Abstract
In this study, which is based on spectral disentangling in binary systems, ε Lupi (HD 136504) has been studied. ε Lupi is a double-lined spectroscopic binary system (SB2) consisting of two early type B stars. A total of 575 spectra of ε Lupi downloaded from the PolarBase database were used for spectral disentangling. Before spectral disentangling, we cleaned telluric lines, merged orders, normalized the continuum of spectra. To obtain individual spectra of the components, FDBinary code was used. Consequently, the spectra of the components of the ε Lupi system were separated in the wavelength range 3920 - 8560 Å. The radial velocities and atmospheric parameters of the primary and secondary components will be found using with the resultant normalized spectra of ε Lupi.
References
- [1] Simon, K. P., Sturm, E., & Fiedler, A. 1994. Spectroscopic Analysis of Hot Binaries. Astronomy and Astrophysics, 292, 507.
- [2] Pavlovski, K., Southworth, J., Tamajo, E.,2018. Physical Properties and CNO Abundances for High-Mass Stars in Four Main-Sequence Detached Eclipsing Binaries: V478 Cyg, AHCep, V453Cyg, and V578 Mon. Monthly Notice of the Royal Astronomical Society, 3129-3147.
- [3] Hadrava, P. (1995). Orbital elements of multiple spectroscopic stars. Astronomy and Astrophysics Supplement Series, 114, 393.
- [4] Ilijic, S., 2003. Spectral Disentangling of Close Binary Stars. University of Zagreb Faculty of Sciences, Degree of master, Zagreb, 65 s.
- [5] Thackeray A. D., 1970. The Double-Lined Spectroscopic Binary ɛ Lupi (HD 136504). Monthly Notice of the Royal Astronomical Society, 149, 75-80.
- [6] Campbell, W. W. & Moore, J. H., 1928. PubL Lick Obs. XVI, 223.
- [7] Moore, J. H., 1910. Lick Obs. BulLy 6, 151.
- [8] Pavlovski, K., Hensberge, H., 2006. Modern Analysis Techniques for Spectroscopic Binaries. International Astronomical Union,136-147.
- [9] Pavlovski, K., Hensberge, H., 2010. Reconstruction and Analysis of Component Spectra of Binary and Multiple Stars. Astronomical Society of Pasific, 207-216.
- [10] Simon, K. P., & Sturm, E. 1995. Disentangling of Composite Spectra. Astronomy and Astrophysics, 281, 286.
- [11] Harmanec, P., et al. 1997. The Eclipsing and Spectroscopic Binary V 436 Persei ≡ 1 Persei. Astronomy and Astrophysics, 319, 867.
- [12] Lanz, T., Hubeny, I. 2007. A Grid Of Nlte Line-Blanketed Model Atmospheres Of Early B-Type Stars. ApJS
- [13] FDBinary Web Adresi: http://sail.zpf.fer.hr/fdbinary/ (Son erişim tarihi: 16.03.2022)
- [14] PolarBase Web Adresi: http://polarbase.irap.omp.eu/ (Son erişim tarihi: 16.03.2022)
- [15] iSpec Web Adresi : https://www.blancocuaresma.com/s/iSpec/manual/introduction (son erişim tarihi: 16.03.2022)
- [16] Blanco-Cuaresma, S., et al. 2014. Determining Stellar Atmospheric Parameters and Chemical Abundances of FGK Stars with iSpec. Astronomy and Astrophysics, 569, A111.
Abstract
Çift yıldız sistemlerinde tayfsal çözümleme konusunu ele alan bu çalışmada, ε Lupi (HD 136504) yıldızı incelendi. ε Lupi iki erken tür B yıldızından oluşan çift çizgili tayfsal çift (SB2) sistemdir. Tayfsal çözümleme için ε Lupi’ye ait PolarBase arşivinden indirilen toplam 575 tayf kullanıldı. Çift sisteme ait bileşen tayfları ayırmadan önce tellürik çizgileri temizleme, tayf parçalarını(order) birleştirme, süreklilik normalizasyonu vb. işlemler uygulandı. ε Lupi’ye ait bileşen tayfların ayrı ayrı elde edilmesi için FDBinary kodu kullanıldı. Sonuç olarak, ε Lupi’nin bileşen tayfları 3920 - 8560 Å dalgaboyu aralığında ayrıldı. Bu çalışma sonucunda ε Lupi’nin bileşenlerine ait normalize tayflar kullanılarak dikine hızlar ve atmosferik parametreler bulunabilir.
References
- [1] Simon, K. P., Sturm, E., & Fiedler, A. 1994. Spectroscopic Analysis of Hot Binaries. Astronomy and Astrophysics, 292, 507.
- [2] Pavlovski, K., Southworth, J., Tamajo, E.,2018. Physical Properties and CNO Abundances for High-Mass Stars in Four Main-Sequence Detached Eclipsing Binaries: V478 Cyg, AHCep, V453Cyg, and V578 Mon. Monthly Notice of the Royal Astronomical Society, 3129-3147.
- [3] Hadrava, P. (1995). Orbital elements of multiple spectroscopic stars. Astronomy and Astrophysics Supplement Series, 114, 393.
- [4] Ilijic, S., 2003. Spectral Disentangling of Close Binary Stars. University of Zagreb Faculty of Sciences, Degree of master, Zagreb, 65 s.
- [5] Thackeray A. D., 1970. The Double-Lined Spectroscopic Binary ɛ Lupi (HD 136504). Monthly Notice of the Royal Astronomical Society, 149, 75-80.
- [6] Campbell, W. W. & Moore, J. H., 1928. PubL Lick Obs. XVI, 223.
- [7] Moore, J. H., 1910. Lick Obs. BulLy 6, 151.
- [8] Pavlovski, K., Hensberge, H., 2006. Modern Analysis Techniques for Spectroscopic Binaries. International Astronomical Union,136-147.
- [9] Pavlovski, K., Hensberge, H., 2010. Reconstruction and Analysis of Component Spectra of Binary and Multiple Stars. Astronomical Society of Pasific, 207-216.
- [10] Simon, K. P., & Sturm, E. 1995. Disentangling of Composite Spectra. Astronomy and Astrophysics, 281, 286.
- [11] Harmanec, P., et al. 1997. The Eclipsing and Spectroscopic Binary V 436 Persei ≡ 1 Persei. Astronomy and Astrophysics, 319, 867.
- [12] Lanz, T., Hubeny, I. 2007. A Grid Of Nlte Line-Blanketed Model Atmospheres Of Early B-Type Stars. ApJS
- [13] FDBinary Web Adresi: http://sail.zpf.fer.hr/fdbinary/ (Son erişim tarihi: 16.03.2022)
- [14] PolarBase Web Adresi: http://polarbase.irap.omp.eu/ (Son erişim tarihi: 16.03.2022)
- [15] iSpec Web Adresi : https://www.blancocuaresma.com/s/iSpec/manual/introduction (son erişim tarihi: 16.03.2022)
- [16] Blanco-Cuaresma, S., et al. 2014. Determining Stellar Atmospheric Parameters and Chemical Abundances of FGK Stars with iSpec. Astronomy and Astrophysics, 569, A111.
Details
| Primary Language | Turkish |
|---|---|
| Subjects | Astronomical Sciences (Other) |
| Journal Section | Research Articles |
| Authors | |
| Publication Date | June 30, 2022 |
| Published in Issue | Year 2022 Volume: 2 Issue: 1 |
