Hostname: page-component-586b7cd67f-r5fsc Total loading time: 0 Render date: 2024-11-29T03:36:34.118Z Has data issue: false hasContentIssue false
  • English
  • Français

The evolution of the spiral galaxy M51a

Published online by Cambridge University Press:  17 August 2016

Xiaoyu Kang ,
Fenghui Zhang  and
Ruixiang Chang
Xiaoyu Kang
Affiliation:
Yunnan Observatories, CAS, Kunming, 650011, China email: [email protected] Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, China University of Chinese Academy of Sciences, Beijing, 100049, China
Fenghui Zhang
Affiliation:
Yunnan Observatories, CAS, Kunming, 650011, China email: [email protected] Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, China
Ruixiang Chang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A simple model for M51a is constructed to explore its evolutionary history by assuming its disk grows from continuous gas infall, which is shaped by a free parameter-the infall-peak time tp. By adopting a constant infall-peak time tp = 7.0Gyr, our model predictions can reproduce most of the observed constraints and still show that the disk of M51a forms inside-out. Our results also show that the current molecular gas surface density, the star-formation rate and the UV-band surface brightness are important quantities to trace the effect of recent interactions on galactic star-formation process.

Keywords

galaxies: abundancegalaxies: evolutiongalaxies: individual: M51agalaxies: spiral
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S319: Galaxies at High Redshift and Their Evolution Over Cosmic Time , August 2015 , pp. 129
Copyright
Copyright © International Astronomical Union 2016 

References

Kang, X., Chang, R., Zhang, F., Cheng, L., & Wang, L. 2015, MNRAS, 449, 414 CrossRefGoogle Scholar