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Rocket spectroscopy of ζ Puppis below 1100 Å

Published online by Cambridge University Press:  14 August 2015

Andrew M. Smith
Andrew M. Smith*
Affiliation:
NASA, Goddard Space Flight Center, Greenbelt, Md., U.S.A.

Abstract

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A spectrum of ζ Pup extending from 920 Å to 1360 Å with approximately 0.8 Å resolution has been recorded at rocket altitudes. Tentative identification of 38 multiplets below 1100 Å has been made from which it is concluded that all the lines appearing in a model atmosphere (Hickok and Morton, 1968) with Te = 37450K have been detected with the exception of those masked by telluric N2 or strong P Cygni-like profiles. Additional absorption lines indicate a wide range of ionization and excitation entirely consistent with observations in the visible spectral region of similar type stars; they also appear to affect sensibly the energy distribution within the spectrum. From newly detected blue-shifted absorption features produced by the ions Svi (933.4 Å, 944.5 Å), Niv (955.3 Å), Niii (991.0 Å), and Ovi (1033.8 Å) mean radial velocities of 1200, 530, 1800 and 1900 km sec−1 respectively have been derived. It is pointed out that the transition in Niv (955.3 Å) does not originate in the ground state configuration as do the other P Cygni profile transitions, but from an excited level which can decay radiatively to the ground state. It seems likely, therefore, that the profile is generated close to the photosphere, and this, together with previously reported results, constitutes evidence for a positive velocity gradient in the detected portion of the circumstellar envelope. On the basis of available data, ions in the ground state of Nv, Niv (by inference) and Niii are all present in the circumstellar envelope, the abundance of the latter remaining large enough to produce a strong P Cygni profile.

Type
Part II: Stellar Line Spectra
Information
Symposium - International Astronomical Union , Volume 36: Ultraviolet Stellar Spectra and Related Ground-Based Observations , 1970 , pp. 164 - 172
Copyright
Copyright © Reidel 1970 

References

Bradley, P. T. and Morton, D. C.: 1969, Astrophys. J. 156, 687.Google Scholar
Carruthers, G. R.: 1968, Astrophys. J. 151, 269.Google Scholar
Hickok, F. R. and Morton, D. C.: 1968, Astrophys. J. 152, 203.Google Scholar
Kelly, R. L.: n.d., Table of Emission lines in the Vacuum Ultraviolet for a Elements, University of Calif. Radiation Laboratory, No. 5612.Google Scholar
Kelly, R. L.: 1968, Atomic Emission Lines Below 2000 Å, U.S. Naval Research Laboratory Report No. 6648.Google Scholar
Moore, C. E.: 1950, N.B.S. Circ., No. 488, Sec. 1.Google Scholar
Moore, C. E.: 1965, N.S.R.D.S.-N.B.S. 3, Sec. 1.Google Scholar
Morton, D. C.: 1969a, preprint, Princeton University.Google Scholar
Morton, D. C.: 1969b, Astrophys. Space Sci. 3, 117.Google Scholar
Morton, D. C., Jenkins, E. B., and Brooks, N. H.: 1969, Astrophys. J. 155, 875.Google Scholar
Smith, A. M.: 1969, Astrophys. J. 156, 93.Google Scholar
Stecher, T. P.: 1968, in Wolf-Rayet Stars (ed. by Gebbie, K. B. and Thomas, R. N.), National Bureau of Standards Special Publication 307, Washington, D.C. Google Scholar