Line Identification and Photometric Observations of the Future Planetary Nebula IRAS 18062+2410 = V886 Her in 1997-1999

Details Line Identification and Photometric Observations of the Future Planetary Nebula IRAS 18062+2410 = V886 Her in 1997-1999 Line Identification and Photometric Observations of the Future Planetary Nebula IRAS 18062+2410 = V886 Her in 1997-1999

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001astl...27...99a&link_type=abstract

Astronomy Letters, vol. 27, p. 99-107 (2001)

Astronomy and Astrophysics

Astronomy

12

Protoplanetary Objects, Photometric Observations, Spectra

Scientific paper

Photoelectric UBV observations of V886 Her in 1998-1999 have shown that the pattern of its variability is retained: irregular rapid light variations with an amplitude up to 0.3 mag in V and the absence of any correlation between color and magnitude. As previously, the amplitude was at a maximum in U, which is most likely attributable to the variable Balmer continuum emitted by stellar wind. A high-resolution spectrum of the star is identified. The overwhelming majority of absorption lines, apart from HI and HeI, belong to OII, NII, CII, and SiIII. The profiles of hydrogen and helium lines are a superposition of a stellar absorption line with comparatively broad wings and a narrow strong emission feature of the envelope. The HeI 5016, 5876, and 7065 A lines have P Cyg profiles, whereas the remaining helium lines are seen in absorption. The emission spectrum of the envelope is represented by numerous permitted and forbidden lines of ionized metals and by [NII], [SII], and [OI] lines typical of planetary-nebula spectra, as well as by strong OI, NI, and SiII lines. There are no [OIII] lines. The radial velocity of the system measured from photospheric absorption features is = +55.72 km/s, while the mean radial velocity as measured from emission features of the envelope is +50.95 km/s. The object is most likely an extremely young planetary nebula.

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