HUSCAP logo Hokkaido Univ. logo

Hokkaido University Collection of Scholarly and Academic Papers >
Graduate School of Science / Faculty of Science >
Peer-reviewed Journal Articles, etc >

Dense cloud formation and star formation in a barred galaxy

Files in This Item:
MNRAS-2013-Nimori-2175-82-1.pdf1.68 MBPDFView/Open
Please use this identifier to cite or link to this item:

Title: Dense cloud formation and star formation in a barred galaxy
Authors: Nimori, M. Browse this author
Habe, A. Browse this author →KAKEN DB
Sorai, K. Browse this author
Watanabe, Y. Browse this author
Hirota, A. Browse this author
Namekata, D. Browse this author
Keywords: ISM: clouds
galaxies: ISM
galaxies: kinematics and dynamics
galaxies: star formation
galaxies: structure
Issue Date: 21-Dec-2012
Publisher: The Royal Astronomical Society (Oxford University Press)
Journal Title: Monthly Notices of the Royal Astronomical Society
Volume: 429
Start Page: 2175
End Page: 2182
Publisher DOI: 10.1093/mnras/sts487
Abstract: We investigate the properties of massive, dense clouds formed in a barred galaxy and their possible relation to star formation, performing a two-dimensional hydrodynamical simulation with the gravitational potential obtained from the 2MASS data from the barred spiral galaxy, M83. Since the environment for cloud formation and evolution in the bar region is expected to be different from that in the spiral arm region, barred galaxies are a good target to study the environmental effects on cloud formation and the subsequent star formation. Our simulation uses for an initial 80 Myr isothermal flow of non-self gravitating gas in the barred potential, then including radiative cooling, heating and self-gravitation of the gas for the next 40 Myr, during which dense clumps are formed. We identify many cold, dense gas clumps for which the mass is more than 10(4) M-circle dot (a value corresponding to the molecular clouds) and study the physical properties of these clumps. The relation of the velocity dispersion of the identified clump's internal motion with the clump size is similar to that observed in the molecular clouds of our Galaxy. We find that the virial parameters for clumps in the bar region are larger than that in the spiral arm region. From our numerical results, we estimate star formation in the bar and spiral arm regions by applying the simple model of Krumholz & McKee (2005). The mean relation between star formation rate and gas surface density agrees well with the observed Kennicutt-Schmidt relation. The star formation efficiency in the bar region is similar to 60 per cent of the spiral arm region. This trend is consistent with observations of barred galaxies.
Description: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 The Authors Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved.
Type: article
Appears in Collections:理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)

Submitter: 羽部 朝男

Export metadata:

OAI-PMH ( junii2 , jpcoar_1.0 )

MathJax is now OFF:


 - Hokkaido University