Time-resolved interstellar Pu-244 and Fe-60 Ppofiles in a Be- 10 dated ferromanganese crust

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dc.contributor.authorKoll, Den_AU
dc.contributor.authorWallner, Aen_AU
dc.contributor.authorHotchkis, MACen_AU
dc.contributor.authorChild, DPen_AU
dc.contributor.authorFifield, LKen_AU
dc.contributor.authorFroehlich, MBen_AU
dc.contributor.authorHarnett, Men_AU
dc.contributor.authorLachner, Jen_AU
dc.contributor.authorMerchel, Sen_AU
dc.contributor.authorPavetich, Sen_AU
dc.contributor.authorRugel, Gen_AU
dc.contributor.authorSlavkovska, Zen_AU
dc.contributor.authorTims, SGen_AU
dc.date.accessioned2023-01-20T02:06:32Zen_AU
dc.date.available2023-01-20T02:06:32Zen_AU
dc.date.issued2021-11en_AU
dc.date.statistics2022-06-30en_AU
dc.description.abstractMore than 20 years have passed since the first attempts to find live supernova Fe-60 (t1/2 = 2.6 Myr) in a deep-sea ferromanganese crust [1]. Within these 20 years, strong evidence was presented for a global influx of supernova dust into several geological samples around 2 Myr ago. Recently, a much younger continuous influx was found in Antarctic snow and in deep-sea sediments [2-4] and an older peak around 7 Myr in deep-sea crusts [5,6]. The long-lived isotope Pu-244 (t1/2 = 80 Myr) is produced in the astrophysical r-process similarly to most of the heaviest elements. Although the production mechanism is believed to be understood, the astrophysical site is heavily disputed. Most likely scenarios involve a combination of rare supernovae and neutron star mergers. The search for Pu-244 signatures in samples with known Fe-60 signatures allows to test for either common influx patterns or independent Pu-244 influxes disentangled from stellar Fe-60. Accordingly, this information provides a unique and direct experimental approach for identifying the production site of the heavy elements. Very recently and first reported in the AMS-14 conference, the first detection of interstellar Pu-244 was published [6]. This was only feasible by achieving the highest detection efficiencies for plutonium in AMS ever reported [7]. The achieved time resolution of 4.5 Myr integrates over the supernova influxes and is therefore not high enough to unequivocally show a correlated influx pattern of Fe-60 and Pu-244. Based on this progress, we are now aiming to measure highly time-resolved profiles of Fe-60 and Pu-244 in the largest ferromanganese crust used so far. Results on the characterization of the crust including cosmogenic Be-10 (t1/2 = 1.4 Myr) dating and a 10 Myr profile of interstellar Fe-60 including the confirmation of the 7 Myr influx will be presented along with first data on interstellar Pu-244.en_AU
dc.identifier.citationKoll, D., Wallner, A., Hotchkis, M., Child, D., Fifield, K., Froehlich, M., Harnett, M., Lachner, J., Merchel, S., Pavetich, S., Rugel, G., Slavkovska, Z., & Tims, S., (2021). Time-resolved interstellar Pu-244 and Fe-60 Ppofiles in a Be- 10 dated ferromanganese crust. Paper presented to the 15th International Conference on Accelerator Mass Spectrometry. ANSTO Sydney, Australia. November 15th – 19th, 2021, (pp. 155). Retrieved from: https://ams15sydney.com/wp-content/uploads/2021/11/AMS-15-Full-Program-and-Abstract-Book-R-1.pdfen_AU
dc.identifier.conferenceenddate19 November 2021en_AU
dc.identifier.conferencename15th International Conference on Accelerator Mass Spectrometryen_AU
dc.identifier.conferenceplaceSydney, Australiaen_AU
dc.identifier.conferencestartdate15 November 2021en_AU
dc.identifier.pagination155en_AU
dc.identifier.urihttps://ams15sydney.com/wp-content/uploads/2021/11/AMS-15-Full-Program-and-Abstract-Book-R-1.pdfen_AU
dc.identifier.urihttps://apo.ansto.gov.au/dspace/handle/10238/14443en_AU
dc.language.isoenen_AU
dc.publisherAustralian Nuclear Science and Technology Organisationen_AU
dc.subjectInterstellar spaceen_AU
dc.subjectNova modelen_AU
dc.subjectDustsen_AU
dc.subjectPlutonium 244en_AU
dc.subjectIron 60en_AU
dc.subjectMass spectroscopyen_AU
dc.subjectCarbon 14en_AU
dc.titleTime-resolved interstellar Pu-244 and Fe-60 Ppofiles in a Be- 10 dated ferromanganese crusten_AU
dc.typeConference Abstracten_AU
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