Ulteriori informazioni
This book focuses on the stellar disk evolution and gas disk turbulence of the most numerous galaxies in the local Universe - the dwarf galaxies. The "outside-in" disk shrinking mode was established for a relatively large sample of dwarf galaxies for the first time, and this is in contrast to the "inside-out" disk growth mode found for spiral galaxies. Double exponential brightness profiles also correspond to double exponential stellar mass profiles for dwarf galaxies, which is again different from most spiral galaxies. The cool gas distribution in dwarf galaxies was probed with the spatial power spectra of hydrogen iodide (HI) gas emission, and provided indirect evidence that inner disks of dwarf galaxies have proportionally more cool gas than outer disks. The finding that no correlation exists between gas power spectral indices and star formation gave important constraints on the relation between turbulence and star formation in dwarf galaxies.
Sommario
Introduction.- Stellar Disk Evolution of Dwarf Irregular Galaxies.- Turbulence and Multiple Temperature Components of HI Gas in Dwarf Irregular Galaxies.- Nearby Major Mergers.
Info autore
Dr. Hong-Xin Zhang received his Ph.D. in Astrophysics from the University of Chinese Academy of Sciences in July 2012. His major research project was on the star formation history variations and the interstellar medium turbulence in nearby galaxies. Subsequently, he became a post-doc fellow working with Prof. Eric Peng at the Department of Astronomy, Peking University, focusing on studying the nature of Ultra-compact Dwarf Galaxies in the Virgo Cluster.
Riassunto
This book focuses on the stellar disk evolution and gas disk turbulence of the most numerous galaxies in the local Universe – the dwarf galaxies. The “outside-in” disk shrinking mode was established for a relatively large sample of dwarf galaxies for the first time, and this is in contrast to the “inside-out” disk growth mode found for spiral galaxies. Double exponential brightness profiles also correspond to double exponential stellar mass profiles for dwarf galaxies, which is again different from most spiral galaxies. The cool gas distribution in dwarf galaxies was probed with the spatial power spectra of hydrogen iodide (HI) gas emission, and provided indirect evidence that inner disks of dwarf galaxies have proportionally more cool gas than outer disks. The finding that no correlation exists between gas power spectral indices and star formation gave important constraints on the relation between turbulence and star formation in dwarf galaxies.
