Magnetic fields in planetary nebulae and post-AGB nebulae

Magnetic fields are an important but largely unknown ingredient of planetary nebulae. They have been detected in oxygen-rich asymptotic giant branch (AGB) and post-AGB stars, and may play a role in the shaping of their nebulae. Here we present SCUBA submillimetre polarimetric observations of four bipolar planetary nebulae and post-AGB stars, including two oxygen-rich and two carbon-rich nebulae, to determine the geometry of the magnetic field by dust alignment. Three of the four sources (NGC 7027, 6537 and 6302) present a well-defined toroidal magnetic field oriented along their equatorial torus or disc. NGC 6302 may also show field lines along the bipolar outflow. CRL 2688 shows a complex field structure, where part of the field aligns with the torus, whilst an other part approximately aligns with the polar outflow. It also presents marked asymmetries in its magnetic structure. NGC 7027 shows evidence for a disorganized field in the south-west corner, where the SCUBA shows an indication for an outflow. The findings show a clear correlation between field orientation and nebular structure.     

Pulsar nebulae

Several of the exotic supernova remnants are re-interpreted as pulsar-illuminated former windzones. The class of supernova remnants thus splits into (i) (the usual) shell remnants and (ii) pulsar nebulae in which a (fairly young) pulsar blows its relativistic wind into its low-density environs.     

Rotational dynamics of subsolar sublimating triaxial comets

A model with subsolar water sublimation on a triaxial, ellipsoidal comet nucleus is presented for the calculation of reactive torques. The resulting differential equations describing the comet's rotation are then Hamiltonian, and gravity-gradients are trivial to include. While effects derived from a weak perturbing function are neither able to change the rotational excitation nor the spin magnitude of the nucleus, it is shown how the spin orientation of comets can change significantly over an orbital run. However, of the four comets studied, 1P, 19P, 46P and the Rosetta target 67P, 19P and 46P were the only objects clearly exhibiting this feature, thereby confirming a technique used to derive the consequences of a more elaborate model of sublimation induced torques. In particular, the rotational parameters of 67P were seen to be very stable, indicating that a highly kinematical model of its rotation for the mapping of the comet's gravitational field during the Rosetta mission can be used. The model's hierarchy with 1P/Halley as the object with highest excitation probability, is consistent with observations.     

Hydrogen-poor planetary nebulae

Five planetary nebulae are known to show hydrogen-poor material nearthe central star. In the case of A58, this gas was ejected following alate thermal pulse similar to Sakurai's Object. In this paper I will reviewthese five objects. One of them, IRAS 18333 –2357, may not be a truePN. I will show that there is a strong case for a relation to the [WC]stars and their relatives, the weak emission-line stars. The surfaceabundances of the [WC] stars are explained via diffuse overshoot intothe helium layer. The hydrogen-poor PNe do not support this: theirabundances indicate a change of abundance with depth in the heliumlayer. A short-lived phase of very high mass loss, the r-AGB, isindicated. Sakurai's Object may be at the start of such a phase, and mayevolve to very low stellar temperatures.     

Observations of southern nebulae

Spectroscopic observations of 10 HII regions in the southern hemisphere are presented. The observations cover the spectral region 3600–8000 Å.European Southern Observatory     

Planetary nebulae and ALMA

Our understanding of the late evolution of intermediate mass stars (∼1–8M_⊙) through the planetary nebula phase is undergoing major developments. Observations at infrared and millimeter wavelengths have revealed important components of neutral gas and dust in the nebulae that directly trace their formation from mass-loss on the Asymptotic Giant Branch. At the same time, high resolution imaging, especially with the Hubble Space Telescope, has revealed a surprising array of structures in the nebulae: multiple arcs, tori, jets, and myriads of small scale fragments. None of these are fully understood, and all involve the neutral gas component. This paper highlights recent observations of these structures and discusses the open questions, with an emphasis on those areas where observations with ALMA are likely to make important contributions.     

Theoretical models of planetary nebulae

Theoretical models are attempted for eight moderate excitation planetary nebulae which have been intensively observed with the image-tube scanner at Lick and in other investigations. The models are uniform density structures, often truncated, with central star energy distributions and chemical compositions so adjusted as to give an optimum fit with the observations. Although a satisfactory representation can be obtained for most of the stronger, usually observed lines, those arising from the 3p ³ configuration, specifically the nebular transitions of [Sii], [Cliii], and [Ariv], often give difficulties. A comparison with results of model predictions with those from simple, traditional procedures generally shows a good agreement, except in those instances where different judgments are made in interpreting emissions of ions of 3p ⁿ configurations.     

