期刊
ASTROPHYSICAL JOURNAL
卷 810, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/810/1/33
关键词
ISM: structure; Local Group; magnetohydrodynamics (MHD); turbulence
资金
- NASA Einstein Fellowship
- Center for Magnetic Self-Organization in Astrophysical
- Center for Magnetic Self-Organization in Laboratory Plasmas
- NSF [AST 1212096, AST-1056780]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1212096] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [0821899] Funding Source: National Science Foundation
We present the results of the Velocity Coordinate Spectrum (VCS) technique to calculate the velocity power spectrum of turbulence in the Small Magellanic Cloud (SMC) in 21 cm emission. We present an updated version of the VCS technique that takes into account regular motions, which is an important factor in our SMC VCS analysis. We have obtained a velocity spectral index of -3.85, a cold phase sonic Mach number of 5.6, and an injection scale of 2.3 kpc. The spectral index is steeper than the Kolmogorov index, which is expected for shock-dominated turbulence. The injection scale of 2.3 kpc suggests that HI supershells or tidal interactions with the Large Magellanic Cloud are the dominant drivers of turbulence in this dwarf galaxy. This implies that turbulence may be driven by multiple mechanisms in galaxies and that galaxy-galaxy interactions may play an important role in addition to supernova feedback.
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