Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (47) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (2)
· Associated Articles
· Also-Read Articles (Reads History)
· Translate This Page
Effects of magnetic fields and rotation on the fragmentation of filamentary molecular clouds - Comparison of the theory with the Orion A cloud [ Erratum: 1993ApJ...412L..75H ]
Hanawa, Tomoyuki; Nakamura, Fumitaka; Matsumoto, Tomoaki; Nakano, Takenori; Tatematsu, Ken'ichi; Umemoto, Tomofumi; Kameya, Osamu; Hirano, Naomi; Hasegawa, Tetsuo; Kaifu, Norio; Yamamoto, Satoshi
AA(Nagoya Univ., Japan), AB(Nagoya Univ., Japan), AC(Nagoya Univ., Japan), AD(Nobeyama Radio Observatory, Minamimaki, Japan), AE(Nobeyama Radio Observatory, Minamimaki, Japan), AF(Nobeyama Radio Observatory, Minamimaki, Japan), AG(National Astronomical Observatory, Mizusawa, Japan), AH(Hitotsubashi Univ., Kunitachi, Japan), AI(Tokyo Univ., Mitaka, Japan), AJ(National Astronomical Observatory, Mitaka, Japan)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 404, no. 2, p. L83-L86. (ApJL Homepage)
Publication Date:
NASA/STI Keywords:
Fragmentation, H Ii Regions, Interstellar Magnetic Fields, Magnetohydrodynamic Stability, Molecular Clouds, Rotation, Carbon Monoxide, Emission Spectra, Line Spectra
Bibliographic Code:


We discuss the fragmentation of a filamentary molecular cloud on the basis of a magnetohydrodynamical stability analysis and the observations of the Orion A cloud with the Nobeyama 45 m telescope. Our model cloud has axial and helical magnetic fields and rotates around the axis. The dispersion relation for this cloud shows that the presence of a magnetic field and/or rotation shortens the wavelength of the most unstable mode, i.e., the mean distance between the adjacent fragments, measured in units of the filament diameter. We compare the theoretical results with the observed clumpy structure of the filamentary Orion A cloud and find that the sum of magnetic and centrifugal forces in the parent cloud was comparable with the pressure force (thermal and turbulent) and has had significant effects on the fragmentation. The rotation velocity of the filament measured in the (C-13)O emission line is consistent with this result.

Associated Articles

Main Paper     Erratum    

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints