Podrobný výpis o publikaci

ZASCHE, P., Z. HENZL, M. MASEK, R. UHLAR, J. KARA, J. MERC a Hana KUČÁKOVÁ. Detection of seven 2+2 doubly eclipsing quadruple systems. ASTRONOMY & ASTROPHYSICS. LES ULIS CEDEX A: EDP SCIENCES S A, 2023, roč. 675, Jul 2023, s. "A113-1"-"A113-10", 10 s. ISSN 0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/202346848.

Další formáty: BibTeX LaTeX RIS

TY  - JOUR
ID  - 77189
AU  - Zasche, P. - Henzl, Z. - Masek, M. - Uhlar, R. - Kara, J. - Merc, J. - Kučáková, Hana
PY  - 2023
TI  - Detection of seven 2+2 doubly eclipsing quadruple systems
JF  - ASTRONOMY & ASTROPHYSICS
VL  - 675
IS  - Jul 2023
SP  - "A113-1"-"A113-10"
EP  - "A113-1"-"A113-10"
PB  - EDP SCIENCES S A
SN  - 00046361
KW  - binaries;eclipsing;stars;fundamental parameters
UR  - https://www.aanda.org/articles/aa/full_html/2023/07/aa46848-23/aa46848-23.html
N2  - In this work, we study a heterogeneous group of seven stellar systems for the first time. Despite their different distances or spectral types, all of them belong to a very rare group of quadruple systems of 2+2 architecture, where both of the inner pairs harbor eclipsing binaries. These systems are: ASASSN-V J102911.57-522413.6 (inner periods 0.57272, and 3.79027 days), V1037 Her (0.78758 and 5.80348 days), WISE J181904.2+241243 (0.36713 and 0.41942 days), V2894 Cyg (2.57434 and 1.30579 days), NSVS 5725040 (1.79368 and 0.76794 days), WISE J210230.8+610816 (1.84324 and 0.57159 days), and ZTF J220518.78+592642.1 (2.79572 and 3.34615 days). Their outer mutual periods are: 9.3, 25.4, 18.7, 27.5, 2.6, 2.2, and 14.0 yr, respectively. These outer periodicities were derived using longer time span of photometric observations of these systems and analysing their period changes of both inner pairs via ETVs (eclipse-timing variations). Most of these studied systems are detached, as evidenced by the proper modelling of their light curves. A few of them show significant eccentric orbits with apsidal motion (e.g., V2894 Cyg, and NSVS 5725040). Further spectroscopic follow-up observations would offer a better characterization of the component star's parameters (for e.g., NSVS 5725040), as well as a potential interferometric detection of the systems as real doubles on their mutual orbits (for e.g., V1037 Her). A rather interesting excess of systems close to a 3:2 mean motion resonance is seen only for early spectral-type stars with higher temperatures.
ER  -

Základní údaje
Originální název	Detection of seven 2+2 doubly eclipsing quadruple systems
Autoři	ZASCHE, P., Z. HENZL, M. MASEK, R. UHLAR, J. KARA, J. MERC a Hana KUČÁKOVÁ (203 Česká republika, domácí).
Vydání	ASTRONOMY & ASTROPHYSICS, LES ULIS CEDEX A, EDP SCIENCES S A, 2023, 0004-6361.

Další údaje
Originální jazyk	angličtina
Typ výsledku	Článek v odborném periodiku
Obor	10308 Astronomy
Stát vydavatele	Francie
Utajení	není předmětem státního či obchodního tajemství
WWW	URL
Kód RIV	RIV/47813059:19630/23:A0000316
Organizační jednotka	Fyzikální ústav v Opavě
Doi	http://dx.doi.org/10.1051/0004-6361/202346848
UT WoS	001025495200001
Klíčová slova anglicky	binaries;eclipsing;stars;fundamental parameters
Štítky	RIV24, UF
Příznaky	Mezinárodní význam, Recenzováno
Změnil	Změnila: Mgr. Pavlína Jalůvková, učo 25213. Změněno: 31. 1. 2024 10:29.

Anotace
In this work, we study a heterogeneous group of seven stellar systems for the first time. Despite their different distances or spectral types, all of them belong to a very rare group of quadruple systems of 2+2 architecture, where both of the inner pairs harbor eclipsing binaries. These systems are: ASASSN-V J102911.57-522413.6 (inner periods 0.57272, and 3.79027 days), V1037 Her (0.78758 and 5.80348 days), WISE J181904.2+241243 (0.36713 and 0.41942 days), V2894 Cyg (2.57434 and 1.30579 days), NSVS 5725040 (1.79368 and 0.76794 days), WISE J210230.8+610816 (1.84324 and 0.57159 days), and ZTF J220518.78+592642.1 (2.79572 and 3.34615 days). Their outer mutual periods are: 9.3, 25.4, 18.7, 27.5, 2.6, 2.2, and 14.0 yr, respectively. These outer periodicities were derived using longer time span of photometric observations of these systems and analysing their period changes of both inner pairs via ETVs (eclipse-timing variations). Most of these studied systems are detached, as evidenced by the proper modelling of their light curves. A few of them show significant eccentric orbits with apsidal motion (e.g., V2894 Cyg, and NSVS 5725040). Further spectroscopic follow-up observations would offer a better characterization of the component star's parameters (for e.g., NSVS 5725040), as well as a potential interferometric detection of the systems as real doubles on their mutual orbits (for e.g., V1037 Her). A rather interesting excess of systems close to a 3:2 mean motion resonance is seen only for early spectral-type stars with higher temperatures.

Anotace

In this work, we study a heterogeneous group of seven stellar systems for the first time. Despite their different distances or spectral types, all of them belong to a very rare group of quadruple systems of 2+2 architecture, where both of the inner pairs harbor eclipsing binaries. These systems are: ASASSN-V J102911.57-522413.6 (inner periods 0.57272, and 3.79027 days), V1037 Her (0.78758 and 5.80348 days), WISE J181904.2+241243 (0.36713 and 0.41942 days), V2894 Cyg (2.57434 and 1.30579 days), NSVS 5725040 (1.79368 and 0.76794 days), WISE J210230.8+610816 (1.84324 and 0.57159 days), and ZTF J220518.78+592642.1 (2.79572 and 3.34615 days). Their outer mutual periods are: 9.3, 25.4, 18.7, 27.5, 2.6, 2.2, and 14.0 yr, respectively. These outer periodicities were derived using longer time span of photometric observations of these systems and analysing their period changes of both inner pairs via ETVs (eclipse-timing variations). Most of these studied systems are detached, as evidenced by the proper modelling of their light curves. A few of them show significant eccentric orbits with apsidal motion (e.g., V2894 Cyg, and NSVS 5725040). Further spectroscopic follow-up observations would offer a better characterization of the component star's parameters (for e.g., NSVS 5725040), as well as a potential interferometric detection of the systems as real doubles on their mutual orbits (for e.g., V1037 Her). A rather interesting excess of systems close to a 3:2 mean motion resonance is seen only for early spectral-type stars with higher temperatures.