Abstract
At a resolution of 0.17 Å, the profile of λλ 5780, 5797 were found to be asymmetric and steeper to the blue. The FWHM of λ 5780 and λ 5797 are respectively 2.7 Å and 1.1 Å. There is also a broad, shallow feature shortward of λ 5780. Equivalent widths of λλ 5780, 5797 were measured at a resolution of 0.26 Å, and they present a very tight correlation. Therefore, it is highly likely that these two diffuse lines have a common origin. The correlation between the equivalent width of λ 5780, EW(λ 5780), and E(B — V) is good for normal field stars. But there is a systematic weakening of λ 5780 in the spectra of Be stars, and the reverse is true for stars in the Scorpius-Ophiucus region. Excluding Be stars, a least square fit gives EW(λ 5780) = 0.75E(B — V) Å mag.−1. From the profiles and structures of the diffuse features, and the correlations with various parameters of the interstellar medium, it is suggested that: (1) the diffuse band λ 4430 may be produced by the preionization of H− and, (2) λλ 5780, 5797 may be due to the pure electronic transitions of the impurity centers in solid grains.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
A’Hearn, M. F.: 1972, Astron. J. 77, 302.
Brück, M. T., Nandy, K., and Seddon, H.: 1969, Physica 41, 128.
Fano, U.: 1961, Phys. Rev. 124, 1866.
Greenberg, J. M.: 1968, in B. M. Middlehurst and L. H. Aller (eds.), Nebulae and Interstellar Matter, U. of Chicago Press, Chicago, Chapter 6.
Greenberg, J. M.: 1971, Nature Phys. Sci. 230, 15.
Herbig, G. H.: 1967, in H. van Woerden (ed.), ‘Radio Astronomy and the Galactic System’, IAU Symp. 31, 85.
Hulst, H. C. van de: 1957, Light Scattering by Small Particles, J. Wiley & Sons Inc., New York.
Ingemann-Hilberg, C. and Rudkjøbing, M.: 1970, Astrophys. Space Sci. 6, 101.
Johnson, F. M.: 1967, in J. M. Greenberg and T. P. Roark (eds.), Colloquium on Interstellar Grains, Rensselaer Polytechnic Institute, 1965, NASA, Washington, NASA SP-140, p. 241.
Nandy, K. and Seddon, H.: 1970, Nature 227, 264.
Rebane, K. K.: 1970, Impurity Spectra of Solids, Plenum Press, New York-London.
Rudkjobing, M.: 1969a, Astrophys. Space Sci. 3, 102.
Rudkjobing, M.: 1969b, Astrophys. Space Sci. 5, 68.
Rudkjobing, M.: 1970, Astrophys. Space Sci. 6, 157.
Stoeckly, R. and Dressler, K.: 1964, Astrophys. J. 139, 240.
Wampler, E. J.: 1966, Astrophys. J. 144, 921.
Wickramasinghe, N. C. and Nandy, K.: 1970, Astrophys. Space Sci. 6, 154.
Wilson, R.: 1958, Astrophys. J. 128, 57.
Wilson, R.: 1964, Pubi. Roy. Obs. Edinburgh 4, 67.
Yen, W. M., Scott, W. C, and Schawlow, A. L.: 1964, Phys. Rev. 136, A271.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1973 IAU
About this chapter
Cite this chapter
Wu, CC. (1973). A Study of the Interstellar Diffuse Absorption Features. In: Greenberg, J.M., Van De Hulst, H.C. (eds) Interstellar Dust and Related Topics. International Astronomical Union / Union Astronomique Internationale, vol 52. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2664-2_13
Download citation
DOI: https://doi.org/10.1007/978-94-010-2664-2_13
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-2666-6
Online ISBN: 978-94-010-2664-2
eBook Packages: Springer Book Archive