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

Мұқаба

Дәйексөз келтіру

Толық мәтін

Ашық рұқсат Ашық рұқсат
Рұқсат жабық Рұқсат берілді
Рұқсат жабық Рұқсат ақылы немесе тек жазылушылар үшін

Аннотация

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.

Толық мәтін

Рұқсат жабық

Авторлар туралы

V. Klochkova

Special Astrophysical Observatory RAS

Хат алмасуға жауапты Автор.
Email: Valentina.R11@yandex.ru
Ресей, Nizhnij Arkhyz

A. Miroshnichenko

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

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

V. Panchuk

Special Astrophysical Observatory RAS

Email: Valentina.R11@yandex.ru
Ресей, Nizhnij Arkhyz

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Әрекет
1. JATS XML
Жүктеу
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.

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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).

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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).

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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).

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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.

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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.

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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.

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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.

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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.

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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.

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