Abstract
High-resolution optical spectra of the IR source IRAS01005+7910 are used to determine the spectral type of its central star, B1.5±0.3, identify the spectral features, and analyze their profile and radial-velocity variations. The systemic velocity V sys = −50.5 km s−1 is determined from the positions of the symmetric and stable profiles of the forbidden [NI], [N II], [OI], [S II], and [Fe II] emission lines. The presence of the [NII] and [SII] forbidden emissions indicates the onset of the ionization of the circumstellar envelope and the fact that the star is very close to undergoing the planetary nebula stage. The broad range of radial velocity V r estimates based on the line cores, which amounts to about 34 km s−1, is partly due to the deformations of the profiles caused by variable emissions. The variations of the V r in the line wings are smaller, about 23 km s−1, and may be due to pulsations and/or hidden binarity of the star. The deformations of the profiles of absorption-emission lines may result from variations of their absorption components caused by the variations of the geometry and kinematics in the wind base. The Hα lines exhibit PCyg III type wind profiles. Deviations of the wind from spherical symmetry are shown to be small. The relatively low wind velocity (27–74 km s−1 from different observations) and the strong intensity of the red emission (it exceeds the continuum level by up to a factor of seven) are typical for hypergiants rather than the classical supergiants. IRAS01005 is an example of spectral mimicry of a low-mass post-AGB star masquerading as a massive hypergiant.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
B. W. Lewis, Astrophys. J. 338, 234 (1989).
L. Likkel, Astrophys. J. 344, 350 (1989).
L. Likkel, T. Forveille, A. Omont, and M. Morris, Astron. and Astrophys. 246, 153 (1991).
L.-A. Nyman, R. S. Booth, U. Carlström, et al., Astron. and Astrophys. Suppl. 93, 121 (1992).
A. Omont, C. Loup, T. Forveille, et al., Astron. and Astrophys. 267, 515 (1993).
J. Y Hu, P. Te Lintel Hekkert, S. Slijkhuis, et al., Astron. and Astrophys. Suppl. 103, 310 (1994).
V. G. Klochkova, M. V. Yushkin, A. S. Miroshnichenko, et al., Astron. and Astrophys. 392, 143 (2002).
Y. Zhang and S. Kwok, Astrophys. J. 730, 126 (2011).
S. Iglesias-Groth and M. Esposito, Astrophys. J. 776, L2 (2013).
B. J. Hrivnak, T. R. Geballe, and S. Kwok, Astrophys. J. 662, 1059 (2007).
B. J. Hrivnak, W. Lu, R. Maupin, and B. D. Spitzbart, Astrophys. J. 709, 1042 (2010).
V. P. Arkhipova, M. A. Burlak, V. F. Esipov, et al., Astronomy Letters 39, 619 (2013).
J. Y. Hu, in: Proc. Torun Workshop on Post-AGB Objects as a Phase of Stellar Evolution, Ed. by R. Szczerba and S. K. Górny (Kluwer Acad. Publ., 2001), p. 317.
V. Panchuk, V. Klochkova, M. Yushkin, and I. Najdenov, in: Proc. IAU General Assembly, Joint Discussion No. 4, Ed. by A. I. Gomez de Castro and M. A. Barstow (Editorial Complutense, Madrid, 2007), p. 179.
