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Kyle M. Walker et al. 2009 ApJ 706 614 doi:10.1088/0004-637X/706/1/614

RUBIDIUM IN THE INTERSTELLAR MEDIUM

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Kyle M. Walker1,5, S. R. Federman1,5, David C. Knauth2,3,6 and David L. Lambert4

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Abstract References

We present observations of interstellar rubidium toward o Per, ζ Per, AE Aur, HD 147889, χ Oph, ζ Oph, and 20 Aql. Theory suggests that stable 85Rb and long-lived 87Rb are produced predominantly by high-mass stars, through a combination of the weak s- and r-processes. The 85Rb/87Rb ratio was determined from measurements of the Rb I line at 7800 Å and was compared to the solar system meteoritic ratio of 2.59. Within 1σ uncertainties, all directions except HD 147889 have Rb isotope ratios consistent with the solar system value. The ratio toward HD 147889 is much lower than the meteoritic value and similar to that toward ρ Oph A; both lines of sight probe the Rho Ophiuchus Molecular Cloud. The earlier result was attributed to a deficit of r-processed 85Rb. Our larger sample suggests instead that 87Rb is enhanced in these two lines of sight. When the total elemental abundance of Rb is compared to the K elemental abundance, the interstellar Rb/K ratio is significantly lower than the meteoritic ratio for all the sight lines in this study. Available interstellar samples for other s- and r- process elements are used to help interpret these results.


Keywords

ISM: abundances; ISM: atoms; stars: individual (omicron Persei, zeta Persei, AE Aurigae, HD 147889, chi Ophiuchi, zeta Ophiuchi, 20 Aquilae)


Dates

Issue 1 (2009 November 20)

Received 2009 January 2, accepted for publication 2009 October 6

Published 2009 November 3



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