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Spectrophotometry of beta Lyrae

Theodore E. Houck

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Abstract

Two hundred and fourteen scans over the wavelength region 1100 A to 1800 A with 10 A resolution were obtained by OAO spacecraft for the eclipsing binary Beta Lyrae between JD 2440889.5 and JD 2440904.5. Preliminary results indicate that: (1) The intensity at primary minimum is almost exactly one-half that at maximum and that the primary eclipse is less deep than that in the visual or longer ultraviolet wavelengths; (2) except for the 1100 to 1200 A region, the depth of the primary eclipse appears independent of wavelength; (3) the energy distribution at secondary minimum is similar to that at primary; (4) the two most prominent emission lines match well both with Si IV and C IV emission observed in gamma Vel and imply an exciting source of high temperature; (5) the emission lines do not show variation with phase.

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Two hundred and fourteen scans over the wavelength region 1100 A to 1800 A with 10 A resolution were obtained by OAO spacecraft for the eclipsing binary Beta Lyrae between JD 2440889.5 and JD 2440904.5. Preliminary results indicate that: (1) The intensity at primary minimum is almost exactly one-half that at maximum and that the primary eclipse is less deep than that in the visual or longer ultraviolet wavelengths; (2) except for the 1100 to 1200 A region, the depth of the primary eclipse appears independent of wavelength; (3) the energy distribution at secondary minimum is similar to that at primary; (4) the two most prominent emission lines match well both with Si IV and C IV emission observed in gamma Vel and imply an exciting source of high temperature; (5) the emission lines do not show variation with phase.

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Available abstract

Two hundred and fourteen scans over the wavelength region 1100 A to 1800 A with 10 A resolution were obtained by OAO spacecraft for the eclipsing binary Beta Lyrae between JD 2440889.5 and JD 2440904.5. Preliminary results indicate that: (1) The intensity at primary minimum is almost exactly one-half that at maximum and that the primary eclipse is less deep than that in the visual or longer ultraviolet wavelengths; (2) except for the 1100 to 1200 A region, the depth of the primary eclipse appears independent of wavelength; (3) the energy distribution at secondary minimum is similar to that at primary; (4) the two most prominent emission lines match well both with Si IV and C IV emission observed in gamma Vel and imply an exciting source of high temperature; (5) the emission lines do not show variation with phase.

Key concepts: Eclipse, Astrophysics, Wavelength, Physics, BETA (programming language), Emission spectrum, Primary (astronomy), Binary star

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