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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2268
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dc.contributor.authorRoshi, Anish D.-
dc.date.accessioned2007-04-18T11:16:36Z-
dc.date.available2007-04-18T11:16:36Z-
dc.date.issued2007-03-20-
dc.identifier.citationAstrophysical Journal, 2007, Vol.658, pL41-L44en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/2268-
dc.descriptionRestricted Access. Restricted Access. Articles older than 2 years are open to all at the journal site (alternative location)en
dc.description.abstractSeveral indirect evidences indicate a magnetic origin for the nonthermal width of spectral lines observed toward molecular clouds. In this Letter, I suggest that the origin of the nonthermal width of carbon recombination lines (CRLs) observed from photodissociation regions (PDRs) near ultracompact H II regions is magnetic and that the magnitude of the line width is an estimate of the Alfvén speed. The magnetic field strengths estimated based on this suggestion compare well with those measured toward molecular clouds with densities similar to PDR densities. I conclude that multifrequency CRL observations have the potential to form a new tool to determine the field strength near star-forming regions.en
dc.format.extent71514 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe University of Chicago Press for the American Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?2007ApJ...658L..41Ren
dc.relation.urihttp://dx.doi.org/10.1086/513465en
dc.rights2007 The American Astronomical Societyen
dc.subjectISM: H II Regions,en
dc.subjectISM: Lines and Bandsen
dc.subjectISM: Magnetic Fieldsen
dc.subjectISM: Moleculesen
dc.subjectMagnetohydrodynamics: MHDen
dc.subjectRadio Lines: ISMen
dc.titleMagnetic fields at the periphery of ultracompact H II regions from carbon recombination line observationsen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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