Long-term optical spectroscopy of B[e] star CI Cam in a quiet state

封面

如何引用文章

全文:

开放存取 开放存取
受限制的访问 ##reader.subscriptionAccessGranted##
受限制的访问 订阅或者付费存取

详细

High-resolution optical spectra of the B[e] star CI Cam were obtained on arbitrary dates 2002–2023 using the 6-meter BTA telescope with the echelle spectrograph NES. The variability over time of the powerful emissions of Hα and He I profiles is found. For two-peaked emissions with «rectangular» profiles, the intensity ratio of blue-shifted and red-shifted peaks is V / R ≥ 1 , except one date. A decrease in the intensity of all two-peak emissions with «rectangular» profiles was revealed as they moved away in time from the 1998 outburst. The average radial velocity for emissions of this type for all observation dates varies in the range Vr(emis – d ) = –(50.8 – 55.7) + 0.2 km/s. The half-amplitude of the change (standard deviation) is equal to ∆Vr= 2.5 km/s. The velocity for single-peaked ion emissions (Si III, Al III, Fe III) differs little from the values of Vr(emis – d ) , but the measurement accuracy for these emissions is worse: the average error for different dates ranges from 0.4 to 1.3 km/s. The systemic velocity is assumed to be Vsys = –55.4 + 0.6 km/s according to the stable position of the forbidden emission [N II] 5754 Å. The position of single-peak emissions [O III] 4959 and 5007 Å is also stable: Vr([O III]) = –54.2 + 0.4 km/s. Emissions [O I] 5577, 6300, 6363 Å, [Ca II] 7291 and 7324 Å are absent from the spectra. Appearance of the emission near 4686 Å is an infrequent event, its intensity rarely exceeds the noise level. Only a wide asymmetric emission with an intensity of about 16% above the continuum was registered in the spectrum for 03.09.2015. Questions arise about the use of this emission to estimate the period of variability of the star and about localization of this feature in the CI Cam system. The photospheric absorptions of N II, S II, and Fe III with a variable position are identified.

全文:

受限制的访问

作者简介

V. Klochkova

Special Astrophysical Observatory RAS

编辑信件的主要联系方式.
Email: Valentina.R11@yandex.ru
俄罗斯联邦, Nizhnij Arkhyz

A. Miroshnichenko

University of North Carolina at Greensboro; Fesenkov Astrophysical Institute, Observatory

Email: Valentina.R11@yandex.ru
美国, Greensboro; Almaty, Kazakhstan

V. Panchuk

Special Astrophysical Observatory RAS

Email: Valentina.R11@yandex.ru
俄罗斯联邦, Nizhnij Arkhyz

参考

  1. P. W. Merrill and C. G. Burwell, 78, 87 (1933).
  2. J. S. Clark, A. S. Miroshnichenko, V. M. Larionov, V. M. Lyuty, et al., Astron. and Astrophys. 356, 50 (2000).
  3. E. S. Bartlett, J. S. Clark, and I. Negueruela, Astron. and Astrophys. 622, id. A93 (2019).
  4. H. J. G. L. M. Lamers, F.-J. Zickgraf, D. de Winter, L. Houziaux, and J. Zorec, Astron. and Astrophys. 340, 117 (1998).
  5. S. Miroshnichenko, V. G. Klochkova, K. S. Bjorkman, and V. E. Panchuk, Astron. and Astrophys. 390, 627 (2002).
  6. S. Beals, Monthly Not. Roy. Astron. Soc. 91, 966 (1931).
  7. F.-J. Zickgraf, Astron. and Astrophys. 408, 257 (2003).
  8. R. I. Hynes, J. S. Clark, E. A. Barsukova, P. J. Callanan, et al., Astron. and Astrophys. 392, 991 (2002).
  9. M. Kraus, Galaxies 7(4), id 83 (2019).
  10. G. Maravelias, M. Kraus, L. S. Cidale, M. Borges Fernandes, M. L. Arias, M. Curé, and G. Vasilopoulos, Monthly Not. Roy. Astron. Soc. 480(1), 320 (2018).
  11. E. L. Robinson, I. I. Ivans, and W. F. Welsh, 565(2), 1169 (2002).
  12. J. Yan, Q. Liu, and H. Hang, Astron. J. 133(4), 1478 (2007).
  13. N. D. Thureau, J. D. Monnier, W. A. Traub, R. Millan-Gabet, et al., Monthly Not. Roy. Astron. Soc. 398(3), 1309 (2009).
  14. V. P. Goranskij, E. A. Barsukova, K. S. Bjorkman, A. N. Burenkov, et al., in The B[e] Phenomenon: Forty Years of Studies, Proc. of a Conf. held at Charles University, Prague, Czech Republic 27 June–1 July 2016; edited by A. Miroshnichenko, S. Zharikov, D. Kor č aková, and M. Wolf; ASP Conf. Ser. 508 (San Francisco: Astronomical Society of the Pacific, 2017), p. 307.
  15. C. S. Kochanek, B. J. Shappee, K. Z. Stanek, T. W.-S. Holoien, et al., Publ. Astron. Soc. Pacific 129(980), 104502 (2017).
  16. V. E. Panchuk, I. D. Najdenov, V. G. Klochkova, A. B. Ivanchik, S. V. Yermakov, and V. A. Murzin, Bull. Spec. Astrophys. Observ. 44, 127 (1997).
  17. В. Е. Панчук, В. Г. Клочкова, М. В. Юшкин, Астрон. журн. 94(9), 808 (2017).
  18. М. В. Юшкин, В. Г. Клочкова, Препринт Спец. Астрофиз. Обсерв. No. 206 (2005).
  19. G. A. Galazutdinov, Astrophys. Bull. 77(4), 519 (2022).
  20. E. L. Chentsov, V. G. Klochkova, and A. S. Miroshnichenko, Astrophys. Bull. 65(2), 150 (2010).
  21. V. G. Klochkova, E. L. Chentsov, Astrophys. Bull. 71(1), 33 (2016).
  22. S. Miroshnichenko, V. G. Klochkova, E. L. Chentsov, V. E. Panchuk, M. V. Yushkin, and N. Manset, Monthly Not. Roy. Astron. Soc. 507(1), 879 (2021).
  23. F. Kupka, N. Piskunov, T. A. Raybchikova, H. C. Stempels, and W. W. Weiss, Astron. and Astrophys. Suppl. Ser. 138, 119 (1999).
  24. S. Miroshnichenko, E. L. Chentsov, V. G. Klochkova, S. V. Zharikov, et al., 700(1), 209 (2009).
  25. V. G. Klochkova, A. S. Miroshnichenko, V. E. Panchuk, N. S. Tavolzhanskaya, and M. V. Yushkin, Astron. Rep. 66(5), 429 (2022).
  26. J. P. Vallée, Astron. J. 135(4), 1301 (2008).
  27. J. Kos and T. Zwitter, 774(1), id. 72 (2013).
  28. Aret, M. Kraus, and M. Šlechta, Monthly Not. Roy. Astron. Soc. 456(2), 1424 (2016).
  29. E. A. Barsukova, N. V. Borisov, A. N. Burenkov, V. P. Goranskii, V. G. Klochkova, and N. V. Metlova, Astron. Rep. 50(8), 664 (2006).
  30. E. A. Barsukova, A. N. Burenkov, V. P. Goranskij, S. V. Zharikov, et al., Astrophys. Bull. 78(1), 1 (2023).
  31. Aret, M. L. Arias, A. Torres, L. S. Cidale, and T. Eenmäe, Boletin de la Asociacion Argentina de Astronomia 61B, 99 (2020).
  32. P. Marston and B. McCollum, Astron. and Astrophys. 477(1), 193 (2008).
  33. M. Kraus, T. Liimets, C. E. Cappa, L. S Cidale, et al., Astron. J. 154(5), id. 186 (2017).

