Recombination Coefficient of Heavy Elements Using Photoionization Modeling

Belay Sitotaw Goshu

doi:doi:10.11648/j.ajaa.20170504.11

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Recombination Coefficient of Heavy Elements Using Photoionization Modeling

Belay Sitotaw Goshu

Published in American Journal of Astronomy and Astrophysics (Volume 5, Issue 4)

Received: 10 June 2017 Accepted: 23 June 2017 Published: 28 September 2017

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Abstract

The main purpose of this work is to calculate the radiative, dielectronic and total recombination of non-hydrogenic elements. We applied the photoionization codes to investigate the recombination coefficients. We have calculated radiative and dielectronic recombination coefficients of some elements at different temperatures and ionization stages. The results are obtained at low temperatures between 5,000 and 20,000 K and it shows that the dielectronic coefficients are not negligible relative to radiative recombination by assuming the solar abundances of H, He, C, N, O, Ne and S. We determined the total recombination coefficients of each element and compared them with previous works. Our calculations the radiative dielectric and total recombination coefficients of oxygen, nitrogen, carbon, neon and sulphur ions at a given temperature agree with the previous works.

Published in	American Journal of Astronomy and Astrophysics (Volume 5, Issue 4)
DOI	10.11648/j.ajaa.20170504.11
Page(s)	42-49
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

Photoionization, Radiative, Dielectronic Recombination Coefficients

References

[1]	P’equignot D., Petitjean P., &Boission C., 1991, A&A, 251, 680.
[2]	Burgess A., 1965, ApJ, 17, 198.
[3]	Tarter C. B., 1973, ApJ, 168, 313.
[4]	Tarter C. B., 1971, ApJ, 168, 313.
[5]	Aldrovandi S. M. V., and Pequigno D., 1973, A&A, 25, 137.
[6]	Aldrovandi S. M. V., and Pequigno D., 1973, Rev. Bras. Fis. 4, 491.
[7]	Gould R. J., 1978, ApJ, 219, 250.
[8]	Ferland G. J., 2011, Hazy a brief introduction to cloudy, University of Kentucky internal report.
[9]	Osterbrock D. E., 1989, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei, University of Science Book, California, Santa Crux.
[10]	Susmita ChakravortyAjit K. Kembhavi, Martin Elvis, Gary Ferland and N. R. Badnell, 2008, MNRAS, 384, 24.
[11]	Burgess A. and Seaton, M. J., 1960a, MNRAS, 120, 76.
[12]	Sultana N., 1999, ApJS, 120, 131.
[13]	Osterbrock D. E., 1974, Astrophysics of Gaseous Nebulae, San Francisco: Freeman.
[14]	Woods D. T., Shull J. M., & Sarazin C. L., 1981, ApJ, 399, 401.
[15]	Michael A. Dopita& Ralph S. Sutherland, 1999, Diffuse matter in the universe. The Australian National University, Can-berra.
[16]	Anil K. Pradhan and Sultana N. Nahar, 2011, Atomic Astrophysics and Spectroscopy, United Kingdom at the University Press, Cambridge.
[17]	Dopita M. A. and Sutherland R. S., 2001, Diffuse Matter in the Universe, Subtitle, Edition, Physics of Monograph.
[18]	Shull J. M. & Steenberg, M. V., 1982, ApJ, 48, 95-107.
[19]	Liu X., 2010, arxiv: 1001.3715v2 [astro.ph.GA]. The dark secrets of gaseous nebulae highlights from deep spectroscopy.
[20]	Jon C. Weisheit, ApJ, 1973, 185, 877.
[21]	Bates D. R. and Massey H. S. W., 1943. The negative ions of atomic and molecular oxygen. Philosophical Transactions and of the Royal Society of London, Series A, 239(806): 269-304.
[22]	Massey H. S. W. and Bates D. R., 1942. The properties of neutral and ionized atomic oxygen influence on the upper atmosphere. Reports in Physics, 9(1), 62-74.
[23]	Orban Z., Altun, A., Ka’llberg A., Simonsson, G., Andler A., Pa_al M., Blom P., La’fgren S., Trotsenko S., BAuhm & Schuch R., 2009 A & A 498, 909.
[24]	Burgess A., 1964. Dielectronic recombination and the temperature of the solar corona. ApJ, 139, 776
[25]	Sultana N. Nahar and Anil K. Pradhan, 2006, ApJS, 162, 417.
[26]	Fogel M., Bandell N. R., Glans P., Loch S. D., Madzunkov S., Abdel-NabySh. A., Pindzola M. S., & Schuch R., 2005, A&A, 442, 757
[27]	Altun Z., Yumak A., Bandell N. R., Loch S. D., Pindzola M. S., 2006, A&, 447, 1165.
[28]	Drake G. W. F., 1996, in Drake G. W., ed., Atomic, Molecular, and Optical Physics Handbook. American Institute of Physics, Woodbury, New York, p. 154.
[29]	Nussbaumer H. & Storey P. J., 1983, A&A, 126, 74.
[30]	Sultana N. Nahar& Anil K. Pradhan, 1995, ApJ, 447, 966
[31]	Jacobs V. L., Davis J., Kepple P. C., and Blaha M., 1977b, Apj, 215, 690.
[32]	Goharji A. A., 1988, Durham Thesis, Durham University
[33]	Bandell N. R., 2005, A&A, 447, 389.
[34]	Williams R. E., Jenkins E. B., Baldwin J. A., Zhang Y., Sharpee B., Lellegrini E., and Philips M., 2008, ApJ, 677, 1100-1119.

