The 2003–2004 multisite photometric campaign for the β Cephei and eclipsing star 16 (EN) Lacertae with an appendix on 2 Andromedae, the variable comparison star

Jerzykiewicz, M.; Handler, G.; Daszyńska‐Daszkiewicz, J.; Pigulski, A.; Poretti, E.; Rodríguez‐López, C.; Amado, P. J.; Kołaczkowski, Z.; Uytterhoeven, K.; Dorokhova, T. N.; Dorokhov, N. I.; Lorenz, D.; Zsuffa, D.; Kim, S.-L.; Bourge, P.-O.; Acke, B.; Verhoelst, Tijl; Drummond, R.; Movchan, Alexander; Lee, J.-A.; Stȩślicki, M.; Molenda-Żakowicz, J.; Garrido, R.; Kim, S.-H.; Michalska, G.; Paparó, M.; Antoci, V.; Aerts, C.

doi:10.1093/mnras/stv1958

Cited by 10 publications

(7 citation statements)

References 56 publications

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“…The B2 IV primary of the former is also a well-known Cephei variable, while the B5 IV primary of the latter is an SPB star. The pre-MS nature of the secondary of 16 (EN) Lac was suggested by Pigulski & Jerzykiewicz (1988) and confirmed by Jerzykiewicz et al (2015), while that of Eri is established in Section 6 of the present paper.…”

Section: Introductionsupporting

confidence: 73%

BRITE observations of $ν$ Centauri and $γ$ Lupi, the first non-eclipsing members of the new class of nascent binaries

Jerzykiewicz,

Pigulski,

Michalska

et al. 2021

Preprint

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Results of an analysis of the BRITE-Constellation and SMEI photometry and radial-velocity observations, archival and new, of two single-lined spectroscopic binary systems Centauri and Lupi are reported. In the case of Lup AB, a visual binary, an examination of the light-time effect shows that component A is the spectroscopic binary. Both Cen and Lup exhibit light variations with the orbital period. The variations are caused by the reflection effect, i.e. heating of the secondary's hemisphere by the early-B main sequence (MS) primary component's light. The modelling of the light curves augmented with the fundamental parameters of the primary components obtained from the literature photometric data and Hipparcos parallaxes, shows that the secondary components are pre-MS stars, in the process of contracting onto the MS. Cen and Lup A are thus found to be non-eclipsing counterparts of the B2 IV eclipsing binary (and a Cephei variable) 16 (EN) Lac, the B5 IV eclipsing binary (and an SPB variable) Eri, and the recently discovered LMC nascent eclipsing binaries.

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Section: Introductionsupporting

confidence: 73%

BRITE observations of $ν$ Centauri and $γ$ Lupi, the first non-eclipsing members of the new class of nascent binaries

Jerzykiewicz,

Pigulski,

Michalska

et al. 2021

Preprint

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“…However, no precise mass measurement currently exists for a β Cep pulsator. A few have been found in binary systems, for example EN Lac (Jerzykiewicz et al 2015), V381 Car (Freyhammer et al 2005) and α Vir (Tkachenko et al 2016), but in each case the mass is not precisely known because either the secondary star is not detectable in spectra or the orbital inclination is poorly determined due to the lack of eclipses.…”

Section: Introductionmentioning

confidence: 99%

Discovery of β Cep pulsations in the eclipsing binary V453 Cygni

Southworth

Bowman

Tkachenko

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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V453 Cyg is an eclipsing binary containing 14 and 11 $\, {\rm M}_\odot$ stars in an eccentric short-period orbit. We have discovered β Cep-type pulsations in this system using Transiting Exoplanet Survey Satellite data. We identify seven significant pulsation frequencies, between 2.37 and 10.51 d−1, in the primary star. These include six frequencies that are separated by yet significantly offset from harmonics of the orbital frequency, indicating they are tidally perturbed modes. We have determined the physical properties of the system to high precision: V453 Cyg A is the first β Cep pulsator with a precise mass measurement. The system is a vital tracer of the physical processes that govern the evolution of massive single and binary stars.

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“…In a review on intrinsic variability among binary and multiple systems, Pigulski [24] mentioned four β Cep pulsating stars in EB systems known at the time: 16 Lac, V381 Car, η Ori, and λ Sco. 16 Lac is a well detached system with a near-circular orbit of period 12.0968 d [25]. V381 Car is a detached system with an an almost circular orbit of period 8.32457 d, probably without apsidal motion [26].…”

Section: Ebs With Main-sequence (Or Slightly Evolved) B-type Pulsatorsmentioning

confidence: 99%

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Lampens

2021

Galaxies

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Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) mass transfer between the components and/or magnetic activity. How these phenomena and the orbital changes affect the different types of pulsations excited in one or more components, offers a new window of opportunity to better understand the physics of pulsations.

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The 2003–2004 multisite photometric campaign for the β Cephei and eclipsing star 16 (EN) Lacertae with an appendix on 2 Andromedae, the variable comparison star

Cited by 10 publications

References 56 publications

BRITE observations of $ν$ Centauri and $γ$ Lupi, the first non-eclipsing members of the new class of nascent binaries

BRITE observations of $ν$ Centauri and $γ$ Lupi, the first non-eclipsing members of the new class of nascent binaries

Discovery of β Cep pulsations in the eclipsing binary V453 Cygni

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

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