catherine M. Deibel
Brent Delbridge
Katrin Eppinger
Thomas Faestermann
Jennifer Fallis
Blake Freeman
Brian Fulton
Alejandro García
Uwe Greife
Bing Guo
Ulrike Hager
Clemens Herlitzius
Ralf Hertenberger
David Hutcheon
Andreas Knecht
Reiner Krüken
Alison Laird
Olga Lepyoshkina
Er Tao Li
Peter Maierbeck
Dave Ottewell
Anuj Parikh
Chris Ruiz
Anne Sallaska
Dominik Seiler
Kathrin Wimmer
Hans Friedrich Wirth
Chris Wrede
Publication date
1 December 2010
Publisher
LSU Digital Commons
Abstract
The analysis of microscopic grains within primitive meteorites has revealed isotopic ratios largely characteristic of the conditions thought to prevail in various astrophysical environments. Recently, several grains have been identified with isotopic signatures similar to those predicted within the ejecta of nova explosions on oxygen-neon white dwarfs. A possible smoking gun for a grain of nova origin is a large 33S abundance: nucleosynthesis calculations predict as much as 150 times the solar abundance of 33S in the ejecta of oxygen-neon novae. This overproduction factor may, however, vary by factors of at least 0.01 - 3 because of uncertainties in the 33S(p,γ)34Cl reaction rate over nova temperatures. In addition, better knowledge of this rate would help with the interpretation of nova observations over the S-Ca mass region, and contribute towards the firm establishment of a nucleosynthetic endpoint in these phenomena. Finally, constraining this rate may help to finally confirm or rule out the decay of an isomeric state of 34Cl (Ex = 146 keV, t1/2 =32 min) as a source for observable gamma-rays from novae. Direct examinations of the 33S(p,γ)34Cl reaction in the past have only identified resonances down to Er = 434 keV. At nova temperatures, lower-lying resonances could certainly play a dominant role. Several recent, complementary studies dedicated to improving our knowledge of the 33S(p,γ)34Cl rate, using both indirect methods (measurement of the 34S( 3He,t)34Cl and 33S(3He,d) 34Cl reactions with the Munich Q3D spectrograph) and direct methods (in normal kinematics at CENPA, University of Washington, and in inverse kinematics with the DRAGON recoil mass separator at TRIUMF) are presented here. Our results affect predictions of sulphur isotopic ratios in nova ejecta (e.g. 32S/33S) that may be used as diagnostic tools for the nova paternity of grains. © ?Copyright owned by the author(s)
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Last time updated on 26/10/2023