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APA Style

Belay Sitotaw Goshu. (2017). Recombination Coefficient of Heavy Elements Using Photoionization Modeling. American Journal of Astronomy and Astrophysics, 5(4), 42-49. https://doi.org/10.11648/j.ajaa.20170504.11

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Belay Sitotaw Goshu. Recombination Coefficient of Heavy Elements Using Photoionization Modeling. Am. J. Astron. Astrophys. 2017, 5(4), 42-49. doi: 10.11648/j.ajaa.20170504.11

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AMA Style

Belay Sitotaw Goshu. Recombination Coefficient of Heavy Elements Using Photoionization Modeling. Am J Astron Astrophys. 2017;5(4):42-49. doi: 10.11648/j.ajaa.20170504.11

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@article{10.11648/j.ajaa.20170504.11,
  author = {Belay Sitotaw Goshu},
  title = {Recombination Coefficient of Heavy Elements Using Photoionization Modeling},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {5},
  number = {4},
  pages = {42-49},
  doi = {10.11648/j.ajaa.20170504.11},
  url = {https://doi.org/10.11648/j.ajaa.20170504.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20170504.11},
  abstract = {The main purpose of this work is to calculate the radiative, dielectronic and total recombination of non-hydrogenic elements. We applied the photoionization codes to investigate the recombination coefficients. We have calculated radiative and dielectronic recombination coefficients of some elements at different temperatures and ionization stages. The results are obtained at low temperatures between 5,000 and 20,000 K and it shows that the dielectronic coefficients are not negligible relative to radiative recombination by assuming the solar abundances of H, He, C, N, O, Ne and S. We determined the total recombination coefficients of each element and compared them with previous works. Our calculations the radiative dielectric and total recombination coefficients of oxygen, nitrogen, carbon, neon and sulphur ions at a given temperature agree with the previous works.},
 year = {2017}
}

