Photoionization models of Planetary Nebulae

Morisset, Charles

doi:10.1017/s1743921317001004

Cited by 3 publications

(2 citation statements)

References 32 publications

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“…In our case, the n e ([Fe III]) = 10790 +3230 −2620 cm −3 we obtain for the low res-olution spectrum is rather close to the density of HH 204. This confirms the importance of the warning given by Morisset (2017) who, through photoionization models, predict large errors in the determination of the physical conditions and chemical abundances in nebulae if one assumes a single component when, in fact, there are several and some of them is composed by high-density gas. The exercise we present in this section is an observational confirmation.…”

Section: The Effects Of Lowering the Spatial And Spectral Resolutionsupporting

confidence: 73%

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Méndez-Delgado

Esteban

García‐Rojas

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the analysis of physical conditions, chemical composition, and kinematic properties of two bow shocks – HH 529 II and HH 529 III – of the fully photoionized Herbig–Haro object HH 529 in the Orion Nebula. The data were obtained with the Ultraviolet and Visual Echelle Spectrograph at the 8.2m Very Large Telescope and 20 yr of Hubble Space Telescope imaging. We separate the emission of the high-velocity components of HH 529 II and III from the nebular one, determining ne and Te in all components through multiple diagnostics, including some based on recombination lines (RLs). We derive ionic abundances of several ions, based on collisionally excited lines and RLs. We find a good agreement between the predictions of the temperature fluctuation paradigm (t2) and the abundance discrepancy factor (ADF) in the main emission of the Orion Nebula. However, t2 cannot account for the higher ADF found in HH 529 II and III. We estimate 6 per cent of Fe in the gas phase of the Orion Nebula, while this value increases to 14 per cent in HH 529 II and between 10 and 25 per cent in HH 529 III. We find that such increase is probably due to the destruction of dust grains in the bow shocks. We find an overabundance of C, O, Ne, S, Cl, and Ar of about 0.1 dex in HH 529 II and III that might be related to the inclusion of H-deficient material from the source of the HH 529 flow. We determine the proper motions of HH 529 finding multiple discrete features. We estimate a flow angle with respect to the sky plane of 58° ± 4° for HH 529.

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Section: The Effects Of Lowering the Spatial And Spectral Resolutionsupporting

confidence: 73%

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Méndez-Delgado

Esteban

García‐Rojas

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…All the elements except for Ar have higher ICFs in the polar direction and lower in the equatorial region ( Figure 10). 3D photoionization models have demonstrated that the ICFs vary within the nebula (Morisset 2017). Moreover, it has also been suggested that a correction on the ICFs may be needed when we deal with non-spherical nebulae (Gonçalves et al 2012) and Abell 14 is one of these cases.…”

Section: Ionic and Total Abundancesmentioning

confidence: 99%

Exploring the differences of integrated and spatially resolved analysis using integral field unit data: the case of Abell 14

Akras

Monteiro

Aleman

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a new approach to study planetary nebulae using integral field spectroscopy. VLT@VIMOS datacube of the planetary nebula Abell 14 is analysed in three different ways by extracting: (i) the integrated spectrum, (ii) 1-dimensional simulated long slit spectra for different position angles and (iii) spaxel-by-spaxel spectra. These data are used to built emission-line diagnostic diagrams and explore the ionization structure and excitation mechanisms combining data from 1-and 3-dimensional photoionization models. The integrated and 1D simulated spectra are suitable for developing diagnostic diagrams, while the spaxel spectra can lead to misinterpretation of the observations. We find that the emission-line ratios of Abell 14 are consistent with UV photo-ionized emission; however, there are some pieces of evidence of an additional thermal mechanism. The chemical abundances confirm its previous classification as a Type I planetary nebula, without spatial variation. We find, though, variation in the ionization correction factors (ICFs) as a function of the slit position angle. The star at the geometric centre of Abell 14 has an A5 spectral type with an effective temperature of T eff = 7909±135 K and surface gravity log(g) = 1.4±0.1 cm s −2 . Hence, this star cannot be responsible for the ionization state of the nebula. Gaia parallaxes of this star yield distances between 3.6 and 4.5 kpc in good agreement with the distance derived from a 3-dimensional photoionization modelling of Abell 14, indicating the presence of a binary system at the centre of the planetary nebula.

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Morphology and ionization characteristics of planetary nebulae PB 1 and PC 19

Bandyopadhyay

Das

Mondal

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present results of our study of two planetary nebulae (PNe), PB1 and PC 19. We use the optical spectra of these two PNe observed at 2 m Himalayan Chandra Telescope and also archival and literature data for the study. We use the morphokinematic code shape to construct 3D morphologies of the PNe and the photoionization code cloudy to model the observed spectra. The 3D model of PB 1 consists of an elongated shell surrounded by a bipolar halo and that of PC 19 consists of an open lobed bipolar structure and a spiral filamentary pair. We analyse the ionization structure of the PNe by deriving several plasma parameters and by photoionization modelling. We estimate the elemental abundances of the elements, He, C, N, O, Ne, S, Ar, and Cl, from our analysis. We find He, C, and N abundances to be significantly higher in case of PB 1. We estimate different physical parameters of the central stars, namely effective temperature, luminosity, and gravity, and of the nebula, namely hydrogen density profiles, radii, etc., from photoionization modelling. We estimate distances to the PNe as ∼4.3 kpc for PB 1 and as ∼5.6 kpc for PC 19 by fitting the photoionization models to absolute observed fluxes. Progenitor masses are estimated from theoretical evolutionary trajectories and are found to be ∼1.67 and ∼2.38 M⊙ for PB 1 and PC 19, respectively.

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Photoionization models of Planetary Nebulae

Cited by 3 publications

References 32 publications

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Exploring the differences of integrated and spatially resolved analysis using integral field unit data: the case of Abell 14

Morphology and ionization characteristics of planetary nebulae PB 1 and PC 19

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