prikaz prve stranice dokumenta The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3
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Scientific paper - Original scientific paper
The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3
Astronomy & Astrophysics, 649 (2021); A109. https://doi.org/10.1051/0004-6361/202140571
Graczyk, D.; Pietrzyński, G.; Galan, C.; Gieren, W.; Tkachenko, A.; Anderson, R. I.; Gallenne, A.; Górski, M.; Hajdu, G.; Kałuszyński, M.; Karczmarek, P.; Kervella, P.; Maxted, P. F. L.; Nardetto, N.; Narloch, W.; Pavlovski, Krešimir; Pilecki, B.; Pych, W.; Southworth, J.; Storm, J.; Suchomska, K.; Taormina, M.; Villanova, S.; Wielgórski, P.; Zgirski, B.; Konorski, P. More authors...

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Graczyk, D., Pietrzyński, G., Galan, C., Gieren, W., Tkachenko, A., Anderson, R. I. ... Konorski, P. (2021). The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3. Astronomy & Astrophysics, 649.. doi: 10.1051/0004-6361/202140571

Graczyk, D., et al. "The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3." Astronomy & Astrophysics, vol. 649, 2021. https://doi.org/10.1051/0004-6361/202140571

Graczyk, D., G. Pietrzyński, C. Galan, W. Gieren, A. Tkachenko, R. I. Anderson, A. Gallenne, et al. "The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3." Astronomy & Astrophysics 649 (2021). https://doi.org/10.1051/0004-6361/202140571

Graczyk, D., et al. (2021) 'The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3', Astronomy & Astrophysics, 649. doi: 10.1051/0004-6361/202140571

Graczyk D, Pietrzyński G, Galan C, Gieren W, Tkachenko A, Anderson RI, and sur.. The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3. Astronomy & Astrophysics [Internet]. 2021 May 26 [cited 2024 October 01];649. doi: 10.1051/0004-6361/202140571

D. Graczyk, et al., "The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3", Astronomy & Astrophysics, vol. 649, May 2021. [Online]. Available at: https://urn.nsk.hr/urn:nbn:hr:217:769643. [Accessed: 01 October 2024]

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Metadata
Title (english)The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3
AuthorD. Graczyk
AuthorG. Pietrzyński
AuthorC. Galan
AuthorW. Gieren
AuthorA. Tkachenko
AuthorR. I. Anderson
AuthorA. Gallenne
AuthorM. Górski
AuthorG. Hajdu
AuthorM. Kałuszyński
AuthorP. Karczmarek
AuthorP. Kervella
AuthorP. F. L. Maxted
AuthorN. Nardetto
AuthorW. Narloch
AuthorKrešimir Pavlovski
AuthorB. Pilecki
AuthorW. Pych
AuthorJ. Southworth
AuthorJ. Storm
AuthorK. Suchomska
AuthorM. Taormina
AuthorS. Villanova
AuthorP. Wielgórski
AuthorB. Zgirski
AuthorP. Konorski
Author's institutionUniversity of Zagreb
Faculty of Science
(Department of Physics)
Scientific / art field,
discipline and subdiscipline		NATURAL SCIENCES
Physics
Abstract (english)
Aims. The surface brightness–colour relation (SBCR) is a basic tool for establishing precise and accurate distances within the Local Group. Detached eclipsing binary stars with accurately determined radii and trigonometric parallaxes allow calibration of the SBCRs with unprecedented accuracy. Methods. We analysed four nearby eclipsing binary stars containing late F-type main sequence components: AL Ari, AL Dor, FM Leo, and BN Scl. We determined very precise spectroscopic orbits and combined them with high-precision ground- and space-based photometry. We derived the astrophysical parameters of their components with mean errors of 0.1% for mass and 0.4% for radius. We combined those four systems with another 24 nearby eclipsing binaries with accurately known radii from the literature for which Gaia EDR3 parallaxes are available in order to derive the SBCRs. Results. The resulting SBCRs cover stellar spectral types from B9 V to G7 V. For calibrations, we used Johnson optical B and V, Gaia GBP and G, and 2MASS JHK bands. The most precise relations are calibrated using the infrared K band and allow angular diameters of A-, F-, and G-type dwarf and subgiant stars to be predicted with a precision of 1%.
Keywords (english)
Languageenglish
Publication typeScientific paper - Original scientific paper
Publication statusPublished
Peer reviewPeer review - international
Publication versionPublished version
Journal titleAstronomy & Astrophysics
Numberingvol. 649, A109
p-ISSN0004-6361
e-ISSN1432-0746
DOIhttps://doi.org/10.1051/0004-6361/202140571
URN:NBNurn:nbn:hr:217:769643
Publication2021-05-26
Document URLhttps://www.aanda.org/10.1051/0004-6361/202140571
Type of resourceText
Access conditionsOpen access
Terms of useLicence In copyright icon
Public note© ESO 2021. Received 15 February 2021. Accepted 2 March 2021. Published online 26 May 2021.
Created on2024-09-14 19:35:41