American Journal of Astronomy and Astrophysics

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Ionization Structure of Heavy Metals for Planetary Nebulae

Received: 21 April 2018    Accepted: 25 May 2018    Published: 03 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.

DOI 10.11648/j.ajaa.20180602.12
Published in American Journal of Astronomy and Astrophysics (Volume 6, Issue 2, June 2018)
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), 2024. Published by Science Publishing Group

Keywords

Planetary Nebulae, Abundances, Photoionization, Star Evolution

References
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Author Information
  • 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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    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://download.sciencepg.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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