Ionization Structure of Heavy Metals Due to Charge Transfer for the Case of Oxygen and Nitrogen
International Journal of Astrophysics and Space Science
Volume 5, Issue 2, April 2017, Pages: 32-40
Received: Mar. 7, 2017;
Accepted: Mar. 17, 2017;
Published: May 24, 2017
Views 971 Downloads 24
Belay Sitotaw Goshu, Department of Physics, Dire-Dawa University, Dire-Dawa, Ethiopia; Department of Mathematics, Astronomy and Computing Science, Unisa, South Africa
The main aim of this work is to investigate the effect of charge transfer reaction upon gaseous nebula structure, temperature and recombination coefficients of nitrogen and oxygen. We have been used CLOUDY 90 to determine the ionization structure of nitrogen and oxygen. We have used the abundance of heavy elements relative to hydrogen He = -1.07, C = -3.44, N = -4.07, O = -3.31 and Ne = -3.91. Ionization structure of hydrogen, helium, oxygen and nitrogen, electron temperature and the recombination coefficient are compared with the effective temperatures of 75000 K and 100000 K with the luminosity intensity of 1038 erg s-1. The result revealed that the ionization structures of elements are highly dependent on the transfer of charge and effective temperatures. In addition, we also tabulate the recombination coefficient of nitrogen and oxygen at different states with temperature of 5000 K, 10000 K, 15000 K and 20000 K. This calculation confirms with the results of previous calculation done by different scholars.
Belay Sitotaw Goshu,
Ionization Structure of Heavy Metals Due to Charge Transfer for the Case of Oxygen and Nitrogen, International Journal of Astrophysics and Space Science.
Vol. 5, No. 2,
2017, pp. 32-40.
Wilkes B. J., Ferland G. J., Hanes D. and Truran J. W. (1981). Cloudy 90 Numerical Simulations of Plasma and their Spectra, NMRAS 197-1w.
Peimbert M., 1975, Ann. Rev. Astron. Astrophys., 13, 113.
Aldrovandi S. M. V and Pe'quignot D. (1973). Radiative and Dielectronic Recombination coefficients for complex ions, Astro. Astrophys, 25, 137.
Asplund E., Grevesse N., Sauval A., and Scott P. (2009). The Chemical Composition of the Sun, 2009, ARAA, 47, 481.
Williams R. E. (1973). Mon. NOt R. astr. Soc., 164, 111-119.
Perquignot, D. Aldrovandi, S. M. V. and Stasinska, G. (1978). Charge Transfer Reaction: A consistent Model of the Planetary Nebulae NGC 7027, A&A, 63, 313.
Chamberlian J. W., 1956, ApJ, 124, 390.
Field G. & Steigman G. (1971). Charge transfer and ionization equilibrium in the interstellar medium, Astrophysics journal, 166, 59.
Steigman G. (1974). Charge transfer reactions in multiply charged ion-atom collisions. ApJ, 199, 642-646.
Osterbrock E. D. (1989). Astrophysics of Gaseous Nebulae and Active Galactic Nuclei, California University of Science Book.
Peach G. (1967). MeM. R. A. S., 71, 13.
Seaton M. J., (1969). The ionization structure of planetary nebulae–VII. The heavy elements. MNRAS, 146, 171F.
Watson W. D., Gas Phase Reactions in Astrophysics, 1978, ARA&A, 16: 585-615.
Brown R. L., 1972, Ap. and Space. Sci., 16, 274.
Mallik D. C. V. (1975). Temperature and Emission line Structure at the Edges of HII regions, ApJ, 197, 355-363.
Ferland G. J. et al., 2010, Hazy a brief introduction to CLOUDY C10.00.
Perinotto M. (1977). On the Nitrogen and Oxygen Abundances in Nebulae, A & A, 61, 247-249.
Davidson K. and Tucker W., 1970, ApJ, 161, 437.
Peimbert M., Luis F. Rodriguez and Siliva, Torres-Peimbert (1974). Ionization Structure of Gaseous Nebulae: Sulphur, Nitrogen and Helium, Nacional Autonoma de Mexico, Vol 1.
Aldrovandi S. M. V and Pe'quignot D., 1976, Astro. Astrophys, 25, 137-140.
Castellanos M., Dia’z A. I., and Terlevich E. (2002). A Comprehensive study of reported high giant H II regions- I. Detailed abundances analysis. Mon. Not. R. Astron. Soc. 329, 315.
Fang X., Storey P. J., and Liu X. W. (2011). New effective recombination coefficients for nebular N II lines. A&A, 530, A18.
Flower D. R and Seaton M. J. (1969). The Ionization Structure of Planetary Nebulae: V III the Heavy Elements, MNRAS, 146, 243-263.