Spectroscopy and photometry of the protoplanetary nebula candidate stHα62 = IRAS 07171+1823

Details Spectroscopy and photometry of the protoplanetary nebula candidate stHα62 = IRAS 07171+1823 Spectroscopy and photometry of the protoplanetary nebula candidate stHα62 = IRAS 07171+1823

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006astl...32..661a&link_type=abstract

Astronomy Letters, vol. 32, Issue 10, p.661-670

Astronomy and Astrophysics

Astronomy

2

Pacs Numbers 97.30.Eh, 97.10.Fy, 97.20.Ec, 97.82.Jw

Scientific paper

We present the results of spectroscopic and photometric observations for the B star StHα62 with an IR excess, a post-AGB candidate identified with the IR source IRAS 07171+1823. High-resolution spectroscopy has allowed the λ4330 7340 Å spectrum of the star to be identified: it contains absorption lines of an early B star and emission lines of a gaseous shell. The residual line intensities have been measured. The heliocentric radial velocities measured from absorption lines of the star and emission lines of the shell are = +45 ± 1 and +52 ± 1 km s-1, respectively. The line-of-sight velocities of gas-dust clouds determined from the interstellar Na I lines are 12 and 33 km s-1. The He I λ5876 Å line exhibits a P Cyg profile, which is indicative of an ongoing mass loss by the star. The expansion velocity of the outer shell estimated from forbidden lines is 12 13 km s-1. Quantitative classification gives the spectral type B0.51 for the star. The parameters of the gaseous shell have been determined: N e = 3.1 × 103 cm-3 and T e ˜ 21 000 K. Over 4 years of its observations, the star showed rapid irregular light variations with the amplitudes ΔV = &
$0(m) .2
; , ΔB = &
0(m) .2
; , and ΔU = &
0(m) .3
; and no color-magnitude correlation. We estimate the total extinction for the star from our photometric observations as A v = &
0(m) .4$
; . Near-IR observations have revealed dust radiation with a temperature of ˜1300 K. We estimate the distance to StHα62 to be r = 5.2 ± 1.2 kpc by assuming that the star is a low-mass (M = 0.55 ± 0.05 M &sun;) protoplanetary nebula.

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