Ionization Structure of Heavy Metals for Planetary Nebulae

Belay Sitotaw Goshu

doi:doi:10.11648/j.ajaa.20180602.12

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Ionization Structure of Heavy Metals for Planetary Nebulae

Belay Sitotaw Goshu

Published in American Journal of Astronomy and Astrophysics (Volume 6, Issue 2)

Received: 21 April 2018 Accepted: 25 May 2018 Published: 3 July 2018

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Abstract

The purpose of this work to reproduces the flux of lines emitted by the ionized gas, resulting in a good agreement between observed and predicted line fluxes, temperatures and electron density with the chemical abundances of ionic species with carbon and oxygen rich planetary. The model has been calculated using clouds of dust grains in order to calculate the electron temperature, density, and emission fluxes. The dust grain with polycyclic aromatic hydrocarbons (PAH) physics combined with thick shell geometry solves the problem of the heating and allows the fitting of fluxes lines, the electron temperatures and the ionization structure of the nebula. Among other lines, we determined line ratio of CIIλ4267A, [NII] λ5755A, 6584A, 6548A, [SII] λ4078A, 4070A, 6716A, and 6731A and compared the results with the observation data by changing the abundances of C, N, O and S, which are enhanced by a factor of 2. The analysis of the ionization structure of the gas, as well as this calculation of the flux of ions, is presented in this work. Therefore, our result revealed that flux lines like [NII] λ6584A, [OII] λ3727A+29A and [OIII] λ5007A greater than the observed fluxes. The nebulae are found to have low electron temperature than found by the previous author, but the electron density is high.

Published in	American Journal of Astronomy and Astrophysics (Volume 6, Issue 2)
DOI	10.11648/j.ajaa.20180602.12
Page(s)	39-48
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2018. Published by Science Publishing Group

Keywords

Planetary Nebulae, Abundances, Photoionization, Star Evolution

References

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Belay Sitotaw Goshu. (2018). Ionization Structure of Heavy Metals for Planetary Nebulae. American Journal of Astronomy and Astrophysics, 6(2), 39-48. https://doi.org/10.11648/j.ajaa.20180602.12

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Belay Sitotaw Goshu. Ionization Structure of Heavy Metals for Planetary Nebulae. Am. J. Astron. Astrophys. 2018, 6(2), 39-48. doi: 10.11648/j.ajaa.20180602.12

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AMA Style

Belay Sitotaw Goshu. Ionization Structure of Heavy Metals for Planetary Nebulae. Am J Astron Astrophys. 2018;6(2):39-48. doi: 10.11648/j.ajaa.20180602.12

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@article{10.11648/j.ajaa.20180602.12,
  author = {Belay Sitotaw Goshu},
  title = {Ionization Structure of Heavy Metals for Planetary Nebulae},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {6},
  number = {2},
  pages = {39-48},
  doi = {10.11648/j.ajaa.20180602.12},
  url = {https://doi.org/10.11648/j.ajaa.20180602.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20180602.12},
  abstract = {The purpose of this work to reproduces the flux of lines emitted by the ionized gas, resulting in a good agreement between observed and predicted line fluxes, temperatures and electron density with the chemical abundances of ionic species with carbon and oxygen rich planetary. The model has been calculated using clouds of dust grains in order to calculate the electron temperature, density, and emission fluxes. The dust grain with polycyclic aromatic hydrocarbons (PAH) physics combined with thick shell geometry solves the problem of the heating and allows the fitting of fluxes lines, the electron temperatures and the ionization structure of the nebula. Among other lines, we determined line ratio of CIIλ4267A, [NII] λ5755A, 6584A, 6548A, [SII] λ4078A, 4070A, 6716A, and 6731A and compared the results with the observation data by changing the abundances of C, N, O and S, which are enhanced by a factor of 2. The analysis of the ionization structure of the gas, as well as this calculation of the flux of ions, is presented in this work. Therefore, our result revealed that flux lines like [NII] λ6584A, [OII] λ3727A+29A and [OIII] λ5007A greater than the observed fluxes. The nebulae are found to have low electron temperature than found by the previous author, but the electron density is high.},
 year = {2018}
}

