Issue |
A&A
Volume 451, Number 3, June I 2006
|
|
---|---|---|
Page(s) | 925 - 935 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20054192 | |
Published online | 04 May 2006 |
Planetary nebulae with emission-line central stars
1
Centrum Astronomii UMK, ul. Gagarina 11, 87-100 Torun, Poland e-mail: [Krzysztof.Gesicki;Krzysztof.Gozdziewski]@astri.uni.torun.pl
2
School of Physics and Astronomy, University of Manchester, PO Box 88, Manchester M60 1QD, UK e-mail: a.zijlstra@umist.ac.uk
3
Observatoire astronomique de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France e-mail: acker@astro.u-strasbg.fr
4
Copernicus Astronomical Center, ul.Rabianska 8, 87-100 Torun, Poland e-mail: skg@ncac.torun.pl
5
Space Telescope European Co-ordinating Facility, ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany e-mail: jwalsh@eso.org
Received:
12
September
2005
Accepted:
29
December
2005
The kinematic structure of a sample of planetary nebulae, consisting of 23 [WR] central stars, 21 weak emission line stars (wels), and 57 non-emission line central stars, is studied. The [WR] stars are shown to be surrounded by turbulent nebulae, a characteristic shared by some wels but almost completely absent from the non-emission line stars. The fraction of objects showing turbulence for non-emission-line stars, wels, and [WR] stars is 7%, 24%, and 91%, respectively. The [WR] stars show a distinct IRAS 12-micron excess, indicative of small dust grains, which is not found for wels. The [WR]-star nebulae are on average more centrally condensed than those of other stars. On the age-temperature diagram, the wels are located on tracks of both high and low stellar mass, while [WR] stars trace a narrow range of intermediate masses. Emission-line stars are not found on the cooling track. One group of wels may form a sequence wels–[WO] stars with increasing temperature. For the other groups, both the wels and the [WR] stars appear to represent several, independent evolutionary tracks. We find a discontinuity in the [WR] stellar temperature distribution and suggest different evolutionary sequences above and below the temperature gap. One group of cool [WR] stars has no counterpart among any other group of PNe and may represent binary evolution. A prime factor distinguishing wels and [WR] stars appears to be stellar luminosity. We find no evidence for an increase in the nebular expansion velocity with time.
Key words: planetary nebulae: general / stars: evolution
© ESO, 2006
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.