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HD 199719’un Çizgi Ortay Analizi

Year 2020, Volume: 15 Issue: 1, 90 - 99, 31.05.2020
https://doi.org/10.29233/sdufeffd.676757

Abstract

Bu çalışmada, TÜBİTAK Ulusal Gözlemevinde (TUG) devam etmekte olan ötegezegen araştırmasının bir parçası olarak HD 199719’un tayfsal çizgi ortaylarının (bisektör) değişimleri incelendi. Gözlemsel tayflara bir şablon tayf ile çapraz korelasyon fonksiyonları (CCF) uygulanarak, ortalama çizgi profilleri elde edildi. Bu profillerden çizgi ortayları belirlendi. Bu çizgi ortaylarını nicel olarak tanımlamak için çizgi ortay ölçütleri kullanıldı. Bu ölçütler ile çizgi profillerindeki hız alanları hesaplandı ve dikine hız ölçümleri arasındaki ilişki araştırıldı. Yıldızın doğası kaynaklı (bulgurlanma (granülasyon), zonklama (pulsasyon), manyetik etkinlik kaynaklı yüzey lekeleri ve manyetik çevrim gibi) etkileri araştırmak için çizgi ortayların yanı sıra, Hα ve H çizgilerinin eşdeğer genişlik ölçümleri de yapıldı. Yıldızın çizgi ortay hız ile dikine hız değerleri arasında bir korelasyon olmadığı görüldü. Çizgi ortay hız ölçümleri (BIS ve BVC) için yapılan dönem analizlerinde 4.88 ve 10.36 günlük dönemleri işaret eden pikler elde edildi. Hα’nın eşdeğer genişlik ölçümleri için uzun dönemli bir değişim olabileceği görülse de, benzer bir değişim H’nın eşdeğer genişlik ölçümlerinde elde edilmedi.

Supporting Institution

TÜBİTAK

Project Number

114F099

Thanks

Çalışma kapsamında yıldızın gözlemlerinde kullanılan RTT150 (Antalya’da Tübitak Ulusal Gözlemevinde bulunan 1,5 m’lik teleskop) ve 15ARTT150-718 proje kapsamındaki destekleri için TÜBİTAK’a teşekkür ederiz. Fotometrik gözlemlerin gerçekleştiği Ankara Üniversitesi Kreiken Rasathanesi’ne desteklerinden dolayı teşekkür ederiz. Bu çalışma 114F099 numaralı TÜBİTAK Projesi kapsamında desteklenmiştir.

References

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  • [2] S. H. Saar and R. A. Donahue, “Activity-Related Radial Velocity Variation in Cool Stars,” The Astrophysical J., 485(1), 319 – 327,1997.
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  • [4] G L. Lindegren and D. Dravins, “The fundamental definition of ‘radial velocity,” Astronomy & Astrophysics, 401(3),1185 – 1201, 2003.
  • [5] D. Queloz, G. W. Henry, J. P. Sivan, S. L. Baliunas, J. L. Beuzit, R. A. Donahue, M. Mayor, D. Naef, C. Perrier, and S. Udry, “No planet for HD 166435,” Astronomy and Astrophysics, 379, 279 – 287, 2001.
  • [6] D. F. Gray, Lectures on Spectral-line Analysis: F,G, and K stars. Arva: Ontario Gray, 1988, pp. 308.
  • [7] A. P. Hatzes, M. Fridlund, G. Nachmani, T. Mazeh, D. Valencia, G. Hébrard, L. Carone, M. Pätzold, S. Udry, F. Bouchy, M. Deleuil, C. Moutou, P. Barge, P. Bordé, H. Deeg, B. Tingley, R. Dvorak, D. Gandolfi, S. Ferraz-Mello, G. Wuchterl, E. Guenther, T. Guillot, H. Rauer, A. Erikson, J. Cabrera, S. Csizmadia, A. Léger, H. Lammer, J. Weingrill, D. Queloz, R. Alonso, D. Rouan, and J. Schneider, “The Mass of CoRoT-7b,” The Astrophysical J., 743 (1), 75, 2011.
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  • [9] X. Dumusque, N. C. Santos, S. Udry, C. Lovis, and X. Bonfils, “Planetary detection limits taking into account stellar noise. II. Effect of stellar spot groups on radial-velocities,” Astronomy & Astrophysics, 527, A182, 2011b.
  • [10] I. Boisse, F. Bouchy, G. Hébrard, X. Bonfils, N. Santos, and S. Vauclair, “Disentangling between stellar activity and planetary signals,” Astronomy & Astrophysics, 528, A4, 2011.
  • [11] S. Aigrain, F. Pont and S. Zucker, “A simple method to estimate radial velocity variations due to stellar activity using photometry,” Monthly Notices of the Royal Astronomical Society, 419 (4), 3147–3158, 2012.
  • [12] M. Yılmaz, B. Sato, I. Bikmaev, S. O. Selam, H. Izumiura, V. Keskin, E. Kambe, S. S. Melnikov, A. Galeev, İ. Özavcı, E. N. Irtuganov, and R. Ya Zhuchkov, “A Jupiter-mass planet around the K0 giant HD 208897,” Astronomy & Astrophysics, 608, A14,2017.
  • [13] M. Yılmaz, S. O. Selam, B. Sato, I. Bikmaev, H. Izumiura, V. Keskin, and E. Kambe, “The line bisectors of G type giant star HD 199719,” in Proc. The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Uppsala, 2016.
  • [14] R. P. Butler, G. W. Marcy, E. Williams, C. McCarthy, S. S. Vogt, and P. Dosanjh, “Attaining doppler precision of 3 M s-1,” Publications of the Astronomical Society of the Pacific, 108, 500, 1996.
  • [15] Networks[Online]. Available: https://www.harrisgeospatial.com/Software-Technology/IDL#language
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  • [18] O. Kochıkhov. Networks[Online]. Available: https://www.astro.uu.se/~oleg/binmag.html
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  • [20] T. Ryabchikova, N. Piskunov, R. L. Kurucz, H. C. Stempels, U. Heiter, Yu Pakhomov and P S Barklem, “A major upgrade of the VALD database,” Physica Scripta (IOP), 90 (5), 054005 (4pp), 2015.
  • [21] F. Castelli and R. L. Kurucz, “New grids of ATLAS9 model atmospheres,” in Proc. IAU Symposium Modelling of Stellar Atmospheres, 2004.
  • [22] T. H. Dall, N. C. Santos, T. Arentoft, T. R. Bedding, and H. Kjeldsen, “Bisectors of the Cross Correlation Function Applied to Stellar Spectra,” Astronomy & Astrophysics, 454, 341–348 2006.
  • [23] B.C. Lee, I. Hank, M. G. Park, D. E. Mkrtichan, A. P. Hatzes, G. Jeong, and K. M. Kim, “Long-period variations in the radial velocity of spectroscopic binary M giant μ Ursae Majoris,” The Astronomical J., 151(4), 106, 2016.
  • [24] D. F. Gray, The Observation and Analysis of Stellar Photospheres, 3rd edition, Cambridge, Press: Cambridge University, 533, 2005.

