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- Wouter Vlemmings
Argelander-Institut für Astronomie
Auf dem Hügel 71,
- wouter (at) astro.uni-bonn.de
- tel:+49 (0)228 733670
fax:+49 (0)228 731775
Current project include:
Massive star formation magnetic field database
The processes governing the formation of massive stars is still unknown, and magnetic fields potentially play a crucial role. However, observations of magnetic fields in these regions are few. In this project the student will work with recent Effelsberg and Parkes telescope methanol maser observations to determine the role of the magnetic field in a large sample (~80) high mass star forming regions.
Magnetism shaping planetary nebulae
Planetary Nebulae (PNe) are the descendents of stars with a similar mass to our Sun. While the progenitor stars are spherically symmetric, a large fraction of PNe have asymmetric shapes (only 20% of the PNe are spherical). The origin of these spectacular shapes is still a matter of debate, but mounting evidence points towards magnetic fields. This project will study the magnetic field around evolved stars that will become PNe using VLBI polarization observations of masers.
Non-Emmy Noether group related:
The birth sites of pulsars
Using VLBI observations it has been possible to accurately determine distances and sky velocities of pulsar, which are essential ingredients for a good understanding of the birth properties of these compact objects. Born from Supernova explosions, pulsars have long been known to reach extremely high space and rotational velocities and recent astrometric observations strongly suggest that significant kick velocities are imparted upon the pulsar birth. This project will use the current astrometric data taken using the VLBA for a number of pulsars to determine their likely orbits through the Galaxy and determine possible birth locations. This will not only allow for a determination of the spatial pulsar birth distribution but also provides crucial inputs in the study of the pulsar birth space velocity and initial spin velocity, which in turn are essential for accurate modeling of the Supernova core collapse processes.