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dc.creatorPavel, Michael D.en_US
dc.creatorClemens, D. P.en_US
dc.date.accessioned2016-04-28T19:37:58Z
dc.date.available2016-04-28T19:37:58Z
dc.date.issued2012-12en
dc.identifierdoi:10.15781/T2QF9G
dc.identifier.citationPavel, Michael D., and Dan P. Clemens. "H II Region Driven Galactic Bubbles and Their Relationship to the Galactic Magnetic Field." The Astrophysical Journal, Vol. 760, No. 2 (Dec., 2012): 150.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34968
dc.description.abstractThe relative alignments of mid-infrared traced Galactic bubbles are compared to the orientation of the mean Galactic magnetic field in the disk. The orientations of bubbles in the northern Galactic plane were measured and are consistent with random orientations-no preferential alignment with respect to the Galactic disk was found. A subsample of H II region driven Galactic bubbles was identified, and as a single population they show random orientations. When this subsample was further divided into subthermal and suprathermal H II regions, based on hydrogen radio recombination linewidths, the subthermal H II regions showed a marginal deviation from random orientations, but the suprathermal H II regions showed significant alignment with the Galactic plane. The mean orientation of the Galactic disk magnetic field was characterized using new near-infrared starlight polarimetry and the suprathermal H II regions were found to preferentially align with the disk magnetic field. If suprathermal linewidths are associated with younger H II regions, then the evolution of young H II regions is significantly affected by the Galactic magnetic field. As H II regions age, they cease to be strongly linked to the Galactic magnetic field, as surrounding density variations come to dominate their morphological evolution. From the new observations, the ratios of magnetic-to-ram pressures in the expanding ionization fronts were estimated for younger H II regions.en_US
dc.description.sponsorshipNSF AST 06-07500, 09-07790en_US
dc.description.sponsorshipNASAen_US
dc.description.sponsorshipW. M. Keck Foundationen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjecth ii regionsen_US
dc.subjectinfrared: ismen_US
dc.subjectism: bubblesen_US
dc.subjectism: magnetic fieldsen_US
dc.subjectradioen_US
dc.subjectlines: ismen_US
dc.subjecttechniques: polarimetricen_US
dc.subjectpolarization survey gpipsen_US
dc.subjectstar-forming-regionsen_US
dc.subjectplanetary-nebulaeen_US
dc.subjectohen_US
dc.subjectmasersen_US
dc.subjectinterstellar bubblesen_US
dc.subjectmilky-wayen_US
dc.subjectevolutionen_US
dc.subjectdiscoveryen_US
dc.subjectmodelsen_US
dc.subjectgalaxyen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleH II Region Driven Galactic Bubbles And Their Relationship To The Galactic Magnetic Fielden_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2012_12_galacticbubbles.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/760/2/150en_US
dc.contributor.utaustinauthorPavel, Michael D.en_US
dc.relation.ispartofserialAstrophysical Journalen_US


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