The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10456319" target="_blank" >RIV/00216208:11320/22:10456319 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mkBOsjgerh" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mkBOsjgerh</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202244335" target="_blank" >10.1051/0004-6361/202244335</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Popis výsledku v původním jazyce

CzeV343 (=V849 Aur) was previously identified as a candidate double eclipsing binary (2+2 quadruple), where the orbital periods of the two eclipsing binaries (P-A approximate to 1.2 days and P-B approximate to 0.8 days) lie very close to a 3:2 resonance. Here, we analyze 11 yr of groundbased photometry, four sectors of Transiting Exoplanet Survey Satellite (TESS) 2-min and full-frame photometry, and two optical spectra. We construct a global model of our photometry, including apsidal motion of binary A and the light-travel time effect (LTTE) of the mutual outer orbit, and explore the parameter space with Markov chain Monte Carlo. We estimate component masses for binary A (1.8 + 1.3 M-circle dot) and binary B (1.4 + 1.2 M-circle dot). We identify the pseudo-synchronous rotation signal of binary A in TESS photometry. We detect apsidal motion in binary A with a period of about 33 yr, which is fully explained by tidal and rotational contributions of stars aligned with the orbit. The mutual orbit has a period of about 1450 days and an eccentricity of about 0.7. The LTTE amplitude is small, which points to low inclination of the outer orbit and a high degree of misalignment with the inner orbits. We find that when apsidal motion and the mutual orbit are taken into account, the orbital period resonance is exact to within 10-5 cycles/day. Many properties of CzeV343 are not compatible with requirements of the 3:2 resonance capture theory for coplanar orbits. Future evolution of CzeV343 can lead to mergers, triple common envelope, double white dwarf binaries, or a Type Ia supernova. More complex evolutionary pathways will likely arise from dynamical instability caused by orbital expansion when either of the binaries undergoes mass transfer. This instability has not been explored so far in 2+2 quadruples.

Název v anglickém jazyce

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Popis výsledku anglicky

CzeV343 (=V849 Aur) was previously identified as a candidate double eclipsing binary (2+2 quadruple), where the orbital periods of the two eclipsing binaries (P-A approximate to 1.2 days and P-B approximate to 0.8 days) lie very close to a 3:2 resonance. Here, we analyze 11 yr of groundbased photometry, four sectors of Transiting Exoplanet Survey Satellite (TESS) 2-min and full-frame photometry, and two optical spectra. We construct a global model of our photometry, including apsidal motion of binary A and the light-travel time effect (LTTE) of the mutual outer orbit, and explore the parameter space with Markov chain Monte Carlo. We estimate component masses for binary A (1.8 + 1.3 M-circle dot) and binary B (1.4 + 1.2 M-circle dot). We identify the pseudo-synchronous rotation signal of binary A in TESS photometry. We detect apsidal motion in binary A with a period of about 33 yr, which is fully explained by tidal and rotational contributions of stars aligned with the orbit. The mutual orbit has a period of about 1450 days and an eccentricity of about 0.7. The LTTE amplitude is small, which points to low inclination of the outer orbit and a high degree of misalignment with the inner orbits. We find that when apsidal motion and the mutual orbit are taken into account, the orbital period resonance is exact to within 10-5 cycles/day. Many properties of CzeV343 are not compatible with requirements of the 3:2 resonance capture theory for coplanar orbits. Future evolution of CzeV343 can lead to mergers, triple common envelope, double white dwarf binaries, or a Type Ia supernova. More complex evolutionary pathways will likely arise from dynamical instability caused by orbital expansion when either of the binaries undergoes mass transfer. This instability has not been explored so far in 2+2 quadruples.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/LTAUSA18093" target="_blank" >LTAUSA18093: Časová proměnnost v astronomii: účast v projektu All-Sky Automated Survey for Supernovae</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

667

Číslo periodika v rámci svazku

Nov

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

29

Strana od-do

A53

Kód UT WoS článku

000878844600007

EID výsledku v databázi Scopus

2-s2.0-85145262537