Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007astl...33..604a&link_type=abstract
Astronomy Letters, Volume 33, Issue 9, pp.604-614
Astronomy and Astrophysics
Astronomy
5
Scientific paper
We present our long-term photometric and spectroscopic observations of a high-latitude B supergiant with an infrared excess—the protoplanetary nebula IRAS 18062+2410. Our U BV observations in 2000 2006 have confirmed the rapid irregular photometric variability of the star with a maximum amplitude as high as 0{./ m }4 in V that we found previously. The B— V and U— B color indices vary with amplitudes as high as 0{./ m }10 and 0{./ m }25, respectively, and show no clear correlation with the brightness. Our V-band CCD observations on 11 nights in 2006 have revealed brightness trends during the night. The variability of IRAS18062+2410 is similar in pattern to the light variations in other hot post-AGB objects and some of the nuclei of young planetary nebulae. We assume that pulsations and a variable stellar wind can be responsible for the variability of these stars. In addition to the rapid variability, our 12-year-long observations have revealed a systematic decline in the mean brightness of IRAS 18062+2410. This may be related to a rise in the temperature of the star at constant luminosity as a result of its evolution. Low-resolution spectroscopic observations have shown a systematic increase in the equivalent widths of the H α, H β, [NII]λ6584 Å, OI λ8446 Å, and [OII] λ7320 7330 Å emission lines. The changes in the star’s emission line spectrum are probably caused by an increase in the degree of ionization of the gas shell due to a rise in the temperature of the ionizing star. Our photometric and spectroscopic observations of IRAS 18062+2410 confirm the previously made assumptions that the star evolves very rapidly to the region of planetary nebulae.
Arkhipova V. P.
Esipov Valentine F.
Ikonnikova N. P.
Komissarova G. V.
Noskova R. I.
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