J/A+A/667/A53 Photometry of the double eclipsing binary CzeV343 (Pejcha+, 2022)
The complex dynamical past and future of double eclipsing binary CzeV343:
Misaligned orbits and period resonance.
Pejcha O., Cagas P., Landri C., Fausnaugh M.M., De Rosa G., Prieto J.L.,
Henzl Z., Pesta M.
<Astron. Astrophys. 667, A53 (2022)>
=2022A&A...667A..53P 2022A&A...667A..53P (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Photometry
Keywords: binaries: close - binaries: eclipsing - stars: evolution -
stars: individual: CzeV343
Abstract:
CzeV343 (=V849 Aur) was previously identified as a candidate double
eclipsing binary (2+2 quadruple), where the orbital periods of the two
eclipsing binaries (PA∼1.2-days and PB∼0.8-days) lie very close to
3:2 resonance. Here, we analyze 11 years of ground-based photometry, 4
sectors of TESS 2-minute and full-frame photometry, and two optical
spectra. We construct a global model of our photometry, including
apsidal motion of binary A and 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+1.3M☉) and binary B (1.4+1.2M☉). We identify
pseudo-synchronous rotation signal of binary A in TESS photometry. We
detect apsidal motion in binary A with a period of about 33 years,
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 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 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 so far explored in 2+2 quadruples.
Description:
Ground-based photometry of CzeV343. Our dataset includes the
measurements already published by Cagas & Pejcha (2012A&A...544L...3C 2012A&A...544L...3C,
Cat. J/A+A/544/L3), but the data differ in detail due to changes in
image processing and we thus reproduce them here.
Objects:
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RA (2000) DE Designation(s)
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05 48 24.008 +30 57 03.64 CzeV343 = GSC 02405-01886
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 25 12257 Ground-based photometry of CzeV343
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See also:
J/A+A/544/L3 : Photometry of the double eclipsing binary CzeV343 (Cagas+, 2012)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 11 F11.6 d HJD Heliocentric Julian Date (HJD-2450000)
13- 18 F6.4 mag dmag Differential magnitude
20- 25 F6.4 mag e_dmag Magnitude uncertainty
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Acknowledgements:
Ondrej Pejcha, pejcha(at)utf.mff.cuni.cz
(End) Patricia Vannier [CDS] 16-Aug-2022