• L.N. Kondratyeva Fesenkov Astrophysical Institute, Almaty, Kazakhstan
  • E.K. Denissyuk Fesenkov Astrophysical Institute, Almaty, Kazakhstan
  • I.V. Reva Fesenkov Astrophysical Institute, Almaty, Kazakhstan
  • M.A. Krugov I.V. Reva

Ключевые слова:

protoplanetary nebulae, emission lines; B V R values; individual: IRAS20462 3416.


RAS20462 + 3416 belongs to low-mass post-AGB stars with a dense compact envelope, which was
formed in the process of the mass loss by the star at the end of the pulsating AGB phase. The spectrum of the object
consists of the HI, [NII], [SII] emission lines and of HeI, which is mainly observed in absorbtion.
The temperature of the central star corresponds to the value Teff = 19500 ± 500К, the electron density is 104
cm-3. Several episodes of gas ejection from the atmosphere of the central star were recorded. So, in 1993 - 1994,
PCygni profiles appeared in the UV and optical spectral lines. The stellar wind velocity was ~ 800 - 990 km/s. The
photometric variability of the object was noted by many authors. In particular, quasi-periodic oscillations of
brightness in the optical range with an amplitude of 0.m1 - 0.m2 and a period of ~ 4 days were detected. Rapid
fluctuations in brightness can be caused by stellar pulsations and continuing mass loss.
In this paper, we present new spectral and photometric data obtained mainly in 2015–2018. Irregular brightness
variations were detected in B, V, and R filters with an amplitude of ~ 0m.4. The results of spectral observations
indicate a gradual increase in emission line fluxes. Thus, absolute fluxes in Hβ, Hα, [NII] lines increased by about
30 – 40%.
In terms of its physical parameters and the nature of the spectrum, the object is similar to a young planetary
nebula of low excitation. However, the irregular variability of brightness and fluxes in emission lines, as well as the
observed episodes of the matter ejection, indicate that the shell formation has not finishhed. Most likely this object
can be considered as a protoplanetary nebula.