Introduction to Magnetic Fields and Filaments in Star Formation

Magnetic field extrapolations and filamentary loop substructure have been key results in understanding the solar atmosphere and coronal heating. Arecibo’s 21-cm neutral hydrogen data reveal pervasive interstellar filaments that follow the galactic magnetic field lines revealed by Planck’s all-sky dust polarization maps. The small scales of the solar coronal and the large scales of interstellar matter hint that there may be a role for magnetic fields and filaments at every step of the star formation process. Herschel observations established that molecular filaments are the preferred sites of star formation. SOFIA’s new instrument, HAWC+, studies the role of magnetic fields in filaments on sub-parsec scales. ALMA polarization observations probe regions surrounding young protostars. Sub-orbital platforms, such as BLASTPOL and BLAST-TNG, deliver a wealth of data on magnetic fields in the interstellar medium. This talk sets the stage, allowing the session components to knits the big and small pictures together to provide a better understanding of galactic magnetic fields and filaments in star forming regions.