Properties and nature of Be stars 31. The binary nature, light
variability, physical elements, and emission-line changes of HD
81357

J 2019

Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357

KOUBSKY, P., P. HARMANEC, M. BROZ, L. KOTKOVA, S. YANG et. al.

Základní údaje

Originální název

Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357

Autoři

KOUBSKY, P. (garant), P. HARMANEC, M. BROZ, L. KOTKOVA, S. YANG, H. BOZIC, D. SUDAR, Y. FREMAT, D. KORCAKOVA, Viktor VOTRUBA (203 Česká republika, domácí), P. SKODA, M. SLECHTA a D. RUZDJAK

Vydání

ASTRONOMY & ASTROPHYSICS, LES ULIS CEDEX A, EDP SCIENCES S A, 2019, 1432-0746

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 5.636

Kód RIV

RIV/00216224:14310/19:00113465

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1051/0004-6361/201834597

UT WoS

000485215200002

Klíčová slova anglicky

binaries: close; binaries: spectroscopic; stars: emission-line Be; stars: fundamental parameters; stars: individual: HD 81357

Štítky

rivok

Změněno: 11. 5. 2020 10:37, Mgr. Marie Šípková, DiS.

Anotace

V originále

Reliable determination of the basic physical properties of hot emission-line binaries with Roche-lobe filling secondaries is important for developing the theory of mass exchange in binaries. It is not easy, however, due to the presence of circumstellar matter. Here, we report the first detailed investigation of a new representative of this class of binaries, HD 81357, based on the analysis of spectra and photometry from several observatories. HD 81357 was found to be a double-lined spectroscopic binary and an ellipsoidal variable seen under an intermediate orbital inclination of similar to(63 +/- 5)degrees, having an orbital period of 33.(d)77445(41) and a circular orbit. From an automated comparison of the observed and synthetic spectra, we estimate the component's effective temperatures to be 12930(540) K and 4260(24) K. The combined light-curve and orbital solutions, also constrained by a very accurate Gaia Data Release 2 parallax, give the following values of the basic physical properties: masses 3.36 +/- 0.15 and 0.34 +/- 0.04 M-circle dot(N), radii 3.9 +/- 0.2 and 13.97 +/- 0.05 R-circle dot(N), and a mass ratio 10.0 +/- 0.5. Evolutionary modelling of the system including the phase of mass transfer between the components indicated that HD 81357 is a system observed in the final slow phase of the mass exchange after the mass-ratio reversal. Contrary to what has been seen for similar binaries like AU Mon, no cyclic light variations were found on a time scale an order of magnitude longer than the orbital period.

Citovat

KOUBSKY, P., P. HARMANEC, M. BROZ, L. KOTKOVA, S. YANG, H. BOZIC, D. SUDAR, Y. FREMAT, D. KORCAKOVA, Viktor VOTRUBA, P. SKODA, M. SLECHTA a D. RUZDJAK. Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357. ASTRONOMY & ASTROPHYSICS. LES ULIS CEDEX A: EDP SCIENCES S A, 2019, roč. 629, SEP 12 2019, s. 1-14. ISSN 1432-0746. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201834597.

@article{1641697,
   author = {Koubsky, P. and Harmanec, P. and Broz, M. and Kotkova, L. and Yang, S. and Bozic, H. and Sudar, D. and Fremat, Y. and Korcakova, D. and Votruba, Viktor and Skoda, P. and Slechta, M. and Ruzdjak, D.},
   article_location = {LES ULIS CEDEX A},
   article_number = {SEP 12 2019},
   doi = {http://dx.doi.org/10.1051/0004-6361/201834597},
   keywords = {binaries: close; binaries: spectroscopic; stars: emission-line Be; stars: fundamental parameters; stars: individual: HD 81357},
   language = {eng},
   issn = {1432-0746},
   journal = {ASTRONOMY & ASTROPHYSICS},
   title = {Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357},
   url = {https://arxiv.org/pdf/1908.02719.pdf},
   volume = {629},
   year = {2019}
}

TY  - JOUR
ID  - 1641697
AU  - Koubsky, P. - Harmanec, P. - Broz, M. - Kotkova, L. - Yang, S. - Bozic, H. - Sudar, D. - Fremat, Y. - Korcakova, D. - Votruba, Viktor - Skoda, P. - Slechta, M. - Ruzdjak, D.
PY  - 2019
TI  - Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357
JF  - ASTRONOMY & ASTROPHYSICS
VL  - 629
IS  - SEP 12 2019
SP  - 1-14
EP  - 1-14
PB  - EDP SCIENCES S A
SN  - 14320746
KW  - binaries: close
KW  - binaries: spectroscopic
KW  - stars: emission-line Be
KW  - stars: fundamental parameters
KW  - stars: individual: HD 81357
UR  - https://arxiv.org/pdf/1908.02719.pdf
L2  - https://arxiv.org/pdf/1908.02719.pdf
N2  - Reliable determination of the basic physical properties of hot emission-line binaries with Roche-lobe filling secondaries is important for developing the theory of mass exchange in binaries. It is not easy, however, due to the presence of circumstellar matter. Here, we report the first detailed investigation of a new representative of this class of binaries, HD 81357, based on the analysis of spectra and photometry from several observatories. HD 81357 was found to be a double-lined spectroscopic binary and an ellipsoidal variable seen under an intermediate orbital inclination of similar to(63 +/- 5)degrees, having an orbital period of 33.(d)77445(41) and a circular orbit. From an automated comparison of the observed and synthetic spectra, we estimate the component's effective temperatures to be 12930(540) K and 4260(24) K. The combined light-curve and orbital solutions, also constrained by a very accurate Gaia Data Release 2 parallax, give the following values of the basic physical properties: masses 3.36 +/- 0.15 and 0.34 +/- 0.04 M-circle dot(N), radii 3.9 +/- 0.2 and 13.97 +/- 0.05 R-circle dot(N), and a mass ratio 10.0 +/- 0.5. Evolutionary modelling of the system including the phase of mass transfer between the components indicated that HD 81357 is a system observed in the final slow phase of the mass exchange after the mass-ratio reversal. Contrary to what has been seen for similar binaries like AU Mon, no cyclic light variations were found on a time scale an order of magnitude longer than the orbital period.
ER  -

KOUBSKY, P., P. HARMANEC, M. BROZ, L. KOTKOVA, S. YANG, H. BOZIC, D. SUDAR, Y. FREMAT, D. KORCAKOVA, Viktor VOTRUBA, P. SKODA, M. SLECHTA a D. RUZDJAK. Properties and nature of Be stars 31. The binary nature, light variability, physical elements, and emission-line changes of HD 81357. \textit{ASTRONOMY \&{}amp; ASTROPHYSICS}. LES ULIS CEDEX A: EDP SCIENCES S A, 2019, roč.~629, SEP 12 2019, s.~1-14. ISSN~1432-0746. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201834597.

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