The distribution and properties of very young stellar systems
| Název práce v češtině: | The distribution and properties of very young stellar systems |
|---|---|
| Název v anglickém jazyce: | The distribution and properties of very young stellar systems |
| Akademický rok vypsání: | 2024/2025 |
| Typ práce: | disertační práce |
| Jazyk práce: | čeština |
| Ústav: | Astronomický ústav UK (32-AUUK) |
| Vedoucí / školitel: | prof. RNDr. Pavel Kroupa, Ph.D. |
| Řešitel: |
| Zásady pro vypracování |
| The student will read the bibliography and will discuss it with the supervisor (P. Kroupa) and collaborators (notably Tereza Jerabkova). This should take about six months. I am leaving the exact description of the topic somewhat open for now, because the student will need to iterate on a precise research problem to work on, depending on the students particular interests. The student will then begin the research work which will include the installation of a suitable simulation programme, such as Aarseth's Nbody6 or 7 and/or the AMUSE package, and the GalIMF code developed in Prague. After coming to know how to employ these programmes and after writing the initialisation and data reduction programmes, the numerical experiments will be begun. The topics to be studied will range from the properties of exo-planetary systems to the evolution of star clusters in the Galaxy using the Nbody6/7 and/or AMUSE packages, and research on the star-cluster- and stellar-populations of galaxies using the GalIMF code. After the second year, at least one research publication should be submitted. Depending on progress and any possible new research problems that may come up, the third year should end with at least a second research publication being submitted. Thereafter the thesis preparation can begin. During this process, the student will need to fulfil the formal obligations of the PhD programme at the Astronomical Institute which includes attending a number of lectures, taking the exams and also doing the state exam.
|
| Seznam odborné literatury |
| The student should read the following papers:
https://ui.adsabs.harvard.edu/abs/1999PASP..111.1333A/abstract From NBODY1 to NBODY6: The Growth of an Industry https://ui.adsabs.harvard.edu/abs/2018araa.book.....P/abstract Astrophysical Recipes; The art of AMUSE https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.4418J/abstract A stellar relic filament in the Orion star-forming region https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.2205B/abstract Uncovering a 260 pc wide, 35-Myr-old filamentary relic of star formation https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.5652K/abstract Very high redshift quasars and the rapid emergence of supermassive black holes https://ui.adsabs.harvard.edu/abs/2017A%26A...608A..53J/abstract The formation of ultra compact dwarf galaxies and massive globular clusters. Quasar-like objects to test for a variable stellar initial mass function https://ui.adsabs.harvard.edu/abs/2018A%26A...620A..39J/abstract Impact of metallicity and star formation rate on the time-dependent, galaxy-wide stellar initial mass function https://ui.adsabs.harvard.edu/abs/2020A%26A...637A..68Y/abstract Chemical evolution of ultra-faint dwarf galaxies in the self-consistently calculated integrated galactic IMF theory https://ui.adsabs.harvard.edu/abs/2019A%26A...632A.110Y/abstract The star formation timescale of elliptical galaxies. Fitting [Mg/Fe] and total metallicity simultaneously https://ui.adsabs.harvard.edu/abs/2019A%26A...629A..93Y/abstract Chemical evolution of elliptical galaxies with a variable IMF. A publicly available code https://ui.adsabs.harvard.edu/abs/2017A%26A...607A.126Y/abstract The optimally sampled galaxy-wide stellar initial mass function. Observational tests and the publicly available GalIMF code |