prikaz prve stranice dokumenta Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis
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Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis
Astronomy & Astrophysics, 658 (2022); A92. https://doi.org/10.1051/0004-6361/202142292
Pavlovski, Krešimir; Hummel, C. A.; Tkachenko, A.; Dervişoğlu, A.; Kayhan, C.; Zavala, R. T.; Hutter, D. J.; Tycner, C.; Şahin, T.; Audenaert, J.; Baeyens, R.; Bodensteiner, J.; Bowman, D. M.; Gebruers, S.; Jannsen, N. E.; Mombarg, J. S. G. Više autora...

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Pavlovski, K., Hummel, C. A., Tkachenko, A., Dervişoğlu, A., Kayhan, C., Zavala, R. T. ... Mombarg, J. S. G. (2022). Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis. Astronomy & Astrophysics, 658.. doi: 10.1051/0004-6361/202142292

Pavlovski, Krešimir, et al. "Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis." Astronomy & Astrophysics, vol. 658, 2022. https://doi.org/10.1051/0004-6361/202142292

Pavlovski, Krešimir, C. A. Hummel, A. Tkachenko, A. Dervişoğlu, C. Kayhan, R. T. Zavala, D. J. Hutter, et al. "Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis." Astronomy & Astrophysics 658 (2022). https://doi.org/10.1051/0004-6361/202142292

Pavlovski, K., et al. (2022) 'Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis', Astronomy & Astrophysics, 658. doi: 10.1051/0004-6361/202142292

Pavlovski K, Hummel CA, Tkachenko A, Dervişoğlu A, Kayhan C, Zavala RT, i sur.. Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis. Astronomy & Astrophysics [Internet]. 04.02.2022. [pristupljeno 24.12.2024.];658. doi: 10.1051/0004-6361/202142292

K. Pavlovski, et al., "Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis", Astronomy & Astrophysics, vol. 658, Veljača 2022. [Online]. Dostupno na: https://urn.nsk.hr/urn:nbn:hr:217:703276. [Citirano: 24.12.2024.]

Za citiranje koristite ovu mrežnu adresu: https://urn.nsk.hr/urn:nbn:hr:217:703276
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Naslov (engleski)Dynamical parallax, physical parameters, and evolutionary status of the components of the bright eclipsing binary α Draconis
AutorKrešimir Pavlovski
AutorC. A. Hummel
AutorA. Tkachenko
AutorA. Dervişoğlu
AutorC. Kayhan
AutorR. T. Zavala
AutorD. J. Hutter
AutorC. Tycner
AutorT. Şahin
AutorJ. Audenaert
AutorR. Baeyens
AutorJ. Bodensteiner
AutorD. M. Bowman
AutorS. Gebruers
AutorN. E. Jannsen
AutorJ. S. G. Mombarg
Autorova ustanovaSveučilište u Zagrebu
Prirodoslovno-matematički fakultet
(Fizički odsjek)
Znanstveno / umjetničko
područje, polje i grana		PRIRODNE ZNANOSTI
Fizika
Sažetak (engleski)
Aims: Both components of the bright eclipsing binary α Dra have been resolved using long baseline interferometry and the secondary component has been shown to contribute approximately 15% of the total flux ; however, a spectroscopic detection of the companion star has so far been unsuccessful. We aim for a firm spectroscopic detection of the secondary component of α Dra using state-of-the-art spectroscopic analysis methods for very high-quality spectroscopic observations. This will allow the determination of fundamental and atmospheric properties of the components in the system with high precision and accuracy. Methods: To achieve our goals, we use a combined data set from interferometry with the Navy Precision Optical Interferometer (NPOI), photometry with the TESS space observatory, and high-resolution spectroscopy with the HERMES fibre-fed spectrograph at the La Palma observatory. We use the method of spectral disentangling to search for the contribution of a companion star in the observed composite HERMES spectra, to separate the spectral contributions of both components, and to determine orbital elements of the α Dra system. TESS light curves are analysed in an iterative fashion with spectroscopic inference of stellar atmospheric parameters to determine fundamental stellar properties and their uncertainties. Finally, NPOI interferometric measurements are used for determination of the orbital parameters of the system and angular diameters of both binary components. Results: We report the first firm spectroscopic detection of the secondary component in α Dra and deliver disentangled spectra of both binary components. The components' masses and radii are inferred with high precision and accuracy, and are M_A = 3.186 ± 0.044 M⊙, R_A = 4.932 ± 0.036 R⊙, and M_B = 2.431 ± 0.019 M⊙, R_B = 2.326 ± 0.052 R⊙ for the primary and secondary components, respectively. Combined astrometric and spectroscopic analysis yields the semi-major axis of the system, which is ultimately used to derive the dynamical parallax of π = 11.48 ± 0.13 mas, and the distance d = 87.07 ± 1.03 pc to the α Dra system. Evolutionary analysis of both binary components with MESA stellar structure and evolution models suggests the primary is an evolved post-TAMS A-type star, while the companion is a main-sequence A-type star with a convective core mass of M_cc = 0.337 ± 0.011 M⊙. Positions of both binary components in the Kiel- and HR-diagrams suggest a value of the convective core overshooting parameter f_ov well below 0.010 H_p, and we infer the age of the system to be 310 ± 25 Myr. Conclusions: The inferred near-core mixing properties of both components do not support a dependence of the convective core overshooting on the stellar mass. At the same time, the α Dra system provides extra support to hypothesise that the mass discrepancy in eclipsing spectroscopic double-lined binaries is associated with inferior atmospheric modelling of intermediate- and high-mass stars, and less so with the predictive power of stellar structure and evolution models as to the amount of near-core mixing and mass of the convective core.
Ključne riječi (hrvatski)
Jezikengleski
Vrsta publikacijeZnanstveni rad - Izvorni znanstveni rad
Status objaveObjavljen
Vrsta recenzijeRecenziran - međunarodna recenzija
Verzija publikacijeObjavljena verzija rada (izdavačev PDF)
Naslov časopisaAstronomy & Astrophysics
Brojčani podacivol. 658, A92
p-ISSN0004-6361
e-ISSN1432-0746
DOIhttps://doi.org/10.1051/0004-6361/202142292
URN:NBNurn:nbn:hr:217:703276
Datum objave publikacije2022-02-04
URL dokumentahttps://www.aanda.org/10.1051/0004-6361/202142292
Vrsta resursaTekst
Prava pristupaOtvoreni pristup
Uvjeti korištenjaIkona licence Zaštićeno autorskim pravom.
Javna napomena© ESO 2022. Received 23 September 2021. Accepted 2 November 2021. Published online 04 February 2022. Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.
Datum i vrijeme pohrane2024-08-09 18:55:16