Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..523k&link_type=abstract
Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 3, 1991, p. 523-545.
Astronomy and Astrophysics
Astronomy
8
Balmer Series, Emission Spectra, Peculiar Stars, Stellar Spectrophotometry, Ubv Spectra, Hydrogen, Metallicity, Stellar Mass Accretion, Symbiotic Stars, White Dwarf Stars
Scientific paper
This study presents three-color photometry and spectroscopic monitoring observations of PU Vulpeculae made at Okayama from 1983 through 1989. Variable degrees of line weakening and a UV excess were found from 1983 to 1987. The weakening first appeared in Fe I and Fe II, and later also in Ti II and Sc II. B-beta was occasionally observed as an emission line during the same period. The weak-line phase continued until late 1987, when the emission lines of H Balmer, Fe II, and forbidden Fe II became dominant. An unusual brightening in the U-B color and a gradual fading of magnitude V were also observed. The radial velocity changed with an amplitude of about 50 km/s until 1985; since 1986 it has maintained an almost constant value. The origin of the line weakening is discussed in terms of a possible interaction with an emission component, and the recent activity is interpreted by a mass-accreting white-dwarf model.
Kanamitsu Osamu
Norimoto Yuji
Watanabe Etusji
Yamashita Yasumasa
Yutani Masami
No associations
LandOfFree
Weak-line to emission-line phases of PU Vulpeculae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Weak-line to emission-line phases of PU Vulpeculae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Weak-line to emission-line phases of PU Vulpeculae will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1286124