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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1080
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dc.contributor.authorAnantharamaiah, K.R.-
dc.date.accessioned2006-01-04T05:49:32Z-
dc.date.available2006-01-04T05:49:32Z-
dc.date.issued1985-
dc.identifier.citationJournal of Astrophysics and Astronomy, 1985, Vol. 6, p203-226.en
dc.identifier.issn0250-6335-
dc.identifier.urihttp://hdl.handle.net/2289/1080-
dc.description.abstractThe properties of diffuse ionized gas in the inner Galaxy are derived from a recent survey of the H 272-alpha recombination line (324.99 MHz) in the direction of 34 H II regions, 12 SNRs, and six regions of continuum minimum in the Galactic plane. The derived properties of the gas are an electron density of 0.5-6/cu cm, an electron temperature of 3000-8000 K, and emission measures of 500-3000 pc/cm exp 6. It is suggested that the low-frequency recombination lines arise in low-density envelopes of the H II regions; it is found that these envelopes should have electron densities in the range 1-10/cu cm and linear sizes of 30-300 pc in order to produce the observed H 272-alpha lines.en
dc.format.extent1137256 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherIndian Academy of Sciences, Bangalore, India.en
dc.rightsIndian Academy of Sciences, Bangalore, India.en
dc.subjectGalaxyen
dc.subjectRecombinational linesen
dc.subjectGalactic rigeen
dc.subjectInterstellar mediumen
dc.subjectElectron densitiesen
dc.subjectH2 regionsen
dc.subjectLow density envelopesen
dc.titleLow density ionized gas in the inner Galaxy - interpretation of recombination line observations at 325 MHz.en
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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