A. K. Kuratova, O. V. Zakhozhay, K. S. Kuratov, V. A. Zakhozhay, A. S. Miroshnichenko


IRAS 22150+6109 star belongs to L 1188 star forming region in Perseus, according to [1] located at distance of 910 pc from the Sun. Photometric observations in the visible range that were carried out in 1997-1999 have revealed  the  following  features  of  the  object:  source variability 0.2m, interstellar absorption reaches the value of AV = 2m [2], visual brightness of V ≈ 10.8m [3]. In near IR region (JHK bands) the emission excess is observed around 1m  in  comparison  with  visible  range:  J ≈ 9.8m,  H ≈ 9.7m, K ≈ 9.6m [4].  Flux  data  in  four  bands  contained  in  WISE catalog [5], confirmed the further increase of IR-excess in wavelength  range  of  3.4-21 µm.  According  to  AKARI catalog  [6]  where  the  emission  fluxes  are  in  wavelength range  of  18-160 µm,  IR-flux  increase  continues  nearly about  60  µm,  thereafter  it  starts  to  decrease.  Such  star’s spectral energy distribution (SED) is typical in the presence of dust disk surrounding it.  According  to  the  analysis  of  color  average  data  in optical  range  and  optical  spectrum,  star’s  spectral  classcan be determined as В2-В3 of initial main sequence [7]. Fundamental parameters assessment according to [8] is as follows: weight – 6.5 0.5 Мsun and radius – 5 Rsun.  The aim of the work is to carry out the analysis of star’s coherent  astrophysical  parameters  and  on  their  basis  todetermine parameters of the disk surrounding it.

Ключові слова

IRAS 22150+6109; protoplanetary disk

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