Speaker
Dr
Jenny Feige
(Berlin Institute of Technology)
Description
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{\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy}
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\TITLE{Limits on $^{60}$Fe/$^{26}$Al nucleosynthesis ratios from deep-sea sediment AMS measurements}\\[3mm]
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\AUTHORS{J. Feige$^{1,2}$, A. Wallner$^{2,3}$, L.~K. Fifield$^3$, R. Golser$^2$, S. Merchel$^4$, G. Rugel$^4$, P. Steier$^2$,\\ S.~G. Tims$^3$, S.~R. Winkler$^{2,5}$}
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\AFFILIATION{1}{Department of Astronomy and Astrophysics, Berlin Institute of Technology, Berlin, Germany}
\AFFILIATION{2}{University of Vienna, Faculty of Physics - Isotope Research and Nuclear Physics, Vienna, Austria}
\AFFILIATION{3}{Department of Nuclear Physics, The Australian National University, Canberra, Australia}
\AFFILIATION{4}{Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany}
\AFFILIATION{5}{iThemba LABS, Somerset West, South Africa}
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\centerline{Contact email: {\it feige@astro.physik.tu-berlin.de}}
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The long-lived radionuclide $^{26}$Al (t$_{1/2}$\,=\,0.7\,Myr) has been observed throughout our galaxy, reflecting ongoing nucleosynthesis over the past few million years [1]. It is produced and ejected into the interstellar medium by stellar winds and during supernova explosions. A nearby supernova may leave an imprint of $^{26}$Al in terrestrial archives, complementing the observation of supernova-produced $^{60}$Fe in deep-sea samples. \\
The same set of sediment samples from the Indian Ocean that showed a distinct $^{60}$Fe-signature in layers of ages between 1.7 and 3.2\,Myr [2] was also analyzed for $^{26}$Al. However, additional terrestrial sources producing $^{26}$Al on Earth, such as cosmogenic production in the atmosphere and in-situ production within the sediment, may obscure a supernova imprint. \\
We used our experimental $^{26}$Al data to infer lower limits on $^{60}$Fe/$^{26}$Al nucleosynthesis ratios by comparing the width and the strength of the previously measured $^{60}$Fe-signal to our $^{26}$Al data. We find that our results
generally favour the higher theoretical isotopic supernova ratios and deviate from the observed galactic $^{60}$Fe/$^{26}$Al flux ratio by 2-3 times of the measurement uncertainty.
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\noindent [1] Diehl et al., New Astron. Rev., 52, 440 (2008);
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[2] Wallner, Feige et al., Nature, 532, 69 (2016).}
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Primary author
Dr
Jenny Feige
(Berlin Institute of Technology)
