Magnetic Fields in Sh2-29

It is well known that a large-scale magnetic field structure pervades the disk of the Milky Way, including molecular clouds and star-forming regions. It is possible that the presence of these magnetic field lines plays an important role in the initial stages of star-forming processes, providing support against molecular cloud contraction. However, there is no general consensus on whether these fields are important for the formation of sub- structures such as interstellar filaments, dense cores, and stars. On one hand, if magnetic fields are dynamically effective in this kind of environment, then star formation is probably regulated by the process known as ambipolar diffusion, or by the diffusion processes related to magnetic reconnection. On the other hand, if magnetic fields do not have a very important role on these regions, then other effects, such as turbulence and stellar winds, must provide support against the collapse of molecular clouds.

Furthermore, in later stages, there is clearly a very dynamic interaction between the newborn embedded stellar populations and their surrounding interstellar medium. This interaction significantly affects the morphology of gas and dust structures through radiation pressure and strong stellar winds, especially toward sites of massive star formation. Since the magnetic field is generally frozen within the interstellar gas, its lines are also critically affected in this process.

In this work, we have used multi-band polarimetric data (V, R, I, and H) toward Sh 2-29 in order to study properties from the interstellar magnetic field lines, as well as the size distribution of dust particles.

Related Publication: https://iopscience.iop.org/article/10.1088/0004-637X/783/1/1