dc.contributor.author |
Otsuka, M |
|
dc.contributor.author |
Parthasarathy, M |
|
dc.contributor.author |
Tajitsu, A |
|
dc.contributor.author |
Hubrig, S |
|
dc.date.accessioned |
2020-11-17T13:58:11Z |
|
dc.date.available |
2020-11-17T13:58:11Z |
|
dc.date.issued |
2017-03-20 |
|
dc.identifier.citation |
The Astrophysical Journal, Vol. 838, No. 1, 71 |
en_US |
dc.identifier.issn |
0004-637X |
|
dc.identifier.uri |
http://prints.iiap.res.in/handle/2248/7091 |
|
dc.description |
Restricted Access © The American Astronomical Society https://doi.org/10.3847/1538-4357/aa64d0 |
en_US |
dc.description.abstract |
We 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 1–1.5 M ⊙ 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.language.iso |
en |
en_US |
dc.publisher |
IOP Publishing |
en_US |
dc.subject |
dust, extinction |
en_US |
dc.subject |
ISM: abundances |
en_US |
dc.subject |
planetary nebulae: individual (Hen3-1357) |
en_US |
dc.title |
Physical properties of the very young PN Hen3-1357 (Stingray Nebula) based on multiwavelength observations |
en_US |
dc.type |
Article |
en_US |