Propagation of star formation at sub-kiloparsec scales
| Autor: | E. V. Shimanovskaya, Alexander S. Gusev |
|---|---|
| Rok vydání: | 2019 |
| Předmět: |
Physics
Range (particle radiation) 010308 nuclear & particles physics Star formation Turbulence FOS: Physical sciences Astronomy and Astrophysics Scale (descriptive set theory) Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Astrophysics - Astrophysics of Galaxies 01 natural sciences Galaxy Supernova Star cluster Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) 0103 physical sciences Cluster (physics) Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 488:3045-3054 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stz1881 |
| Popis: | We study the propagation of star formation based on the investigation of the separation of young star clusters from HII regions nearest to them. The relation between the separation and U-B colour index (or age) of a star cluster was found. The average age of star clusters increases with the separation as the 1.0-1.2 power in the separation range from 40 to 200 pc and as the 0.4-0.9 power in the range of 100-500 pc in the galaxies with symmetric morphology. The galaxies with distorted asymmetric disc structure show more complex and steeper (power >1.2 at separations from 40 to 500 pc) dependence between the age and the separation. Our results confirm the findings of previous studies on the dominant role of turbulence in propagation of the star formation process on spatial scales up to 500 pc and on time scales up to 300 Myr. On a smaller scale (= 10 pages, 13 figures, 2 tables. Accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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