Abstract
Ascertainment of the chemical compositions of gaseous nebulae has been a goal of many investigations since the pioneering studies of Bowen and Wyse (1939) and of Wyse (1942). At that epoch it was widely believed that the elemental abundances in all stars and nebulae were essentially the same. The concept of chemical evolution in galaxies was yet to be introduced.
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References to Table 11–3
Peimbert, M., and Serrano, A. 1980, Rev, Mexicana Astron, and Astrophys., 5, 9 (r = 10 kpc).
Kaler, J.B. 1978, Ap. J., 226, 947.
Barker, T. 1978, Ap. J., 221, 145, Group I.
Barker, T. 1978, Ap. J., 221, 145, Group II.
Present survey, r = 10 kpc.
French, H. 1980, Bull. Amer. Astr. Soc., 12, 842; IAU Symposium No. 103, 1983.
Aller, L.H., and Czyzak, S.J. 1981, Proc. Natl. Acad. Sci. USA, 78, 5266.
Beck, S.C., Lacy, J.H., Townes, C.H., Aller, L.H., Geballe, T.R., and Baas, F. 1981, Ap. J., 249, 592.
Dinerstein, H. 1980, Ap. J., 237, 486.
Natta, A., Panagia, N., and Preite-Martinez, A. 1980, Ap. J., 242, 596.
Kaler, J.B. 1978, Ap. J., 225, 527.
Kaler, J.B. 1980, Ap. J., 239, 78.
Aller, L.H. 1978, Proc. Astron. Soc. Australia, 3, 213; IAU Symposium No. 76, 225.
References to Table 11–4
Barker, T. 1980, Ap. J., 237, 482 (see also I.A.U. Symposium No. 103, 1983).
Aldrovandi, S.M.V. 1980, Ap. Space Sci., 71, 393.
Peimbert, M., and Torres-Peimbert, S. 1979, Rev. Mex. Astr. Ap., 4, 341.
Hawley, S.A., and Miller, J.S. 1977, Ap. J., 212. 94.
Adopted from data in Table 3.
References to Table 11–5
M33: Kwitter and Aller (1981), theoretical models.
M101: Sedwick and Aller (1981), theoretical models.
Rayo et al. (1982) derive a smaller N/O and Ne/O ratio but comparable S/O and Ar/O ratios.
Magellanic Clouds: The carbon abundance is from Dufour, Shields, and Talbot (1982). For the other elements we tabulate mean values from this work and from Aller, Keyes, and Czyzak (1977). Theoretical models are employed here to derive IGFs. Extensive investigations were carried out previously by Dufour (1975), the Peimberts (1974–1976), Aller et al. (1974), Dufour and Harlow (1977), and by Pagel et al. (1978).
Galactic Sources: Planetary Nebulae (Tables 3 and 4); Sun (see Table 3).
Orion Nebula: Data by the Peimberts (1977) as revised and extended by Dufour et al. (1982); H II regions (at rgal = 10 kpc), Shaver et al. (1983).
References to Table 11–6
Hawley, S.A. 1978, Ap. J., 224, 417.
Peimbert, M., Torres-Peimbert, S., and Rayo, J.F. 1978, Ap. J., 220, 516.
Talent, D.L., and Dufour, R.J. 1979, Ap. J., 233, 888.
Shaver, P.A., McGee, R.X., Newton, L.M., Danks, A.C., and Pottasch, S.R. 1984, M.N.R.A.S., in press.
References to Table 11–6
Computed from data by: Wannier, P.G. 1980, Ann. Rev. Astron. Astrophys., 18. 399.
The pioneering studies of the chemical compositions of gaseous nebulae were those of:
Bowen, I.S., and Wyse, A.B. 1939, Lick Observatory Bulletin, 19. 1
Wyse, A.B. 1942, Ap. J., 95. 356.
The first detailed investigation explicitly employing modern-type expressions for rates of atomic processes was contained in the last paper of the Harvard series on Physical Processes in Gaseous Nebulae, 1945, Ap. J., 102. 239, but substantial progress was possible only with improved observational data and Seaton’s collisional cross sections (Chapter 5), see, e.g., 1954, Ap. J., 120. 401 (where importance of density fluctuations in NGC 7027 was emphasized); 1957, Ap. J., 125. 84.
