Infrared properties of planetary nebulae with [WR] central stars

Górny, S. K.; Stasińska, G.; Szczerba, R.; Tylenda, R.

doi:10.1051/0004-6361:20011050

Cited by 23 publications

(39 citation statements)

References 39 publications

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“…with the age of the nebula, as also was noted by Gorny et al (2001). These observed trends imply that dust destruction is inefficient as a PN evolves.…”

Section: Dust Mass and Dust-to-gas Mass Ratiosupporting

confidence: 73%

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Infrared properties of planetary nebulae with [WR] and wels central stars

Muthumariappan

Parthasarathy

2020

Monthly Notices of the Royal Astronomical Society

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We report the IR properties of planetary nebulae with WR type and wels central stars known to date and compare them with the IR properties of a sample of PNe with H-rich central stars. We use near-, mid-and far-IR photometric data from archives to derive the IR properties of PNe. We have constructed IR colour-colour diagrams of PNe using measurements from 2M ASS, IRAS, W ISE and Akari bands.[WR] PNe have a larger near-IR emission from the hot dust component and also show a tendency for stronger 12µm emission as compared to the other two groups. Cool AGB dust properties of all PNe are found to be similar. We derived the dust colour temperatures, dust masses, dust-to-gas mass ratios, IR luminosities and IR excess of PNe for these three groups.[WR] PNe and wels-PNe tend to have larger mean values for dust mass when compared to the third group. The average dust-togas mass ratio is found to be similar for the three groups of PNe. While there is a strong correlation of dust temperature and IR luminosity with the age for the three groups of PNe, the dust mass, dust-to-gas mass ratios and IR excess are found to be non-varying as the PNe evolve. [WR] PNe and wels-PNe show very similar distribution of excitation classes and also show similar distribution with Galactic latitude. of emission lines from ions with different ionization potential is related to the temperature evolution and can give the evolutionary connection between [WR] stars of different subtypes. Such quantitative classification schemes of [WR] stars currently in use were given by Crowther, De Marco & Barlow (1998, CDB98) and by Acker & Neiner (2003, AN03). CDB98 find a continuity in the [WR] classification scheme from [WC] to [WO] and suggest that the sequence is primarily due to excitation rather than abundance. All subtypes are seen in a sequence of decreasing stellar temperature from [WO1] → [WO4] → [WC4] → [WC11]. AN03 conclude from this an evolution of stars from post-AGB → [WC11] → [WC4] -[WO4] → [WO1]. Both CDB98 and AN03 find a sparsity of CSPNe in the [WC6-8] subclasses indicating a rapid evolution through this range or a different evolutionary path leading to two ionization sequences which is not yet understood. On the other hand, wels do not have such a classification scheme.Though there are pronounced differences between the [WR] stars and the hydrogen rich CSPNe in their spectra and photospheric abundances etc., the PNe with [WR] stars have many properties which are very similar to those shown by the PNe with hydrogen-

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“…with the age of the nebula, as also was noted by Gorny et al (2001). These observed trends imply that dust destruction is inefficient as a PN evolves.…”

Section: Dust Mass and Dust-to-gas Mass Ratiosupporting

confidence: 73%

“…All the three groups of PNe show similar mean values, taking the dispersion into account. Gorny et al (2001) also have suggested that there is no significant difference in m d /m g for [WR] PNe and non-[WR] PNe.…”

Section: Dust Mass and Dust-to-gas Mass Ratiomentioning

confidence: 99%

Infrared properties of planetary nebulae with [WR] and wels central stars

Muthumariappan

Parthasarathy

2020

Monthly Notices of the Royal Astronomical Society

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“…In the two colour diagram (Fig. 16) of the I(0.82 µm), J(1.25 µm) and K(2.15 µm) bands, most nebulae of all types cluster near colour temperatures of 4000 K. While none of the [WO] objects is found elsewhere, several [WC] nebulae are found at high (J − K) 0 colour indices: foremost PNG 012.2 + 04.9 and PNG 291.3 − 26.2 which have been suspected for the presence of hot dust (Górny et al 2001), and also PNG 004.8 − 22.7, PNG 027.6 + 04.2, and PNG 327.1 − 02.2.…”

Section: Infrared Coloursmentioning

confidence: 95%

Chemical compositions and plasma parameters of planetary nebulae with Wolf-Rayet and wels type central stars

Girard

Köppen

Acker

2006

A&A

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Aims. Chemical compositions and other properties of planetary nebulae around central stars of spectral types [WC], [WO], and wels are compared with those of "normal" central stars, in order to clarify the evolutionary status of each type and their interrelation. Methods. We use plasma diagnostics to derive from optical spectra the plasma parameters and chemical compositions of 48 planetary nebulae. We also reanalyze the published spectra of a sample of 167 non-WR PN. The results as well as the observational data are compared in detail with those from other studies of the objects in common. Results. We confirm that [WC], [WO] and wels nebulae are very similar to those "normal" PN: the relation between [N II] and [O III]electron temperatures, abundances of He, N, O, Ne, S and Ar, and the number of ionizing photons show no significant differences. However, some differences are observed in their infrared (IRAS) properties. wels nebulae appear bluer than [WR] PN. The central star's spectral type is clearly correlated with electron density, temperature and excitation class of the nebula, [WC] nebulae tend to be smaller than the other types. All this corroborates the view of an evolutionary sequence from cool [WC 11] central stars inside dense, low excitation nebulae towards hot [WO 1] stars with low density, high excitation nebulae. The wels PN, however, appear to be a separate class of objects, not linked to WRPN by evolution: nebular excitation, electron temperature and density, and the number of ionizing photons all cover the whole range found in the other types. Their lower mean N/O ratio and slightlylower He/H suggest progenitor stars less massive than for the other PN types. Furthermore, the differences between results of different works are dominated by the differences in observational data rather than differences in the analysis methods.

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“…the spectral type was known or the stellar continuum had been observed but no emission lines were seen (Tylenda et al 1993. Next, we selected objects with IRAS mid-infrared colours similar to the colours of known [WR] PNe (see Górny et al 2001). Therefore, obviously, this sample cannot be used to estimate the proportion of [WR] PNe among PNe in the Galactic bulge.…”

Section: New Observations and Reduction Proceduresmentioning

confidence: 99%

The populations of planetary nebulae in the direction of the Galactic bulge

Górny¹,

Stasińska²,

Escudero

et al. 2004

A&A

Self Cite

127

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Abstract. We have observed 44 planetary nebulae (PNe) in the direction of the Galactic bulge, and merged our data with published ones. We have distinguished, in the merged sample of 164 PNe, those PNe most likely to prtain physically to the Galactic bulge and those most likely to belong to the Galactic disk. We have determined the chemical composition of all the 164 objects in a coherent way. We looked for stellar emission features and discovered 14 (7) The oxygen abundance distribution of bulge PNe is similar in shape to that of the metallicity distribution of bulge giants, but significantly narrower. (8) The location of SB 32 (PN G 349.7-09.1) in the (V lsr , l II ) diagram and its low oxygen abundance argues that it probably belongs to the halo population.

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Infrared properties of planetary nebulae with [WR] central stars

Cited by 23 publications

References 39 publications

Infrared properties of planetary nebulae with [WR] and wels central stars

Infrared properties of planetary nebulae with [WR] and wels central stars

Chemical compositions and plasma parameters of planetary nebulae with Wolf-Rayet and wels type central stars

The populations of planetary nebulae in the direction of the Galactic bulge

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