补充文件

附件文件
动作
1. JATS XML
下载
2. Fig. 1. Hα profiles in the CI Cam spectra obtained on different dates: 18.11.2005 (orange line), 03.09.2015 (black), 21.10.2021 (red), 05.07.2022 (green), 09.02.2023 (blue). Here and in the following figures, the position of the dashed vertical corresponds to the adopted value of Vsys = –55.4 ± 0.6 km/s along the [N II] 5754 Å line, and the continuum level is taken as 1.

下载 (73KB)
索引源数据
3. Fig. 2. Profiles of characteristic emissions in the spectrum on 02/09/2023: Hα (black line), Hβ (red), He I 5876 Å (blue), Fe II 5534 Å (green), Fe II 5425 Å (orange).

下载 (132KB)
索引源数据
4. Fig. 3. Profiles of selected lines in the spectra obtained on 18.11.2008, 13.01.2011, 03.09.2015 and 09.02.2023: [N II] 5754 Å (red line), Fe II 5534 Å (black), Fe II 5234 Å (blue), Fe II 5425 Å (green).

下载 (574KB)
索引源数据
5. Fig. 4. Profiles of [N II] 5754 Å (left) and Fe II 5534 Å (right) emissions in the spectra of different dates: 04.02.2002 (orange line), 19.11.2002 (purple), 18.11.2008 (blue), 03.09.2015 (black), 08.12.2019 (thick black line), 21.10.2021 (red), 05.07.2022 (green).

下载 (300KB)
索引源数据
6. Fig. 5. Fragments of the CI Cam spectra in the wavelength range of 4665–4703 Å, obtained on different dates: 04.02.2002 (orange line), 15.01.2006 (red), 06.12.2006 (green), 07.12.2006 (blue), 18.11.2008 (brown), 03.09.2015 (black line). The position of the vertical corresponds to the wavelength of 4686 Å. Weak emission at a wavelength of about 4678 Å is not identified.

下载 (321KB)
索引源数据
7. Fig. 6. Fragments with absorptions in the CI Cam spectra, from top to bottom: 02/09/2023, 07/05/2022, 10/21/2021. The two upper fragments are shifted along the ordinate axis by 0.5 and 1.0, respectively.

下载 (239KB)
索引源数据
8. Fig. 7. Comparison of fragments containing Hα and forbidden [N II] lines in the spectra of MWC 17 (black line) and CI Cam (red), obtained with the BTA spectrograph NES in December 2005.

下载 (92KB)
索引源数据
9. Fig. 8. Comparison of fragments of the spectrum of MWC 17 (black line) and CI Cam (red), obtained with the BTA and NES spectrograph in December 2005.

下载 (176KB)
索引源数据
10. Fig. 9. Oxygen triplet O I 7773 Å (black line) in the spectrum of CI Cam obtained on 05.07.2022. The red line is the profile of the two-peak emission Fe II 5432 Å in the same spectrum.

下载 (139KB)
索引源数据
11. Fig. 10. Profiles of the Na I 5889 Å (black line) and Na I 5895 Å (red) lines in the spectrum of CI Cam obtained on 21.10.2021. The short verticals indicate the average position of the two interstellar components Vr = -7.0 km/s and -36.7 km/s of the K I 7696 Å line.

下载 (134KB)
索引源数据

版权所有 © The Russian Academy of Sciences, 2024