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Far-Ultraviolet Spectra of Zeta Puppis and γ^{2} Velorum

1969; IOP Publishing; Volume: 155; Linguagem: Inglês

10.1086/149918

1538-4357

D. C. Morton, E. B. Jenkins, N.H. Brooks,

Astro and Planetary Science

view Abstract Citations (71) References (19) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Far-Ultraviolet Spectra of Zeta Puppis and γ^{2} Velorum Morton, Donald C. ; Jenkins, Edward B. ; Brooks, Neil H. Abstract Far-ultraviolet spectra with about 1.6-A resolution were photographed with an all-reflective objective spectrograph on an Aerobee rocket on November 1, 1967. Spectra were obtained of the 05f star ~ Puppis from 1100 to 1965 A and the WC8 + 07 star `y2 Velorum from 1127 to 1193 A. The width of the interstellar Lyman-a absorption line in ~ Pup corresponds to 4.8 X 1O'~ hydrogen atoms cm2 in front of the star. If the outer edge of its flu region is 390 Pc away the average volume density of neutral hydrogen is oniy 0.040 atoms cm3. Interstellar absorption lines of C ii, N i, Al ii, Si iii, S iii, Fe ii, and Fe iii also may be present in the ~ Pup spectrum. Strong resonance absorption lines of C iv, N v, Si iii, and Si iv and an excited line of C iii (6.5 eV) are present in ~ Pup with velocity shifts averaging 1810 km sec' toward shorter wavelengths. These lines must be formed in an expanding shell escaping from the star, similar to the shells found in the hot super- giants in Orion. Excited absorption lines of Heii (40.6 eV) and N iv (16.1 eV) have lesser shifts of 350 and 780 km sec', respectively, and therefore must be formed lower in the atmosphere where the accel- eration occurs. Emission lines of He II, C iv, N iv, and N v are visible close to their laboratory wave- lengths. Photospheric lines of C in, C iv, N in, N iv, 0 iv, Ar iv, Fe iv, and Fe v also seem to be present in ~ Pup Publication: The Astrophysical Journal Pub Date: March 1969 DOI: 10.1086/149918 Bibcode: 1969ApJ...155..875M full text sources ADS | data products SIMBAD (4)