Podrobný výpis o publikaci

VAŇKO, Martin, Theodor PRIBULLA, Pavol GAJDOŠ, Ján BUDAJ, Juraj ZVERKO, Ernst PAUNZEN, Zoltán GARAI, Lubomír HAMBÁLEK, Richard KOMŽÍK a Emil KUNDRA. HD 183986: A High-contrast SB2 System with a Pulsating Component. Astronomical Journal. IOP Publishing, 2022, roč. 163, č. 6, s. 1-14. ISSN 0004-6256. Dostupné z: https://dx.doi.org/10.3847/1538-3881/ac617b.

Další formáty: BibTeX LaTeX RIS

TY  - JOUR
ID  - 1854637
AU  - Vaňko, Martin - Pribulla, Theodor - Gajdoš, Pavol - Budaj, Ján - Zverko, Juraj - Paunzen, Ernst - Garai, Zoltán - Hambálek, Lubomír - Komžík, Richard - Kundra, Emil
PY  - 2022
TI  - HD 183986: A High-contrast SB2 System with a Pulsating Component
JF  - Astronomical Journal
VL  - 163
IS  - 6
SP  - 1-14
EP  - 1-14
PB  - IOP Publishing
SN  - 00046256
KW  - Radial velocity
KW  - Binary stars
KW  - Pulsating variable stars
UR  - https://iopscience.iop.org/article/10.3847/1538-3881/ac617b
N2  - There is a small group of peculiar early-type stars on the main sequence that show different rotation velocities from different spectral lines. This inconsistency might be due to the binary nature of these objects. We aim to verify this hypothesis by a more detailed spectroscopic and photometric investigation of one such object: HD 183986. We obtained 151 high- and medium-resolution spectra that covered an anticipated long orbital period. There is clear evidence of the orbital motion of the primary component. We uncovered a very faint and broad spectrum of the secondary component. The corresponding SB2 orbital parameters, and the component spectra, were obtained by Fourier disentangling using the KOREL code. The component spectra were further modeled by iSpec code to arrive at the atmospheric quantities and the projected rotational velocities. We have proven that this object is a binary star with a period P = 1268.2(11) days, eccentricity e = 0.5728(20), and mass ratio q = 0.655. The primary component is a slowly rotating star ($v\sin i=27$ km s−1) while the cooler and less massive secondary rotates much faster ($v\sin i\,\sim $120 km s−1). Photometric observations obtained by the Transiting Exoplanet Survey Satellite (TESS) satellite were also investigated to shed more light on this object. A multiperiod photometric variability was detected in the TESS data ranging from hours (the δ Sct-type variability) to a few days (spots/rotational variability). The physical parameters of the components and the origin of the photometric variability are discussed in more detail.
ER  -

Základní údaje
Originální název	HD 183986: A High-contrast SB2 System with a Pulsating Component
Autoři	VAŇKO, Martin (garant), Theodor PRIBULLA, Pavol GAJDOŠ, Ján BUDAJ, Juraj ZVERKO, Ernst PAUNZEN (40 Rakousko, domácí), Zoltán GARAI, Lubomír HAMBÁLEK, Richard KOMŽÍK a Emil KUNDRA.
Vydání	Astronomical Journal, IOP Publishing, 2022, 0004-6256.

Další údaje
Originální jazyk	angličtina
Typ výsledku	Článek v odborném periodiku
Obor	10308 Astronomy
Stát vydavatele	Velká Británie a Severní Irsko
Utajení	není předmětem státního či obchodního tajemství
WWW	URL
Impakt faktor	Impact factor: 5.300
Kód RIV	RIV/00216224:14310/22:00125855
Organizační jednotka	Přírodovědecká fakulta
Doi	http://dx.doi.org/10.3847/1538-3881/ac617b
UT WoS	000790528900001
Klíčová slova anglicky	Radial velocity; Binary stars; Pulsating variable stars
Štítky	rivok
Příznaky	Mezinárodní význam, Recenzováno
Změnil	Změnila: Mgr. Marie Šípková, DiS., učo 437722. Změněno: 9. 1. 2023 10:29.

Anotace
There is a small group of peculiar early-type stars on the main sequence that show different rotation velocities from different spectral lines. This inconsistency might be due to the binary nature of these objects. We aim to verify this hypothesis by a more detailed spectroscopic and photometric investigation of one such object: HD 183986. We obtained 151 high- and medium-resolution spectra that covered an anticipated long orbital period. There is clear evidence of the orbital motion of the primary component. We uncovered a very faint and broad spectrum of the secondary component. The corresponding SB2 orbital parameters, and the component spectra, were obtained by Fourier disentangling using the KOREL code. The component spectra were further modeled by iSpec code to arrive at the atmospheric quantities and the projected rotational velocities. We have proven that this object is a binary star with a period P = 1268.2(11) days, eccentricity e = 0.5728(20), and mass ratio q = 0.655. The primary component is a slowly rotating star ($v\sin i=27$ km s−1) while the cooler and less massive secondary rotates much faster ($v\sin i\,\sim $120 km s−1). Photometric observations obtained by the Transiting Exoplanet Survey Satellite (TESS) satellite were also investigated to shed more light on this object. A multiperiod photometric variability was detected in the TESS data ranging from hours (the δ Sct-type variability) to a few days (spots/rotational variability). The physical parameters of the components and the origin of the photometric variability are discussed in more detail.

Anotace

There is a small group of peculiar early-type stars on the main sequence that show different rotation velocities from different spectral lines. This inconsistency might be due to the binary nature of these objects. We aim to verify this hypothesis by a more detailed spectroscopic and photometric investigation of one such object: HD 183986. We obtained 151 high- and medium-resolution spectra that covered an anticipated long orbital period. There is clear evidence of the orbital motion of the primary component. We uncovered a very faint and broad spectrum of the secondary component. The corresponding SB2 orbital parameters, and the component spectra, were obtained by Fourier disentangling using the KOREL code. The component spectra were further modeled by iSpec code to arrive at the atmospheric quantities and the projected rotational velocities. We have proven that this object is a binary star with a period P = 1268.2(11) days, eccentricity e = 0.5728(20), and mass ratio q = 0.655. The primary component is a slowly rotating star ($v\sin i=27$ km s−1) while the cooler and less massive secondary rotates much faster ($v\sin i\,\sim $120 km s−1). Photometric observations obtained by the Transiting Exoplanet Survey Satellite (TESS) satellite were also investigated to shed more light on this object. A multiperiod photometric variability was detected in the TESS data ranging from hours (the δ Sct-type variability) to a few days (spots/rotational variability). The physical parameters of the components and the origin of the photometric variability are discussed in more detail.

Návaznosti
98507, interní kód MU	Název: European Collaborating Astronomer ProjectS: Espana-Czechia-Slovakia (Akronym: ECAPS:E-C-S)
98507, interní kód MU	Investor: Evropská unie, European Collaborating Astronomer ProjectS: Espana-Czechia-Slovakia, Strategická partnerství v oblasti vzdělávání, odborné přípravy a mládeže