Spectrophotometry of three planetary nebulae

The results of a spectroscopic investigation of three possible planetary nebulae, K4- 53, K4- 55, and K4- 57, are presented. It is shown that K4- 53 and K4- 55 are planetary nebulae while K4- 57 can be considered with high probability to be one. The temperatures of the nuclei of these nebulae are determined by Ambartsumian’s method. The optical depths for L_c photons in the region of λ ≤ 912 Å are determined. An anomalously high nitrogen abundance is observed in K4- 55.     

Theoretical models of planetary nebulae

Theoretical models are calculated for 15 planetary nebulae of medium-to-high excitation, following procedures previously described. Initial stellar energy distributions are adopted from Cassinelli (1971), but are subsequently modified to obtain the best representation of optical spectra for the selected objects. Other adjustable parameters include the stellar radius,R ^(*), the nebular density,N _H, the truncation radius,r _c, for the nebular shell, and the chemical composition. Excitationsensitive ratios are usually well-represented as are the actual observed intensities of spectral lines. Forbidden lines arising from 3p ³ configurations, e.g., those of [SII], [ArIV], and [ClIII] offer difficulties. For this sample of nebulae, the mean abundances seem to agree well with those found in an earlier study where the models were used as interpolation devices (Aller, 1978). Our objective is not to use the models to derive abundances explicitly, but rather to use them to find ionization correction factors. Some cautions and limitations of this procedure are described.     

Imaging polarimetry of proto-planetary nebulae

Polarization maps are presented for the three proto-planetary nebulae, Frosty Leo, MZ3 and M2-9. The structure of each object is discussed and geometries derived from these data are compared with those predicted by the currently fashionable two wind hydrodynamical models which account for many of the features of such transient nebulae.     

Accurate coordinates of planetary nebulae

Accurate optical coordinates of 734 PNe, measured on the charts of the Digitized Palomar Sky Survey, are presented. As a result of the discussion about the external accuracy the constants –0.8″ in RA and +0.8″ in DEC should be added to the coordinates measured by us. They were used but rounded off already in CGPN(2000). The list and measurements of new 31 candidates of central stars are given which might be interesting for stellar evolution.     

Plasma diagnostics of planetary nebulae

Diagnostics for the rarefied plasmas in gaseous nebulae are reviewed, beginning with the pioneering papers of V. A. Ambartsumian. These papers, as well as the diagnostic techniques which have been developed on the basis of ideas contained in them, are discussed. Diagnostic techniques for homogeneous, as well as inhomogeneous, plasmas are described. __________ Translated from Astrofizika, Vol. 51, No. 3, pp. 363–383 (August 2008).     

IRSPEC observations of planetary nebulae

We have obtained infrared spectra of planetary nebulae in the 3.0–3.8 m range using IRSPEC, the ESO grating infrared spectrograph, attached to the 3.6-m telescope. We find evidence of an evolution of the carriers of the unidentified emission bands in the 3 m region, and explain the observed behaviour in terms of ion irradiation from fast stellar wind.Based on observations collected at the European Southern Observatory, La Silla, Chile.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Univers, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Spectrophotometry of five planetary nebulae

The results of a spectroscopic investigation of five planetary nebulae are given. The relative intensities of emission lines observed in them were determined. The electron density and electron temperature of the central region of the nebula KjPn 8 were determined. It was shown that the gas in this region is very highly excited. Translated from Astrofizika, Vol. 41, No. 3, pp. 367–375, July–September, 1998.     

Monochromatic observations of planetary nebulae

Monochromatic images in H, H, [Nii] 6584, [Sii] 6717, and [Oiii] 5007 lines are presented for a morphological study of planetary nebulae. Narrow bandpass (=5 to 10Å) interference filters are generally used in order to discriminate peculiar structures existing in different emission lines. However, large bandwidths (=50 Å) along with long exposures, are also necessary in searching for faint nebulosities associated with planetaries.Three faint objects of the Abell's list of old planetary nebulae have been observed through narrow band filters, by means of an image tube (A33, A36 in Chile) or the image photon counting device (A79 at the Haute Provence Observatory). Following the H/[Nii] intensity ratio, a discussion is given about the distance previously derived with some assumptions concerning the measured red fluxes.