Ph.D. University of Mainz, Germany , 2000
I received my Diploma in
Physics in 1997 and my Ph.D. in Astrophysics in 2000 from the
University of Mainz (Group of Prof.
). For my thesis I performed experiments at
IGISOl (Jyväskylä) and CERN/ISOLDE (Geneva) to determine decay
properties of neutron-rich Mn, Ag, and Cd isotopes (with the
aid of the laser ion-source RILIS). The emphasis was put on
the identification of new nuclei in the region of the
subshell/shell closures N=40 and 82, on the one hand to gain
understanding in nuclear structure and on the other hand to
obtain the best possible data (and support for theoretical
extrapolations) to be employed in astrophysical applications.
The astrophysical r-process (rapid neutron capture) involves
nuclei from the line of beta-stability to the neutron
drip-line. Data around shell closures are especially important
in order to understand the behavior of shell effects as a
function of distance from stability.
University of Mainz, 2000 - 2002
I was involved in
collaboration with the European Southern Observatory in the
project ”The First Stars and the Origin of the Elements”. The
specific aim of this project was to measure, with
unprecedented accuracy, the abundance distribution of key
elements in representative sample of second-generation stars.
First results let to a element-consistent picture of CS
22892-052, caused by improved nuclear-data input and new
observations of 15 rare earth elements and of Os and Ir in the
third r-abundance peak. We could obtain a new value for it’s
age of 14.6 +/- 2.4 Gyr, what is a lower limit for the age of
our galaxy, and it was possible to predict a 238U abundance of
log ~ -2.5 +/- 0.1 for this star.
Postdoc Subaru Telescope,
Hilo, Hawaii, 2003 - 2006
working in the field of nuclear astrophysics and used
SUBARU's High Resolution Spectrograph to obtain high
resolution spectra of prospective r-process-enhanced
metal-poor targets to shed light on a variety of
♦ What is the frequency of the enhancement
phenomenon as a function of [Fe/H]?
♦ What is the distribution of the level of
enhancement – e.g. is it bi-modal or continuous?
♦ With what precision is the solar
r-process pattern reproduced from star to star?
♦ How common is the so-called “actinide boost”
problem, where the measured abundance of Th appears up
to 0.4 dex higher than predicted by theory ?
♦ Is there a type of incomplete r-process in
some early progenitors, or was there a time delay before
the major r-process sites could evolve?
♦ Why was the production of the lighter
n-capture elements favored over the heavier such
elements in some stars?
♦ At what metallicity and/or time did the first
main r-process sites come into existence?
♦ What is (are) the astrophysical site(s) of
the r-process ?
Research Engineer, CEA,
Saclay, France 2007-2009
I worked in the EDELWEISS
Project at CEA Saclay (France). The EDELWEISS
experiment is dedicated to the direct detection of dark
matter particles with bolometric detectors located at the
underground laboratory of Modane (the LSM). The stage II of
this experiment is currently running and taking data.
Cryogenic Germanium-Detectors are employed at 17 mK while
temperature and charge of the WIMP event are registered.
Hawaii, Honolulu, 2009 - 2010
ANITA-Projet @ UH
Physics, Kauai Community College 2010 -