J/A+A/573/A65ivo://CDS.VizieR/J/A+A/573/A65doi:10.26093/cds/vizier.35730065CDSHajduk M.van Hoof P.A.M.Zijlstra A.A.2018-01-05T08:56:26Z2014-12-18T09:21:35ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frplanetary-nebulaespectroscopyThe evolution of central stars of planetary nebulae was so far documented in just a few cases. However, spectra collected a few decades ago may provide a good reference for studying the evolution of central stars using the emission line fluxes of their nebulae. We investigated evolutionary changes of the [OIII] 5007{AA} line flux in the spectra of planetary nebulae. We compared nebular fluxes collected during a decade or longer. We used literature data and newly obtained spectra. A grid of Cloudy models was computed using existing evolutionary models, and the models were compared with the observations. An increase of the [OIII] 5007{AA} line flux is frequently observed in young planetary nebulae hosting H-rich central stars. The increasing nebular excitation is the response to the increasing temperature and hardening radiation of the central stars. We did not observe any changes in the nebular fluxes in the planetary nebulae hosting late-type Wolf-Rayet (WR) central stars. This may indicate a slower temperature evolution (which may stem from a different evolutionary status) of late-[WR] stars. In young planetary nebulae with H-rich central stars, the evolution can be followed using optical spectra collected during a decade or longer. The observed evolution of H-rich central stars is consistent with the predictions of the evolutionary models provided in the literature. Late-[WR] stars possibly follow a different evolutionary path.2015A&A...573A..65Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/573/A65CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/573/A65https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/573/A65http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/573/A65https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/573/A65https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/573/A65http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/573/A65GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/573/A65/table2 (Information on each object)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/573/A65/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/573/A65/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/573/A65/table2?GETtext/xml+votable180.050000true285.11062538.35201940.0055555555555555566/12852 14005 14279 14443 14827 14922 20816 20826 28772 28825 28908 28977 29297 30684 31847 32193 41470 43139https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/573/A65?format=asciiOpticaldefaultJ/A+A/573/A65/table2Information on each objectSimbadNameSimbad column added by the CDSmeta.idcharDateIbservtion datetime.epochcharSpplot the spectrummeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the objectmeta.id;meta.maincharprimaryLminWavelength startnminstr.bandwidthintLmaxWavelength endnminstr.bandwidthintRes[0.4/1.3] Resolutionnmspect.resolutionfloatTelTelescope (Torun, Radcliffe or SALT)meta.id;instr.telcharNoNumber of exposuresmeta.numberintTexpExposure timestime.duration;obs.exposureintSlit[1/4] Slit widtharcsecspect.line.widthintsecz[1/1.7] Airmassobs.airMassfloatStdStandard starsmeta.idchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/573/A65/table4Spectra of planetary nebulae: flux datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the objectmeta.id;meta.maincharlambda[318/797] Spectral wavelengthnmem.wldoubleF(lambda)Flux value in mW/m^2^/{AA}cW.m**-2.nm**-1phot.fluxdouble