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TY  - JOUR
T1  - Ionization Structure of Heavy Metals for Planetary Nebulae
AU  - Belay Sitotaw Goshu
Y1  - 2018/07/03
PY  - 2018
N1  - https://doi.org/10.11648/j.ajaa.20180602.12
DO  - 10.11648/j.ajaa.20180602.12
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 39
EP  - 48
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20180602.12
AB  - The purpose of this work to reproduces the flux of lines emitted by the ionized gas, resulting in a good agreement between observed and predicted line fluxes, temperatures and electron density with the chemical abundances of ionic species with carbon and oxygen rich planetary. The model has been calculated using clouds of dust grains in order to calculate the electron temperature, density, and emission fluxes. The dust grain with polycyclic aromatic hydrocarbons (PAH) physics combined with thick shell geometry solves the problem of the heating and allows the fitting of fluxes lines, the electron temperatures and the ionization structure of the nebula. Among other lines, we determined line ratio of CIIλ4267A, [NII] λ5755A, 6584A, 6548A, [SII] λ4078A, 4070A, 6716A, and 6731A and compared the results with the observation data by changing the abundances of C, N, O and S, which are enhanced by a factor of 2. The analysis of the ionization structure of the gas, as well as this calculation of the flux of ions, is presented in this work. Therefore, our result revealed that flux lines like [NII] λ6584A, [OII] λ3727A+29A and [OIII] λ5007A greater than the observed fluxes. The nebulae are found to have low electron temperature than found by the previous author, but the electron density is high.
VL  - 6
IS  - 2
ER  -

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Author Information

Belay Sitotaw Goshu

Department of Physics, Dire Dawa University, Dire Dawa, Ethiopia

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Belay Sitotaw Goshu. (2018). Ionization Structure of Heavy Metals for Planetary Nebulae. American Journal of Astronomy and Astrophysics, 6(2), 39-48. https://doi.org/10.11648/j.ajaa.20180602.12

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ACS Style

Belay Sitotaw Goshu. Ionization Structure of Heavy Metals for Planetary Nebulae. Am. J. Astron. Astrophys. 2018, 6(2), 39-48. doi: 10.11648/j.ajaa.20180602.12

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AMA Style

Belay Sitotaw Goshu. Ionization Structure of Heavy Metals for Planetary Nebulae. Am J Astron Astrophys. 2018;6(2):39-48. doi: 10.11648/j.ajaa.20180602.12

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@article{10.11648/j.ajaa.20180602.12,
  author = {Belay Sitotaw Goshu},
  title = {Ionization Structure of Heavy Metals for Planetary Nebulae},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {6},
  number = {2},
  pages = {39-48},
  doi = {10.11648/j.ajaa.20180602.12},
  url = {https://doi.org/10.11648/j.ajaa.20180602.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20180602.12},
  abstract = {The purpose of this work to reproduces the flux of lines emitted by the ionized gas, resulting in a good agreement between observed and predicted line fluxes, temperatures and electron density with the chemical abundances of ionic species with carbon and oxygen rich planetary. The model has been calculated using clouds of dust grains in order to calculate the electron temperature, density, and emission fluxes. The dust grain with polycyclic aromatic hydrocarbons (PAH) physics combined with thick shell geometry solves the problem of the heating and allows the fitting of fluxes lines, the electron temperatures and the ionization structure of the nebula. Among other lines, we determined line ratio of CIIλ4267A, [NII] λ5755A, 6584A, 6548A, [SII] λ4078A, 4070A, 6716A, and 6731A and compared the results with the observation data by changing the abundances of C, N, O and S, which are enhanced by a factor of 2. The analysis of the ionization structure of the gas, as well as this calculation of the flux of ions, is presented in this work. Therefore, our result revealed that flux lines like [NII] λ6584A, [OII] λ3727A+29A and [OIII] λ5007A greater than the observed fluxes. The nebulae are found to have low electron temperature than found by the previous author, but the electron density is high.},
 year = {2018}
}

Copy | Download

TY  - JOUR
T1  - Ionization Structure of Heavy Metals for Planetary Nebulae
AU  - Belay Sitotaw Goshu
Y1  - 2018/07/03
PY  - 2018
N1  - https://doi.org/10.11648/j.ajaa.20180602.12
DO  - 10.11648/j.ajaa.20180602.12
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 39
EP  - 48
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20180602.12
AB  - The purpose of this work to reproduces the flux of lines emitted by the ionized gas, resulting in a good agreement between observed and predicted line fluxes, temperatures and electron density with the chemical abundances of ionic species with carbon and oxygen rich planetary. The model has been calculated using clouds of dust grains in order to calculate the electron temperature, density, and emission fluxes. The dust grain with polycyclic aromatic hydrocarbons (PAH) physics combined with thick shell geometry solves the problem of the heating and allows the fitting of fluxes lines, the electron temperatures and the ionization structure of the nebula. Among other lines, we determined line ratio of CIIλ4267A, [NII] λ5755A, 6584A, 6548A, [SII] λ4078A, 4070A, 6716A, and 6731A and compared the results with the observation data by changing the abundances of C, N, O and S, which are enhanced by a factor of 2. The analysis of the ionization structure of the gas, as well as this calculation of the flux of ions, is presented in this work. Therefore, our result revealed that flux lines like [NII] λ6584A, [OII] λ3727A+29A and [OIII] λ5007A greater than the observed fluxes. The nebulae are found to have low electron temperature than found by the previous author, but the electron density is high.
VL  - 6
IS  - 2
ER  -

Copy | Download