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Article: Independent emission and absorption abundances for planetary nebulae
Title | Independent emission and absorption abundances for planetary nebulae |
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Authors | |
Keywords | ISM: abundances Planetary nebulae: general Planetary nebulae: individual (He 2-138, NGC 246, NGC 6543, Tc 1) Ultraviolet: ISM |
Issue Date | 2008 |
Publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205 |
Citation | Astrophysical Journal Letters, 2008, v. 677 n. 2, p. 1100-1119 How to Cite? |
Abstract | Emission-line abundances have been uncertain for more than a decade due to unexplained discrepancies in the relative intensities of the forbidden lines and weak permitted recombination lines in PNe and H II regions. The observed intensities of forbidden and recombination lines originating from the same parent ion differ from their theoretical values by factors of more than an order of magnitude in some of these nebulae. In this study we observe UV resonance line absorption in the central stars of PNe produced by the nebular gas and from the same ions that emit optical forbidden lines. We then compare the derived absorption column densities with the emission measures determined from ground-based observations of the nebular forbidden lines. We find for our sample of PNe that the collisionally excited forbidden lines yield column densities that are in basic agreement with the column densities derived for the same ions from the UV absorption lines. A similar comparison involving recombination line column densities produces poorer agreement, although near the limits of the formal uncertainties of the analyses. An additional sample of objects with larger abundance discrepancy factors will need to be studied before a stronger statement can be made that recombination line abundances are not correct. © 2008. The American Astronomical Society. All rights reserved. |
Persistent Identifier | http://hdl.handle.net/10722/138793 |
ISSN | 2023 Impact Factor: 8.8 2023 SCImago Journal Rankings: 2.766 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Williams, R | en_HK |
dc.contributor.author | Jenkins, EB | en_HK |
dc.contributor.author | Baldwin, JA | en_HK |
dc.contributor.author | Zhang, Y | en_HK |
dc.contributor.author | Sharpee, B | en_HK |
dc.contributor.author | Pellegrini, E | en_HK |
dc.contributor.author | Phillips, M | en_HK |
dc.date.accessioned | 2011-09-19T01:40:17Z | - |
dc.date.available | 2011-09-19T01:40:17Z | - |
dc.date.issued | 2008 | en_HK |
dc.identifier.citation | Astrophysical Journal Letters, 2008, v. 677 n. 2, p. 1100-1119 | en_HK |
dc.identifier.issn | 2041-8205 | en_HK |
dc.identifier.uri | http://hdl.handle.net/10722/138793 | - |
dc.description.abstract | Emission-line abundances have been uncertain for more than a decade due to unexplained discrepancies in the relative intensities of the forbidden lines and weak permitted recombination lines in PNe and H II regions. The observed intensities of forbidden and recombination lines originating from the same parent ion differ from their theoretical values by factors of more than an order of magnitude in some of these nebulae. In this study we observe UV resonance line absorption in the central stars of PNe produced by the nebular gas and from the same ions that emit optical forbidden lines. We then compare the derived absorption column densities with the emission measures determined from ground-based observations of the nebular forbidden lines. We find for our sample of PNe that the collisionally excited forbidden lines yield column densities that are in basic agreement with the column densities derived for the same ions from the UV absorption lines. A similar comparison involving recombination line column densities produces poorer agreement, although near the limits of the formal uncertainties of the analyses. An additional sample of objects with larger abundance discrepancy factors will need to be studied before a stronger statement can be made that recombination line abundances are not correct. © 2008. The American Astronomical Society. All rights reserved. | en_HK |
dc.language | eng | - |
dc.publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205 | en_HK |
dc.relation.ispartof | Astrophysical Journal Letters | en_HK |
dc.subject | ISM: abundances | en_HK |
dc.subject | Planetary nebulae: general | en_HK |
dc.subject | Planetary nebulae: individual (He 2-138, NGC 246, NGC 6543, Tc 1) | en_HK |
dc.subject | Ultraviolet: ISM | en_HK |
dc.title | Independent emission and absorption abundances for planetary nebulae | en_HK |
dc.type | Article | en_HK |
dc.identifier.openurl | http://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=677&issue=2&spage=1100&epage=1119&date=2008&atitle=Independent+emission+and+absorption+abundances+for+planetary+nebulae | - |
dc.identifier.email | Zhang, Y: zhangy96@hku.hk | en_HK |
dc.identifier.authority | Zhang, Y=rp00841 | en_HK |
dc.description.nature | published_or_final_version | en_US |
dc.identifier.doi | 10.1086/529065 | en_HK |
dc.identifier.scopus | eid_2-s2.0-42649102669 | en_HK |
dc.identifier.hkuros | 142737 | - |
dc.identifier.volume | 677 | en_HK |
dc.identifier.issue | 2 | en_HK |
dc.identifier.spage | 1100 | en_HK |
dc.identifier.epage | 1119 | en_HK |
dc.identifier.isi | WOS:000254898000024 | - |
dc.publisher.place | United Kingdom | en_HK |
dc.identifier.scopusauthorid | Williams, R=7409604935 | en_HK |
dc.identifier.scopusauthorid | Jenkins, EB=7202285481 | en_HK |
dc.identifier.scopusauthorid | Baldwin, JA=35184774500 | en_HK |
dc.identifier.scopusauthorid | Zhang, Y=23768446500 | en_HK |
dc.identifier.scopusauthorid | Sharpee, B=6602273650 | en_HK |
dc.identifier.scopusauthorid | Pellegrini, E=8404989800 | en_HK |
dc.identifier.scopusauthorid | Phillips, M=7402770160 | en_HK |
dc.identifier.issnl | 2041-8205 | - |