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dc.contributor.authorOtsuka, M-
dc.contributor.authorParthasarathy, M-
dc.contributor.authorTajitsu, A-
dc.contributor.authorHubrig, S-
dc.identifier.citationThe Astrophysical Journal, Vol. 838, No. 2, 71en_US
dc.descriptionRestricted Accessen_US
dc.description.abstractWe carried out a detailed analysis of the interesting and important very young planetary nebula (PN) Hen3-1357 (Stingray Nebula) based on a unique data set of optical to far-IR spectra and photometric images. We calculated the abundances of nine elements using collisionally excited lines (CELs) and recombination lines (RLs). The RL C/O ratio indicates that this PN is O-rich, which is also supported by the detection of the broad 9/18 μm bands from amorphous silicate grains. The observed elemental abundances can be explained by asymptotic giant branch (AGB) nucleosynthesis models for initially 1–1.5Me stars with Z=0.008. The Ne overabundance might be due to the enhancement of 22Ne isotope in the He-rich intershell. Using the spectrum of the central star synthesized by Tlusty as the ionization/heating source of the PN, we constructed the self-consistent photoionization model with Cloudy to the observed quantities and derived the gas and dust masses, dust-to-gas mass ratio, and core mass of the central star. About 80% of the total dust mass is from warm–cold dust component beyond ionization front. Comparison with other Galactic PNe indicates that Hen3-1357 is an ordinary amorphous silicate-rich and O-rich gas PN. Among other studied PNe, IC4846 shows many similarities in properties of the PN to Hen3-1357, although their post-AGB evolution is quite different from each other. Further monitoring of observations and comparisons with other PNe such as IC4846 are necessary to understand the evolution of Hen3-1357.en_US
dc.publisherIOP Publishingen_US
dc.rights© The American Astronomical Society-
dc.titlePhysical properties of the very young PN Hen3-1357 (Stingray Nebula) based on multiwavelength observationsen_US
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