Global Modeling of Spur Formation in Spiral Galaxies

Details Global Modeling of Spur Formation in Spiral Galaxies Global Modeling of Spur Formation in Spiral Galaxies

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20040o&link_type=abstract

Spitzer Proposal ID #20040

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Scientific paper

Spitzer 8 micron Legacy images of M51 and other SINGS galaxies show, in addition to the classic ``beads on a string'' associated with localized star formation, striking intermediate-scale filamentary structures. These features consist of many trailing ``spurs'' extending from the main arms well into the interarm regions. Cospatial ``spur-like'' dust lanes are also evident in HST optical images of M51 and other disk galaxies -- including barred and flocculent types -- suggesting that a similar dynamical process drives their development in many systems. We believe that these spurs are created by the magneto-Jeans instability (MJI), and that nonlinear evolution of the MJI leads to fragmentation into GMCs, and subsequently arm and interarm HII regions. In previous MHD simulations using a simplified local model, the PI demonstrated the formation of gaseous spurs and bound clouds with masses and spacings similar to observations. We propose to extend these models into the global domain, which will allow for realistic effects including curvature of spiral arms, spatial variation of the background surface density, and gradients in the background flow velocity relative to the spiral pattern. In addition to modeling tuned for specific galaxies, we also plan to perform a larger survey to explore the parameter dependence of structural and dynamical development. Since much of the arm and interarm 8 micron emission is produced by PAHs in dusty clumps and filaments, and star formation may be driven by the corresponding gas enhancements, understanding how the ISM is concentrated into these structures may be key to interpretation of many existing and future Spitzer data sets.

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