V. Panchuk, V. Klochkova, M. Yushkin, and I. Najdenov, J. Optical Technology, 76, 87 (2009).
G. A. Galazutdinov, Preprint No. 92 (Special Astrophysical Observatory, Mizhnii Arkhyz, 1992).
N. Siódmiak, M. Meixner, T. Ueta, et al., Astrophys. J. 677, 382 (2008).
A. A. Ferro, Publ. Astron. Soc. Pacific 96, 641 (1984).
L. B. F. M. Waters, C. Waelkens, M. Mayor, and N. R. Trams, Astron. and Astrophys. 269, 242 (1993).
H. van Winckel, C. Waelkens, and L. B. F. M. Waters, Astron. and Astrophys. 293, L25 (1995).
A. Gautschy, Monthly Notices Royal Astron. Soc. 265, 340 (1993).
V. G. Klochkova, Monthly Notices Royal Astron. Soc. 272, 710 (1995).
A. Lèbre, N. Mauron, D. Gillet, and D. Barthès, Astron. and Astrophys. 310, 923 (1996).
D. Barthès, A. Lèbre, D. Gillet, and N. Mauron, Astron. and Astrophys. 359, 168 (2000).
V. G. Klochkova, E. L. Chentsov, N. S. Tavolganskaya, and M. V. Shapovalov, Astrophysical Bulletin 62, 105 (2007).
V. G. Klochkova and E. L. Chentsov, Astronomy Reports 51, 994 (2007).
B. J. Hrivnak, W. Lu, J. Sperauskas, et al., Astrophys. J. 766, 116 (2013).
A. B. Fokin, A. Lèbre, H. Le Coroller, and D. Gillet, Astron. and Astrophys. 378, 546 (2001).
V. G. Klochkova, Astrophysical Bulletin 69, 279 (2014).
V. G. Klochkova, E. L. Chentsov, N. S. Tavolzhanskaya, and V. E. Panchuk, AstronomyReports 51, 642 (2007).
A. S. Miroshnichenko, E. L. Chentsov, V. G. Klochkova, et al., Astrophys. J. 700, 209 (2009).
F. Cazzolato and S. Pineault, Astron. J. 125, 2050 (2003).
V. G. Klochkova, V. E. Panchuk, and N. S. Tavolganskaya, Astronomy Letters 41 (2015) (in press).
C. Loup, T. Forveille, A. Omont, and J. F. Paul, Astron. and Astrophys. Suppl. 99, 291 (1993).
R. Luna, N. L. J. Cox, M. A. Satorre, et. al. Astron. and Astrophys. 480, 133 (2008).
E. L. Chentsov and A. N. Sarkisyan, Astrophysical Bulletin 62, 257 (2007).
V. P. Arkhipova, N. P. Ikonnikova, R. I. Noskova, et al., Astronomy Letters 27, 719 (2001).
V. P. Arkhipova, V. G. Klochkova, and G. V. Sokol, Astronomy Letters 27, 99 (2001).
G. Sarkar, D. A. Garcia-Hernández, M. Parthasarathy, et al., Monthly Notices Royal Astron. Soc. 421, 679 (2012).
G. Sarkar, M. Parthasarathy, and B. E. Reddy, Astron. and Astrophys. 431, 1007 (2005).
D. R. C. Mello, S. Daflon, C. B. Pereira, and I. Hubeny, Astron. and Astrophys. 543, A11 (2012).
G. Gauba and M. Parthasarathy, Astron. and Astrophys. 417, 201 (2004).
V. P. Arkhipova, N. P. Ikonnikova, R. I. Noskova, et al., Astronomy Letters 25, 25 (1999).
M. Parthasarathy, P. Garcia-Lario, Y. Sivarani, et al., Astron. and Astrophys. 357, 241 (2000).
V. P. Arkhipova, V. F. Esipov, N. P. Ikonnikova, et al., Astronomy Letters 33, 604 (2007).
Author information
Authors and Affiliations
Corresponding author
Additional information
Original Russian Text © V.G. Klochkova, E.L. Chentsov, V.E. Panchuk, E.G. Sendzikas, M.V. Yushkin, 2014, published in Astrofizicheskii Byulleten, 2014, Vol. 69, No. 4, pp. 464–479.
Rights and permissions
About this article
Cite this article
Klochkova, V.G., Chentsov, E.L., Panchuk, V.E. et al. Spectral variability of the IR source IRAS 01005+7910 optical component. Astrophys. Bull. 69, 439–453 (2014). https://doi.org/10.1134/S1990341314040063
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1134/S1990341314040063