Bisector Analysis of HD 199719

Year 2020, Volume: 15 Issue: 1, 90 - 99, 31.05.2020
https://doi.org/10.29233/sdufeffd.676757

Abstract

In this study, an analysis of spectral line bisector variations for HD 199719 which was examined as a part of the exoplanet studies that carried on the TÜBİTAK National Observatory (TUG). Cross-correlation functions (CCF) were implemented to the observed spectra using some template spectra to determine mean line profile. Line bisectors were derived from mean line profiles. In order to quantify asymmetries on the line profiles, some bisectors criteria were used. The velocity spans were calculated in the profiles with these criteria and correlation between the star’s radial velocity measurements were investigated. In addition, equivalent width measurements of the Hα and H were performed to check other variability due to nature of star (granulation, pulsation, magnetic cycle and stellar spots due to activity). No correlation has been found between the radial velocity and line bisectors measurements. Period analysis for bisectors (BIS and BVC) show that significant periodicity appearing around 4.88 and 10.36 days. Although there was a long-term variation for the equivalent width measurements of Hα, a similar change was not obtained for equivalent width measurements of H.

Project Number

114F099

References

  • [1] V. V. Makarov, C. A. Beichman, J. H. Catanzarite, D. A. Fischer, J. Lebreton, F. Malbet, and M. Shao, “Starspot jitter in photometry, astrometry and radial velocity measurements,” The Astrophysical J.,707(1), L73 – L76, 2009.
  • [2] S. H. Saar and R. A. Donahue, “Activity-Related Radial Velocity Variation in Cool Stars,” The Astrophysical J., 485(1), 319 – 327,1997.
  • [3] C. J. Schrijver and C. Zwaan, Solar and Stellar Magnetic Activity. Cambridge (Reino Unido): Cambridge University Press, 2000.
  • [4] G L. Lindegren and D. Dravins, “The fundamental definition of ‘radial velocity,” Astronomy & Astrophysics, 401(3),1185 – 1201, 2003.
  • [5] D. Queloz, G. W. Henry, J. P. Sivan, S. L. Baliunas, J. L. Beuzit, R. A. Donahue, M. Mayor, D. Naef, C. Perrier, and S. Udry, “No planet for HD 166435,” Astronomy and Astrophysics, 379, 279 – 287, 2001.
  • [6] D. F. Gray, Lectures on Spectral-line Analysis: F,G, and K stars. Arva: Ontario Gray, 1988, pp. 308.
  • [7] A. P. Hatzes, M. Fridlund, G. Nachmani, T. Mazeh, D. Valencia, G. Hébrard, L. Carone, M. Pätzold, S. Udry, F. Bouchy, M. Deleuil, C. Moutou, P. Barge, P. Bordé, H. Deeg, B. Tingley, R. Dvorak, D. Gandolfi, S. Ferraz-Mello, G. Wuchterl, E. Guenther, T. Guillot, H. Rauer, A. Erikson, J. Cabrera, S. Csizmadia, A. Léger, H. Lammer, J. Weingrill, D. Queloz, R. Alonso, D. Rouan, and J. Schneider, “The Mass of CoRoT-7b,” The Astrophysical J., 743 (1), 75, 2011.
  • [8] O. Lozitsky, “Creation and usage of program code for strong subtelescopic solar magnetic field diagnostics,” in Proc. 21th Young Scientists' Conference on Astronomy and Space Physics, Kyiv, 2014, pp. 34–35.
  • [9] X. Dumusque, N. C. Santos, S. Udry, C. Lovis, and X. Bonfils, “Planetary detection limits taking into account stellar noise. II. Effect of stellar spot groups on radial-velocities,” Astronomy & Astrophysics, 527, A182, 2011b.
