2004A&A...413..329S


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.14CET18:41:15

2004A&A...413..329S - Astronomy and Astrophysics, volume 413, 329-342 (2004/1-1)

Comprehensive modelling of the planetary nebula LMC-SMP61 and its [WC]-type central star.

STASINSKA G., GRAEFENER G., PENA M., HAMANN W.-R., KOESTERKE L. and SZCZERBA R.

Abstract (from CDS):

We present a comprehensive study of the Magellanic Cloud planetary nebula SMP61 and of its nucleus, a Wolf-Rayet type star classified [WC 5-6]. The observational material consists of HST STIS spectroscopy and imaging, together with optical and UV spectroscopic data collected from the literature and infrared fluxes measured by IRAS. We have performed a detailed spectral analysis of the central star, using the Potsdam code for expanding atmospheres in non-LTE. For the central star we determine the following parameters: L*=103.96L, R*=0.42R, T*=87.5kK, {dot}(M)=10–6.12M/yr, v=1400km/s, and a clumping factor of D=4. The elemental abundances by mass are XHe=0.45, XC=0.52, XN<5x10–5, XO=0.03, and XFe<1x10–4. The fluxes from the model stellar atmosphere were used to compute photoionization models of the nebula. All the available observations, within their error bars, were used to constrain these models. We find that the ionizing fluxes predicted by the stellar model are consistent with the fluxes needed by the photoionization model to reproduce the nebular emission, within the error margins. However, there are indications that the stellar model overestimates the number and hardness of Lyman continuum photons. The photoionization models imply a clumped density structure of the nebular material. The observed CIII]λ1909/CIIλ4267 line ratio implies the existence of carbon-rich clumps in the nebula. Such clumps are likely produced by stellar wind ejecta, possibly mixed with the nebular material. We discuss our results with regard to the stellar and nebular post-AGB evolution. The observed Fe-deficiency for the central star indicates that the material which is now visible on the stellar surface has been exposed to s-process nucleosynthesis during previous thermal pulses. The absence of nitrogen allows us to set an upper limit to the remaining H-envelope mass after a possible AGB final thermal pulse. Finally, we infer from the total amount of carbon detected in the nebula that the strong [WC] mass-loss may have been active only for a limited period during the post-AGB evolution.

Abstract Copyright:

Journal keyword(s): stars: Wolf-Rayet - stars: atmospheres - stars: mass-loss - ISM: abundances - ISM: planetary nebulae: individual: SMP61 - ISM: planetary nebulae: general

CDS comments: p. 340 : BD +30 3696 is a misprint for BD +30 3639

Simbad objects: 8

goto Full paper

goto View the reference in ADS

Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 40 PN 00 13 01.0170260109 +72 31 19.032886305   11.63 11.46     [WC8] 582 2
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14348 1
3 IRAS F05258-7343 pA? 05 24 35.9812176149 -73 40 40.213765086   16.48     16.64 WC 58 0
4 SMP LMC 83 PN 05 36 20.7216020344 -67 18 07.659774493 15.56 16.225 14.948   16.558 [WN4.5:] 138 0
5 PN A66 30 PN 08 46 53.4640384491 +17 52 46.368019418   14.23 14.30 13.47   [WC5] 373 0
6 HD 165763 WR* 18 08 28.4691215895 -21 15 11.182287576 7.16 7.54 7.82 8.55   WC6 265 0
7 HD 184738 PN 19 34 45.2337512278 +30 30 58.951476338   10.41 10.44     [WC9] 913 0
8 PN A66 78 PN 21 35 29.3817385380 +31 41 45.450384940   13.04 13.25     [WC5] 294 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2004A&A...413..329S and select 'bookmark this link' or equivalent in the popup menu


2019.11.14-18:41:15

© Université de Strasbourg/CNRS

    • Contact