prikaz prve stranice dokumenta The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses
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The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses
Astronomy and Astrophysics, 637 (2020); A60. https://doi.org/10.1051/0004-6361/202037452
Tkachenko, A.; Pavlovski, Krešimir; Johnston, C.; Pedersen, M. G.; Michielsen, M.; Bowman, D. M.; Southworth, J.; Tsymbal, V.; Aerts, C.

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Tkachenko, A., Pavlovski, K., Johnston, C., Pedersen, M. G., Michielsen, M., Bowman, D. M. ... Aerts, C. (2020). The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses. Astronomy and Astrophysics, 637.. doi: 10.1051/0004-6361/202037452

Tkachenko, A., et al. "The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses." Astronomy and Astrophysics, vol. 637, 2020. https://doi.org/10.1051/0004-6361/202037452

Tkachenko, A., Krešimir Pavlovski, C. Johnston, M. G. Pedersen, M. Michielsen, D. M. Bowman, J. Southworth, V. Tsymbal i C. Aerts. "The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses." Astronomy and Astrophysics 637 (2020). https://doi.org/10.1051/0004-6361/202037452

Tkachenko, A., et al. (2020) 'The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses', Astronomy and Astrophysics, 637. doi: 10.1051/0004-6361/202037452

Tkachenko A, Pavlovski K, Johnston C, Pedersen MG, Michielsen M, Bowman DM, i sur.. The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses. Astronomy and Astrophysics [Internet]. 2020. [pristupljeno 24.12.2024.];637. doi: 10.1051/0004-6361/202037452

A. Tkachenko, et al., "The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses", Astronomy and Astrophysics, vol. 637, 2020. [Online]. Dostupno na: https://urn.nsk.hr/urn:nbn:hr:217:977533. [Citirano: 24.12.2024.]

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Podaci o radu
Naslov (engleski)The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses
AutorA. Tkachenko
AutorKrešimir Pavlovski
AutorC. Johnston
AutorM. G. Pedersen
AutorM. Michielsen
AutorD. M. Bowman
AutorJ. Southworth
AutorV. Tsymbal
AutorC. Aerts
Autorova ustanovaSveučilište u Zagrebu
Prirodoslovno-matematički fakultet
(Fizički odsjek)
Znanstveno / umjetničko
područje, polje i grana		PRIRODNE ZNANOSTI
Fizika
Astronomija i astrofizika
Sažetak (engleski)
Context.Eclipsing, spectroscopic double-lined binary star systems are excellent laboratories for calibrating theories of stellar interior structure and evolution. Their precise and accurate masses and radii measured from binary dynamics offer model-independent constraints and challenge current theories of stellar evolution.Aims.We aim to investigate the mass discrepancy in binary stars. This is the significant difference between stellar components’ masses measured from binary dynamics and those inferred from models of stellar evolution via positions of the components in the Teff−log g Kiel diagram. We study the effect of near-core mixing on the mass of the convective core of the stars and interpret the results in the context of the mass discrepancy.Methods.We fitted stellar isochrones computed from a grid of MESA stellar evolution models to a homogeneous sample of eleven high-mass binary systems. Two scenarios are considered where individual stellar components of a binary system are treated independent of each other and where they are forced to have the same age and initial chemical composition. We also study the effect of the microturbulent velocity and turbulent pressure on the atmosphere model structure and stellar spectral lines, and its link with the mass discrepancy.Results.We find that the mass discrepancy is present in our sample and that it is anti-correlated with the surface gravity of the star.No correlations are found with other fundamental and atmospheric parameters, including the stellar mass. The mass discrepancy canbe partially accounted for by increasing the amount of near-core mixing in stellar evolution models. We also find that ignoring the microturbulent velocity and turbulent pressure in stellar atmosphere models of hot evolved stars results in the overestimation of their effective temperature by up to 8%. Together with enhanced near-core mixing, this can almost entirely account for the∼30% mass discrepancy found for the evolved primary component of V380 Cyg.Conclusions.We find a strong link between the mass discrepancy and the convective core mass. The mass discrepancy can be solved by considering the combined effect of extra near-core boundary mixing and the consistent treatment in the spectrum analysis of hot evolved stars. Our binary modelling results in convective core masses between 17 and 35% of the stellar mass, which is in excellent agreement with the results from gravity-mode asteroseismology of single stars. This implies larger helium core masses near the end of the main sequence than have been anticipated so far.
Ključne riječi (engleski)
Jezikengleski
Vrsta publikacijeZnanstveni rad - Izvorni znanstveni rad
Status objaveObjavljen
Vrsta recenzijeRecenziran - međunarodna recenzija
Verzija publikacijeObjavljena verzija rada (izdavačev PDF)
Naslov časopisaAstronomy and Astrophysics
Brojčani podacivol. 637, A60
p-ISSN0004-6361
e-ISSN1432-0746
DOIhttps://doi.org/10.1051/0004-6361/202037452
URN:NBNurn:nbn:hr:217:977533
Datum objave publikacije2020
ProjektŠifra: IP-2014-09-8656
Naziv (hrvatski): Zvijezde i prašina: struktura, sastav i interakcija
Kratica: STARDUST
Voditelj: Krešimir Pavlovski
Pravna nadležnost: Hrvatska
Financijer: HRZZ
Linija financiranja: IP
URL dokumentahttps://www.aanda.org/articles/aa/abs/2020/05/aa37452-20/aa37452-20.html
Vrsta resursaTekst
Prava pristupaOtvoreni pristup
Uvjeti korištenjaIkona licence Zaštićeno autorskim pravom.
Javna napomena© ESO 2020. Received 7 January 2020. Accepted 19 March 2020. Published online 14 May 2020.
Datum i vrijeme pohrane2020-08-27 19:44:37