Evolution of Planetary Nebulae with WR-type Central Stars

Danehkar, Ashkbiz

doi:10.1086/681244

Cited by 6 publications

(12 citation statements)

References 283 publications

(790 reference statements)

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“…It can be seen that the IFU velocity and dispersion maps of M 1-32 are akin to what found for Th 2-A being viewed almost pole-on (Danehkar 2015). Similarly, the P-V diagrams (see Figure 3) imply that this object has also collimated bipolar outflows with very low inclination (i = 5 • ; in § 4) relative to the line of sight.…”

Section: Spatially-resolved Kinematic Mapssupporting

confidence: 59%

“…The CSPN M 1-32 was classified by Acker & Neiner (2003) as the peculiar [WO 4] based on the wide FWHM of C IV-5801/12 doublet corresponding to a terminal velocity of V ∞ ≃ 4900 km s −1 that is higher than V ∞ ≃ 2000-3000 km s −1 typically seen in usual [WR] CSPNe. The PN Th 2-A whose morpho-kinematic structure was studied by Danehkar (2015) is another object with [WO 3] pec classified by Weidmann et al (2008). Our sample also contains 4 well-known PNe with wels selected from the literature (Tylenda et al 1991(Tylenda et al , 1993Górny et al 1997Górny et al , 2004.…”

Section: Observationsmentioning

confidence: 99%

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Morpho-kinematic properties of Wolf-Rayet planetary nebulae

Danehkar

2021

Preprint

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The majority of planetary nebulae (PNe) show axisymmetric morphologies, whose causes are not well understood. In this work, we present spatially resolved kinematic observations of 14 Galactic PNe surrounding Wolf-Rayet ([WR]) and weak emission-line stars (wels) based on the Hα and [N II] emission taken with the Wide Field Spectrograph on the ANU 2.3-m telescope. Velocity-resolved channel maps and position-velocity diagrams, together with archival Hubble Space Telescope (HST) and ground-based images, are employed to construct three-dimensional morpho-kinematic models of 12 objects using the program SHAPE. Our results indicate that these 12 PNe have elliptical morphologies with either open or closed outer ends. Kinematic maps also illustrate on-sky orientations of elliptically symmetric morphologies of the interior shells in NGC 6578 and NGC 6629, and the compact (≤ 6 arcsec) PNe Pe 1-1, M 3-15, M 1-25, Hen 2-142, and NGC 6567, in agreement with the high-resolution HST images containing morphological details. Point-symmetric knots in Hb 4 exhibit deceleration with distance from the nebular center that could be due to shock collisions with the ambient medium. Velocity dispersion maps of Pe 1-1 disclose point-symmetric knots similar to those in Hb 4. Collimated outflows are also visible in the position-velocity diagrams of M 3-30, M 1-32, M 3-15, and K 2-16, which are reconstructed by tenuous prolate ellipsoids extending upwardly from thick toroidal shells in our models.

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Section: Spatially-resolved Kinematic Mapssupporting

confidence: 59%

Section: Observationsmentioning

confidence: 99%

Morpho-kinematic properties of Wolf-Rayet planetary nebulae

Danehkar

2021

Preprint

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“…Hence, the atomic data for collisional excitation and recombination process are essential to determine physical conditions and elemental abundances of ionized nebulae from collisionally excited and recombination lines (see e.g. Danehkar, Parker, and Ercolano (2013); Danehkar et al (2014); Danehkar (2014); Danehkar, Parker, and Steffen (2016); Danehkar (2018a)).…”

Section: Discussionmentioning

confidence: 99%

AtomNeb: IDL Library for Atomic Data of Ionized Nebulae

Danehkar¹

2019

JOSS

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Ionized gaseous nebulae are interstellar clouds of hydrogen-rich materials, which are photoionized by ultraviolet radiation from stars, making them visible in multi-wavelength bands. Ionized nebulae can be used as an astrophysical tool to trace the chemical composition of the interstellar medium in our Galaxy and other galaxies, and to study mixing processes in stellar evolution. Spectra emitted from ionized nebulae generally contain collisionally excited and recombination lines. Electron temperatures, electron densities, and ionic abundances can be determined from collisionally excited lines (CEL) by solving statistical equilibrium equations using collision strengths (Ω ij ) and transition probabilities (A ij ) of ions. Moreover, physical conditions and chemical abundances can be calculated from recombination lines (RL) using effective recombination coefficients (α eff ) of ions. The atomic data, i.e. Ω ij , A ij , and α eff , are used to calculate line emissivities in nebular spectral analysis tools (e.g.

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“…The API functions of this IDL library can easily be utilized to generate spatially-resolved maps of extinction, temperature, density, and chemical abundances from integral field spectroscopic observations (see e.g. Danehkar, Parker, and Ercolano (2013); Danehkar et al (2014); Danehkar (2014)).…”

Section: Discussionmentioning

confidence: 99%

proEQUIB: IDL Library for Plasma Diagnostics and Abundance Analysis

Danehkar¹

2018

JOSS

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The emission lines emitted from gaseous nebulae carry valuable information about the physical conditions and chemical abundances of ionized gases in these objects, as well as the interstellar reddening. We determine the electron temperature, the electron density, and the ionic abundances from the dereddened fluxes of collisionally excited lines (CEL) and recombination lines (RL) identified in nebular spectra (see e.g. Danehkar, Parker, and Ercolano (2013); Danehkar et al. (2014); Danehkar, Parker, and Steffen (2016); Danehkar (2018b)).proEQUIB is a library including several application programming interface (API) functions developed in the Interactive Data Language (IDL), which can be used to determine temperatures, densities, and chemical abundances from emission lines of ionized nebulae. This IDL library can also be used by the GNU Data Language (GDL) ; Coulais et al. (2010)), which is a free and open-source alternative IDL compiler. This IDL/GDL package employs the IDL library AtomNeb Atomic Data for Ionized Nebulae (Danehkar (2018a)), which contains collision strengths and transition probabilities for collisional excitation calculations, and recombination coefficients for recombination calculations. This package includes several API functions to determine physical conditions and chemical abundances from CEL and RL, derive interstellar extinctions from Balmer lines, and deredden the observed fluxes:• The API functions for the CEL analysis were developed in the IDL programming language based on the algorithm of the FORTRAN program EQUIB (Howarth and Adams (1981); Howarth et al. (2016)), which calculates atomic level populations and line emissivities in statistical equilibrium in multi-level atoms for the given physical conditions. These API functions can be used to determine the electron temperature, the electron density, and the ionic abundances from the dereddened fluxes of collisionally excited lines emitted from ionized gaseous nebulae. • The API functions for the RL analysis were developed in IDL according to the algorithm of the recombination scripts by X. W. Liu and Y. Zhang included in the FORTRAN program MOCASSIN (Ercolano et al. (2003); Ercolano, Barlow, and Storey (2005)). These API functions can be used to determine the ionic abundances from the dereddened fluxes of recombination lines emitted from ionized nebulae.

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Evolution of Planetary Nebulae with WR-type Central Stars

Cited by 6 publications

References 283 publications

Morpho-kinematic properties of Wolf-Rayet planetary nebulae

Morpho-kinematic properties of Wolf-Rayet planetary nebulae

AtomNeb: IDL Library for Atomic Data of Ionized Nebulae

proEQUIB: IDL Library for Plasma Diagnostics and Abundance Analysis

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