Asiago eclipsing binaries program IV. SZ Camelopardalis, a<i>β</i> Cephei pulsator in a quadruple, eclipsing system

Tamajo, E.; Munari, U.; Siviero, A.; Tomasella, L.; Dallaporta, S.

doi:10.1051/0004-6361/201117839

Cited by 10 publications

(19 citation statements)

References 75 publications

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“…Based on the equality of the periods and the phase correspondence between the low-amplitude light curve of SZ Cam and the radial velocity curve of the third body, we concluded that the ellipsoidal shape of the components of the third body is responsible for the lowamplitude light variations. We failed to detect the low-amplitude short-period light pulsations found by Tamajo et al (2012) in our data.…”

Section: Discussioncontrasting

confidence: 88%

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Results of a long-term monitoring of the multiple system SZ Cam

Gorda

2015

Astron. Lett.

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We present the results of the reduction of our photometric and spectroscopic observations for the eclipsing binary SZ Cam performed with the telescopes at the Astronomical Observatory of the Ural Federal University and the Special Astrophysical Observatory of the Russian Academy of Sciences in 1996-2014. Based on an 11-year-long photometric monitoring of SZ Cam, we have obtained new elements of its photometric orbit and parameters of its components. We have detected low-amplitude periodic light variations in SZ Cam that are possibly related to the ellipsoidal shape of the components of the spectroscopic binary third body. Based on published data and our new spectroscopy, we have found new values for the mass ratio, q = 0.72 ± 0.01, and parameters of the radial velocity curves of the components, V 0 = −3.6 ± 1.7 km s −1 , K 1 = 190.2 ± 1.9 km s −1 , and K 2 = 263.0 ± 2.4 km s −1 . The component masses have been estimated to be M 1 = 16.1 M and M 2 = 11.6 M . We have obtained new light elements and parameters of the radial velocity curves for the third body, V 3b 0 = 4.2 ± 0.6 km s −1 and K 3b 1 = 26.6 ± 0.8 km s −1 . We have improved the period of the relative orbit of SZ Cam and the third body, P orb = 55.6 ± 1.5 yr.

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Section: Discussioncontrasting

confidence: 88%

“…Quite recently, the results of a study of SZ Cam based on CCD photometry obtained with a small telescope in 2010-2011 have been published (Tamajo et al 2012). The system's parameters found from these new photometric data agree satisfactorily with the quantities from previous papers.…”

Section: Introductionsupporting

confidence: 67%

Results of a long-term monitoring of the multiple system SZ Cam

Gorda

2015

Astron. Lett.

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“…10. HD 23642: Groenewegen et al (2007); HD 24133: Clausen et al (2010); HD 24909: Degirmenci (1997); HD 25638: Tamajo et al (2012); HD 25833: Giménez & Clausen (1994); HD 32964: Makaganiuk et al (2011);HD 34364: Nordstrom & Johansen (1994); HD 36486: Shenar et al (2015); HD 150136: Mahy et al (2012). Table 3: Predictions of tidal scenario for (non-magnetic) close binaries described in Table 2.…”

Section: Magnetic Binariesmentioning

confidence: 99%

Fossil field decay due to nonlinear tides in massive binaries

Vidal

Cébron

ud‐Doula

et al. 2019

A&A

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Context. Surface magnetic fields have been detected in 5 to 10% of isolated massive stars, hosting outer radiative envelopes. They are often thought to have a fossil origin, resulting from the stellar formation phase. Yet, magnetic massive stars are scarcer in (close) short-period binaries, as reported by the BinaMIcS (Binarity and Magnetic Interaction in various classes of Stars) collaboration. Aims. Different physical conditions in the molecular clouds giving birth to isolated stars and binaries are commonly invoked. In addition, we propose that the observed lower magnetic incidence in close binaries may be due to nonlinear tides. Indeed, close binaries are probably prone to tidal instability, a fluid instability growing upon the equilibrium tidal flow via nonlinear effects. Yet, stratified effects have hitherto been largely overlooked. Methods. We theoretically and numerically investigate tidal instability in rapidly rotating, stably stratified fluids permeated by magnetic fields. We use the short-wavelength stability method to propose a comprehensive (local) theory of tidal instability at the linear onset, discussing damping effects. Then, we propose a mixing-length theory for the mixing generated by tidal instability in the nonlinear regime. We successfully assess our theoretical predictions against proofof-concept, direct numerical simulations. Finally, we compare our predictions with the observations of short-period, double-lined spectroscopic binary systems. Results. Using new analytical results, cross-validated by a direct integration of the stability equations, we show that tidal instability can be generated by nonlinear couplings of inertia-gravity waves with the equilibrium tidal flow in short-period massive binaries, even against the Joule diffusion. In the nonlinear regime, a fossil magnetic field can be dissipated by the turbulent magnetic diffusion induced by the saturated tidal flows. Conclusions. We predict that the turbulent Joule diffusion of fossil fields would occur in a few million years for several short-period massive binaries. Therefore, turbulent tidal flows could explain the observed dearth of some short-period magnetic binaries.

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“…With a median distance of 1 528 pc, O-type binaries are the most distant objects. Closest one is SZ Cam which is 870 pc away (Tamajo et al 2012), the most distant one is DH Cep with 2 767 pc (Hilditch, Harries, & Bell 1996). There exist 10 binaries with O-type primary in the present sample.…”

Section: Space Distributionsmentioning

confidence: 99%

The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way

Eker

Bilir

Soydugan

et al. 2014

Publ. Astron. Soc. Aust.

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The most accurate stellar astrophysical parameters were collected from the solutions of the light and the radial velocity curves of 257 detached double-lined eclipsing binaries in the Milky Way. The catalogue contains masses, radii, surface gravities, effective temperatures, luminosities, projected rotational velocities of the component stars, and the orbital parameters. The number of stars with accurate parameters increased 67% in comparison to the most recent similar collection by Torres, Andersen, & Giménez (2010). Distributions of some basic parameters were investigated. The ranges of effective temperatures, masses, and radii are 2 750 < T eff (K)< 43 000, 0.18 < M/M < 33, and 0.2 < R/R < 21.2, respectively. Being mostly located in one kpc in the Solar neighborhood, the present sample covers distances up to 4.6 kpc within the two local Galactic arms, Carina-Sagittarius and Orion Spur. The number of stars with both mass and radius measurements better than 1% uncertainty is 93, better than 3% uncertainty is 311, and better than 5% uncertainty is 388. It is estimated from the Roche lobe filling factors that 455 stars (88.5% of the sample) are spherical within 1% of uncertainty.

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Asiago eclipsing binaries program IV. SZ Camelopardalis, aβ Cephei pulsator in a quadruple, eclipsing system

Cited by 10 publications

References 75 publications

Results of a long-term monitoring of the multiple system SZ Cam

Results of a long-term monitoring of the multiple system SZ Cam

Fossil field decay due to nonlinear tides in massive binaries

The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way

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