  • [10] I. Boisse, F. Bouchy, G. Hébrard, X. Bonfils, N. Santos, and S. Vauclair, “Disentangling between stellar activity and planetary signals,” Astronomy & Astrophysics, 528, A4, 2011.
  • [11] S. Aigrain, F. Pont and S. Zucker, “A simple method to estimate radial velocity variations due to stellar activity using photometry,” Monthly Notices of the Royal Astronomical Society, 419 (4), 3147–3158, 2012.
  • [12] M. Yılmaz, B. Sato, I. Bikmaev, S. O. Selam, H. Izumiura, V. Keskin, E. Kambe, S. S. Melnikov, A. Galeev, İ. Özavcı, E. N. Irtuganov, and R. Ya Zhuchkov, “A Jupiter-mass planet around the K0 giant HD 208897,” Astronomy & Astrophysics, 608, A14,2017.
  • [13] M. Yılmaz, S. O. Selam, B. Sato, I. Bikmaev, H. Izumiura, V. Keskin, and E. Kambe, “The line bisectors of G type giant star HD 199719,” in Proc. The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Uppsala, 2016.
  • [14] R. P. Butler, G. W. Marcy, E. Williams, C. McCarthy, S. S. Vogt, and P. Dosanjh, “Attaining doppler precision of 3 M s-1,” Publications of the Astronomical Society of the Pacific, 108, 500, 1996.
  • [15] Networks[Online]. Available: https://www.harrisgeospatial.com/Software-Technology/IDL#language
  • [16] F. Van Leeuwen, “Validation of the new Hipparcos reduction,” Astronomy & Astrophysics, 474, 653–664, 2007.
  • [17] D. J. Schlegel, D. P. Finkbeiner, and M. Davis, “Maps of duts infrared emission for use in estimation of reddening and cosmic microwave background radiations foregrounds,” The Astrophysical J., 500, 525-553, 1998.
  • [18] O. Kochıkhov. Networks[Online]. Available: https://www.astro.uu.se/~oleg/binmag.html
  • [19] P.O. Kochukhov, “Spectrum synthesis for magnetic, chemically stratified stellar atmospheres,” in Proc. Physics of Magnetic Stars. Proceedings of the International Conference, Uppsala, 2007, 109.
  • [20] T. Ryabchikova, N. Piskunov, R. L. Kurucz, H. C. Stempels, U. Heiter, Yu Pakhomov and P S Barklem, “A major upgrade of the VALD database,” Physica Scripta (IOP), 90 (5), 054005 (4pp), 2015.
  • [21] F. Castelli and R. L. Kurucz, “New grids of ATLAS9 model atmospheres,” in Proc. IAU Symposium Modelling of Stellar Atmospheres, 2004.
  • [22] T. H. Dall, N. C. Santos, T. Arentoft, T. R. Bedding, and H. Kjeldsen, “Bisectors of the Cross Correlation Function Applied to Stellar Spectra,” Astronomy & Astrophysics, 454, 341–348 2006.
  • [23] B.C. Lee, I. Hank, M. G. Park, D. E. Mkrtichan, A. P. Hatzes, G. Jeong, and K. M. Kim, “Long-period variations in the radial velocity of spectroscopic binary M giant μ Ursae Majoris,” The Astronomical J., 151(4), 106, 2016.
  • [24] D. F. Gray, The Observation and Analysis of Stellar Photospheres, 3rd edition, Cambridge, Press: Cambridge University, 533, 2005.
There are 24 citations in total.

Details

Primary Language Turkish
Subjects Metrology, Applied and Industrial Physics
Journal Section Makaleler
Authors

Didem Dilan İzci 0000-0002-7870-2008

Mesut Yılmaz 0000-0002-3276-0704

Project Number 114F099
Publication Date May 31, 2020
Published in Issue Year 2020 Volume: 15 Issue: 1

Cite

IEEE D. D. İzci and M. Yılmaz, “HD 199719’un Çizgi Ortay Analizi”, Süleyman Demirel University Faculty of Arts and Science Journal of Science, vol. 15, no. 1, pp. 90–99, 2020, doi: 10.29233/sdufeffd.676757.