Feathering Instability of Spiral Arms and OB Star Formation

Details Feathering Instability of Spiral Arms and OB Star Formation Feathering Instability of Spiral Arms and OB Star Formation

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21944109l&link_type=abstract

American Astronomical Society, AAS Meeting #219, #441.09

Astronomy and Astrophysics

Astronomy

Galaxies: Ism, Structure, Instabilities, Ism: Kinematics And Dynamics, Ism: Magnetic Fields

Scientific paper

Quasi-regular substructures of the spiral arm are commonly found in spiral galaxies. These substructures are known as feathers or spurs, and they jut out perpendicularly into the inter-arm region. They also associate with the Giant Molecular Clouds where massive star formation occurs. The formation of these density fluctuation can be studied from the perspective of perturbation of galactic spiral shock. We investigate the gas response under the influcence of the shock perturbation, and formulate the MHD equations in a local two-dimensional quasi-rectangular region between tightly-winding spiral arms. Our theoretical model includes the effect of magnetic field and self-gravity of the gas, we are able to reproduce feather-like structures in the post-shock region. In this semi-analytical framework, the periodic density fluctuations depends on the various background parameters such as pattern speed, strength of spiral arm, surface density of the gas and strength of magnetic field. Potentially this study can help understand the inter-arm environment that will be observed in the nearby galaxies using submillimeter telescope such ALMA in the coming years.

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