Universität Wien FIND

280513 VU PM-Astr Cosmic chemical evolution (PI) (2019W)

Continuous assessment of course work

Registration/Deregistration

Details

max. 25 participants
Language: English

Lecturers

Classes (iCal) - next class is marked with N

starting lecture on Oct. 1st

Tuesday 01.10. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 08.10. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 22.10. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 29.10. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 05.11. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 12.11. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 19.11. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 26.11. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 03.12. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 10.12. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 17.12. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 07.01. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 14.01. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 21.01. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17
Tuesday 28.01. 15:00 - 16:30 Seminarraum 1 Astronomie Sternwarte, Türkenschanzstraße 17

Information

Aims, contents and method of the course

Since shortly after the Big Bang only H, He, and a few lighter elements were produced, the further production of heavier elements in the stellar interior is responsible for the present-day element abundances. By means of stellar evolutionary models the nucleosynthesis of elements can be understood. Their release by various stellar mass-loss processes enrich the interstellar medium in its gas phases differently by these elements. The timescales and quantities of element enrichment and gasdynamical influences as well determine element abundances and abundance ratios, which can both be observed in stars of different ages e.g. in the Milky Way and nearby galaxies. With dynamical models only chemical signatures can provide a detailed insight into galaxy evolution.

Assessment and permitted materials

Selected topics from the literature on nucleosynthesis, stellar mass loss, and galaxy evolution will be prepared by the students and presented to the participants.

Minimum requirements and assessment criteria

Continuous attendance, one presentation at least, and lively participation.

Examination topics

Reading list

will be provided in the lecture

Association in the course directory

Last modified: Fr 27.09.2019 08:48