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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2592
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dc.contributor.authorSurendiranath, R-
dc.contributor.authorKameswara Rao, N-
dc.date.accessioned2008-07-09T08:06:06Z-
dc.date.available2008-07-09T08:06:06Z-
dc.date.issued1995-08-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 275, No. 3, pp. 685 - 698en
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2248/2592-
dc.description.abstractA photoionization code has been developed incorporating provision for the presence of dust mixed with gas. M4-18 has been modelled utilizing optical CCD spectra and other observations ranging from UV to radio wavelengths. T_e and N_e from the model are 6600K and 6050 cm^-3, respectively. The abundances of C, N and Ne are found to be the same as the solar values while O is overabundant by a factor of two and S is lower than the solar value by ~90 per cent. A mono-sized amorphous carbon grain dust model explains the IRAS fluxes satisfactorily but emits poorly in the 1- to 10-μm region. M4-18 is a protoplanetary nebula with properties similar to CPD - 56 deg8032 and V348 Sgr.en
dc.format.extent1731502 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherBlackwell Publishingen
dc.relation.urihttp://adsabs.harvard.edu/abs/1995MNRAS.275..685Sen
dc.subjectRadiative Transferen
dc.subjectStars: Wolf-Rayeten
dc.subjectDusten
dc.subjectExtinctionen
dc.subjectPlanetary Nebulae: Individual: M4-18en
dc.subjectInfrared: Ism: Continuumen
dc.titleA photoionization model of the nebula around the WC11 star M4-18en
dc.typeArticleen
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