The influence of small-scale temperature fluctuations on nebular spectra was examined by M. Peimbert, 1967, Ap. J., 150. 825.
Examples of ionization correction formulae are given by: Peimbert, M., and Costero, R., 1969, Bol. Obs. Tonanzintla y Tacubaya, 5,, 3
Barker, T., 1983, Ap. J., 267. 630
French, H., 1981, Ap. J., 246. 434
Stasiiiska, G., 1978, Astron. Astrophys., 66. 257.
Use of theoretical models in analyses of H II regions is discussed, e.g., by Hawley, S.A., and Grandi S.A., 1978, P.A.S.P., 90, 125
Stasinska, G., 1978, Astron. Astrophys. Suppl., 32. 429
Stasinska, G., 1980, Astron. Astrophys., 84. 320 (see Chapter 7).
Discussions of compositions of planetary nebulae are given in the references to Tables 1, 3, and 4, in IAU Symposia No. 76, 1978, and No. 103, 1983. See also:
Torres-Peimbert, S., and Peimbert, M., 1977, Rev. Mex. Astron. Astrofis., 2, 181.
Barker, T. 1978, Ap. J., 220. 193.
Kaler, J.B. 1970, Ap. J., 160. 887
Kaler, J.B. 1970, Ap. J., 226. 947
Kaler, J.B.1979, Ap. J., 228. 163
Kaler, J.B.1981, Ap. J., 244. 54
Kaler, J.B. 1981, Ap. J., 249. 201.
Boeshaar, G.O. 1975, Ap. J., 195. 695.
Webster, L.B. 1976, M.N.R.A.S., 174. 513.
Price, C.M. 1981, Ap. J., 247. 540.
Aller, L.H., and Czyzak, S.J. 1983, Ap. J. Suppl., 51. 211.
Direct evidence for nuclear processed material is found in the shell ejected from Abell 30. See:
Hazard, C., Terlevich, R., Morton, D.C., Sargent, W.L.W., and Ferland, G. 1980, Nature, 285. 453.
Jacoby G.H., and Ford, H.G. 1983, Ap. J., 266. 298.
Entrapment of certain elements in solid grains can be an important factor in influencing the composition of the gaseous phase. In the context of planetary nebulae, a basic paper is:
Shields, G.A. 1978, Ap. J., 219, 559.
A Few Examples of Analyses of Individual Objects
NGC 7662: Péquignot, D. 1980, Astron. Astrophys., 83, 52.
Harrington, J.P., Seaton, M.J., Adams, S., and Lutz, J.H. 1982, M.N.R.A.S., 199, 517.
IC 3568: Harrington, J.P., and Feibelman, W.A. 1983, Ap. J., 265, 258.
NGC 7009: Perinotto, M., and Benvenuti, P. 1981, Astron. Astrophys., 101, 88.
NGC 7027: Shields, G.A. 1978, Ap. J., 219, 565.
Perinotto, M., Panagia, N., and Benevuti, P. 1980, Astron. Astrophys., 85, 332.
Pequignot, D., and Stasinska, G. 1980, Astron. Astrophys., 81, 121.
NGC 2440: Shields, G.A., Aller, L.H., Keyes, C.D., and Czyzak, S.J. 1981, Ap. J., 248, 569.
Condal, A.R. 1982, Astron. Astrophys., 112, 124.
NGC 6720: See references to Table 1.
NGC 6302: Aller, L.H., Keyes, C.D., Ross, J.E., and O’Mara, B.J. 1981, M.N.R.A.S., 197, 95.
Analyses of Planetary Nebulae in Various Galaxies
The field of endeavor is attracting additional attention as very efficient radiation detection systems become available. A general review with references to earlier work is given by:
Ford, H.C 1983, IAU Symposium No. 103, p. 443.
A few examples of individual investigations:
Magellanic Clouds: Osmer, P. 1976, Ap. J., 203, 352.
Webster, B.L. 1978, IAU Symposium No. 76, 11.
Dufour, R., and Killen R. 1979, Ap. J., 211, 68.
Aller, L.H. 1983, Ap. J., 273, 590.
