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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20160621T123000
DTEND;TZID=Atlantic/Canary:20160621T133000
UID:iactalks-932
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/932
CREATED:2016-06-21T12:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Formation history of old open clusters constrained by detailed aste
 roseismic analysis of red giant stars observed by Kepler
DESCRIPTION:Formation history of old open clusters constrained by detailed 
 asteroseismic analysis of red giant stars observed by Kepler\nDr. Enrico C
 orsaro\n\nStars originate by the gravitational collapse of a turbulent mol
 ecular cloud of a diffuse medium, and are often observed to form clusters.
  Stellar clusters therefore play an important role in our understanding of
  star formation and of the dynamical processes at play. However, investiga
 ting the cluster formation is difficult because the density of the molecul
 ar cloud undergoes a change of many orders of magnitude. Hierarchical-step
  approaches to decompose the problem into different stages are therefore r
 equired, as well as reliable assumptions on the initial conditions in the 
 clouds. In this talk I will report for the first time the use of the full 
 potential of NASA Kepler asteroseismic observations coupled with 3D numeri
 cal simulations, to put strong constraints on the early formation stages o
 f old open clusters. Thanks to a Bayesian peak bagging analysis of about 5
 0 red giant members of NGC 6791 and NGC 6819, the two most populated open 
 clusters observed in the nominal Kepler mission, I derive a complete set o
 f detailed oscillation mode properties for each star, with thousands of os
 cillation modes characterized. I therefore show how these asteroseismic pr
 operties lead to a discovery about the rotation history of stellar cluster
 s. Finally, the observational findings will be compared with hydrodynamica
 l simulations for stellar cluster formation to constrain the physical proc
 esses of turbulence, rotation, and magnetic fields that are in action duri
 ng the collapse of the progenitor cloud into a proto-cluster.
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