Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7601
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dc.contributor.authorKameswara Rao, N-
dc.contributor.authorLambert, D. L-
dc.contributor.authorReddy, A. B. S-
dc.contributor.authorManchado, A-
dc.contributor.authorDiaz-Luis, J. J-
dc.contributor.authorGarcia-Hernandez, D. A-
dc.date.accessioned2021-02-07T06:08:45Z-
dc.date.available2021-02-07T06:08:45Z-
dc.date.issued2020-07-01-
dc.identifier.citationPublications of the Astronomical Society of the Pacific, Vol. 132, No. 1013, 074201en_US
dc.identifier.issn0004-6280-
dc.identifier.urihttp://hdl.handle.net/2248/7601-
dc.descriptionRestricted Accessen_US
dc.description.abstractWe have detected CH+ and CH molecular absorption lines from the youngcompact planetary nebula IC 4997 from high resolution optical spectra. A high-resolution infra-red (H and K bands) spectrum provides detection of H2 emission lines among many other lines. The H2 lines provide an excitation temperature of 2100 K which may result from UV fluorescence in the envelope or from shocks formed at the interface between an expanding outflow of ionized gas and the neutral envelope ejected when the star was on the AGB. It is suggested that the CH+ may result from the endothermic reaction C + H2 → CH+ + H. Intriguingly, CH+ and also CH show a higher expansion velocity than H2 emission suggesting they may be part of the post-shocked gas.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.1088/1538-3873/ab9097-
dc.rights© Astronomical Society of the Pacific-
dc.subjectinterstellar moleculesen_US
dc.subjectcircumstellar gasen_US
dc.titleDetection of CH+, CH and H2 Molecules in the Young Planetary Nebula IC 4997en_US
dc.typeArticleen_US
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