Aller, L.H., Keyes, C.D., Ross, J.E., and O’Mara, B.J. 1980, M.N.R.A.S., 194, 613.
Maran, S., Stecher, T., Gull, T., and Aller, L.H. 1982, Ap. J., 253, L43.
NGC 6822: Dufour, R., and Talent, D. 1980, Ap. J., 235, 22.
M31: Jenner, D., Ford, H., and Jacoby, G. 1979, Ap. J., 227, 392.
Fornax: Danziger, E.J., Dopita, M.A., Hawarden T.G., and Webster, B.L. 1978, Ap. J., 220, 458. See also Maran, S.P. 1984, Ap. J. (in press).
H II Regions and Abundance Gradients in Galaxies:
Although a change in the level of excitation of the H II regions in M33 with a distance from the center was noticed long ago (1942, Aller, L.H., Ap. J., 95, 52)
a systematic study was first undertaken by Searle, L., 1971, Ap. J., 168, 327.
Further investigations were carried out by Smith, H.E., 1975, Ap. J., 199, 591
who extended the study to several spirals, by Shields, G., and Searle, L., 1978, Ap. J., 222, 821
by Sedwick, K.E., and Aller, L.H., 1981, Proc.Nat’l. Acad. Sci. USA, 78, 1994
Rayo, J.F., Peimbert, M., and Torres-Peimbert, S., 1982, Ap. J., 255, 1
who investigated M101. Similar studies have been carried out by many investigators. See also Alloin, D., Collin-Souffrin, S., Joly, M. 1979, Astron. Astrophys. Suppl., 37, 361
Jensen, E.B., and Strom, K.M. and S.E. 1976, Ap. J., 209, 748
Webster, B.L., and Smith M.G. 1983, M.N.R.A.S., 204, 743
A useful summarizing article with an extensive bibliography is: Pagel, B.E.J., and Edmunds, M.G. 1981, Annual Reviews Astron. Astrophys., 19, 77.
See also Peimbert, M. 1975, Ann. Rev. Astron. Astrophys., 13, 113.
The relation between H II regions and star formation in irregular galaxies is discussed by D.A. Hunter, 1982, Ap. J., 260, 81.
Magellanic Clouds: Extensive investigations were carried out by Peimbert, M., and Torres-Peimbert, S., 1974, Ap. J., 193, 327
1976, Ap. J., 204, 581
Aller, L.H., Czyzak, S.J., Reyes, C.D., and Boeshaar, G., 1974, Proc. Nat’l. Acad. Sci. USA, 71, 4496
Dufour, R.J., 1975, Ap. J., 195, 315
Dufour, R.J., and Harlow, W., 1977, Ap. J., 216, 706
Pagel, B.E.J., Edmunds, M.G., Fosbury, R., and Webster, B.L., 1978, M.N.R.A.S., 184, 569.
Theoretical models were calculated by: Dufour, R.J., Shields, G.A., and Talbot, R.J., 1982, Ap. J., 252, 461
Aller, L.H., Keyes, CD., and Czyzak, S.J., 1979, Proc. Nat’l. Acad. Sci. USA, 76, 1525.
Abundance Gradients in Our Galaxy: See particularly Shaver et al., 1984, M.N.R.A.S., in press. For a discussion of abundance gradients obtained for our galaxy from planetary nebulae, see Peimbert, M., and Serrano, A., 1980, Rev. Mex. Astron. Astrofis., 5, 9, and references therein.
Two representative examples describing abundance gradients derived from stars are: Mayor, M., 1976, Astron. Astrophys., 48, 301
Janes, K.A., 1979, Ap. J, Suppl., 39, 135. Some abundance gradients derived from H II regions are listed in Table 6; special attention is directed to the article by Shaver et al. (1982).
Isotope ratios are discussed by: Wannier, P.G., 1980, Ann. Rev. Astron. Astrophys., 18, 399
Penzias, A.A., 1980, Science, 208, 663.
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Aller, L.H. (1984). Chemical Compositions of Gaseous Nebulae. In: Physics of Thermal Gaseous Nebulae. Astrophysics and Space Science Library, vol 112. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-9639-3_11
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