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TY  - JOUR
T1  - Recombination Coefficient of Heavy Elements Using Photoionization Modeling
AU  - Belay Sitotaw Goshu
Y1  - 2017/09/28
PY  - 2017
N1  - https://doi.org/10.11648/j.ajaa.20170504.11
DO  - 10.11648/j.ajaa.20170504.11
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 42
EP  - 49
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20170504.11
AB  - The main purpose of this work is to calculate the radiative, dielectronic and total recombination of non-hydrogenic elements. We applied the photoionization codes to investigate the recombination coefficients. We have calculated radiative and dielectronic recombination coefficients of some elements at different temperatures and ionization stages. The results are obtained at low temperatures between 5,000 and 20,000 K and it shows that the dielectronic coefficients are not negligible relative to radiative recombination by assuming the solar abundances of H, He, C, N, O, Ne and S. We determined the total recombination coefficients of each element and compared them with previous works. Our calculations the radiative dielectric and total recombination coefficients of oxygen, nitrogen, carbon, neon and sulphur ions at a given temperature agree with the previous works.
VL  - 5
IS  - 4
ER  -

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Author Information

Belay Sitotaw Goshu

Department of Physics, Dire-Dawa University, Dire-Dawa, Ethiopia; Department of Mathematics, Astronomy and Computing Science, Unisa, South Africa

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APA Style

Belay Sitotaw Goshu. (2017). Recombination Coefficient of Heavy Elements Using Photoionization Modeling. American Journal of Astronomy and Astrophysics, 5(4), 42-49. https://doi.org/10.11648/j.ajaa.20170504.11

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ACS Style

Belay Sitotaw Goshu. Recombination Coefficient of Heavy Elements Using Photoionization Modeling. Am. J. Astron. Astrophys. 2017, 5(4), 42-49. doi: 10.11648/j.ajaa.20170504.11

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AMA Style

Belay Sitotaw Goshu. Recombination Coefficient of Heavy Elements Using Photoionization Modeling. Am J Astron Astrophys. 2017;5(4):42-49. doi: 10.11648/j.ajaa.20170504.11

Copy | Download

@article{10.11648/j.ajaa.20170504.11,
  author = {Belay Sitotaw Goshu},
  title = {Recombination Coefficient of Heavy Elements Using Photoionization Modeling},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {5},
  number = {4},
  pages = {42-49},
  doi = {10.11648/j.ajaa.20170504.11},
  url = {https://doi.org/10.11648/j.ajaa.20170504.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20170504.11},
  abstract = {The main purpose of this work is to calculate the radiative, dielectronic and total recombination of non-hydrogenic elements. We applied the photoionization codes to investigate the recombination coefficients. We have calculated radiative and dielectronic recombination coefficients of some elements at different temperatures and ionization stages. The results are obtained at low temperatures between 5,000 and 20,000 K and it shows that the dielectronic coefficients are not negligible relative to radiative recombination by assuming the solar abundances of H, He, C, N, O, Ne and S. We determined the total recombination coefficients of each element and compared them with previous works. Our calculations the radiative dielectric and total recombination coefficients of oxygen, nitrogen, carbon, neon and sulphur ions at a given temperature agree with the previous works.},
 year = {2017}
}

Copy | Download

TY  - JOUR
T1  - Recombination Coefficient of Heavy Elements Using Photoionization Modeling
AU  - Belay Sitotaw Goshu
Y1  - 2017/09/28
PY  - 2017
N1  - https://doi.org/10.11648/j.ajaa.20170504.11
DO  - 10.11648/j.ajaa.20170504.11
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 42
EP  - 49
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20170504.11
AB  - The main purpose of this work is to calculate the radiative, dielectronic and total recombination of non-hydrogenic elements. We applied the photoionization codes to investigate the recombination coefficients. We have calculated radiative and dielectronic recombination coefficients of some elements at different temperatures and ionization stages. The results are obtained at low temperatures between 5,000 and 20,000 K and it shows that the dielectronic coefficients are not negligible relative to radiative recombination by assuming the solar abundances of H, He, C, N, O, Ne and S. We determined the total recombination coefficients of each element and compared them with previous works. Our calculations the radiative dielectric and total recombination coefficients of oxygen, nitrogen, carbon, neon and sulphur ions at a given temperature agree with the previous works.
VL  - 5
IS  - 4
ER  -

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