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VERSION:2.0
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METHOD:PUBLISH
BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20091112T000000
DTEND;TZID=Atlantic/Canary:20091112T010000
UID:iactalks-112
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/112
CREATED:2009-11-12T00:00:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Rubidium-rich asymptotic giant branch stars in the Magellanic Cloud
 s
DESCRIPTION:Rubidium-rich asymptotic giant branch stars in the Magellanic C
 louds\nDr. Aníbal García Hernández\n\nAsymptotic Giant Branch (AGB) sta
 rs are a principal source of gas and dust input into the interstellar medi
 um, being an important driver of chemical evolution in galaxies. Rubidium 
 is a key element to distinguish between high mass (~4-8 M⊙) AGB star
 s and low mass (~1-4 M⊙) AGBs - high mass AGBs are predicted to prod
 uce a lot of rubidium as a consequence of the genuine nucleosynthetic proc
 esses (the s-process) that characterise these stars. The Magellanic Clouds
  (MCs) offer a unique opportunity to study the stellar evolution and nucle
 osynthesis of AGB stars in low metallicity environments where distances (a
 nd so the star's luminosity) are known. We present the discovery of extrag
 alactic rubidium-rich AGB stars in the MCs confirming that the more massiv
 e AGB stars are generally brighter than the standard adopted luminosity li
 mit (Mbol~-7.1) for AGB's. In addition, massive MC-AGBs are more enriched 
 in Rb than their galactic counterparts, as it is qualitatively predicted b
 y the present theoretical models; the Rb over-abundance increase with incr
 easing stellar mass and with decreasing metallicity. However, present theo
 retical models are far from matching the extremely high Rb overabundances 
 observed.
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