Velocity and Density Spectra of the Small Magellanic Cloud

By S. Stanimirović, A. Lazarian. 2001

134 citations recorded by the source corpus.

This Letter reports results on the statistical analysis of H I turbulence in the Small Magellanic Cloud (SMC). We use 21 cm channel maps, obtained with the Australia Telescope Compact Array and the Parkes telescope, and analyze the spectrum of observed intensity fluctuations as a function of the velocity slice thickness. We confirm recent predictions by Lazarian & Pogosyan on the change of the power-law index and establish the spectra of three-dimensional density and velocity. The obtained spectral indices, -3.3 and -3.4, are slightly more shallow than the predictions for the Kolmogorov spectrum. This contrasts with the predictions for the shock-type spectra that are steeper than the Kolmogorov one. The nature of the energy injection in the SMC is unclear, as no distinct energy injection scales are observed up to the entire scale of the SMC.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ce2136dfff5689457871cc7551442f0b3ad9b03f

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Citations in the corpus

WHAT IS DRIVING THE H i VELOCITY DISPERSION? (2009, background): “In these two cases, the gas turbulence cannot be explained by SNe (cf. Stanimirović & Lazarian 2001; Dib & Burkert 2005; Pasquali et al. 2008); still, the MRI could account for the observed regime of turbulence.”
Science with ASKAP (2008, background): “Observationally, the signature of turbulence has been detected in molecular clouds ([48] and references therein), H ii regions [145] and H i features [6, 197, 249] on scales ranging from AU to kpc.”
Interstellar Turbulence I: Observations and Processes (2004, unknown): “This blending effect has been studied and substantially confirmed in a number of observations (Dickey et al. 2001, Stanimirovic & Lazarian 2001) and simulations (Ballesteros-Paredes, Vázquez-Semadeni & Scalo 1999; Pichardo et al. 2000; Lazarian et al. 2001; Esquivel et al. 2003).”
DENSITY STUDIES OF MHD INTERSTELLAR TURBULENCE: STATISTICAL MOMENTS, CORRELATIONS AND BISPECTRUM (2008, methodology): “The power spectrum has been used in numerous papers to analyze observations, (see Armstrong, Rickett, & Spangler 1995; Stanimirovic et al. 1999; Stanimirovic & Lazarian 2001).”
Simulations of Magnetohydrodynamic Turbulence in a Strongly Magnetized Medium (2001, result): “Incidentally, recent studies of turbulence of HI in both our Galaxy and SMC (Lazarian 1999, Lazarian & Pogosyan 2000, Stanimirovic & Lazarian 2001) show the spectra of velocity and density consistent with the Kolmogorov scalings6.”
A New Look at the Kinematics of Neutral Hydrogen in the Small Magellanic Cloud (2003, background): “As a dwarf irregular galaxy, the SMC is different from our own Galaxy in many respects, having a lower heavyelement abundance, significantly lower dust content, and a consequently stronger interstellar radiation field (Stanimirović et al. 1999; Stanimirović & Lazarian 2001).”