The early-type multiple system QZ Carinae

Mayer, P.; Lorenz, R.; Drechsel, H.; Abseim, A.

doi:10.1051/0004-6361:20000228

Cited by 23 publications

(27 citation statements)

References 13 publications

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“…The brightest member of this cluster, QZ Car (HD 9326), is a quadruple system which contains two spectroscopic binaries, one of which shows eclipses of a semi-detached nature (Mayer et al 2001). …”

Section: Collinder 228mentioning

confidence: 99%

Absolute dimensions of eclipsing binaries

Southworth

Clausen

2006

A&A

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Context. The study of detached eclipsing binaries which are members of stellar clusters is is a powerful way of determining the properties of the cluster and of constraining the physical ingredients of theoretical stellar evolutionary models. Aims. DW Carinae is a close but detached early B-type eclipsing binary in the young open cluster Collinder 228. We have measured accurate physical properties of the components of DW Car (masses and radii to 1%, effective temperatures to 0.02 dex) and used these to derive the age, metallicity and distance of Collinder 228. Methods. The rotational velocities of both components of DW Car are high, so we have investigated the performance of doubleGaussian fitting, one-and two-dimensional cross-correlation and spectral disentangling for deriving spectroscopic radial velocites in the presence of strong line blending. Gaussian and cross-correlation analyses require substantial corrections for the effects of line blending, which are only partially successful for cross-correlation. Spectral disentangling is to be preferred because it does not assume anything about the shapes of spectral lines, and is not significantly affected by blending. However, it suffers from a proliferation of local minima in the least-squares fit. We show that the most reliable radial velocities are obtained using spectral disentangling constrained by the results of Gaussian fitting. Complete Strömgren uvby light curves have been obtained and accurate radii have been measured from them by modelling the light curves using the Wilson-Devinney program. This procedure also suffers from the presence of many local minima in parameter space, so we have constrained the solution using an accurate spectroscopic light ratio. The effective temperatures and reddening of the system have been found from Strömgren photometric calibrations. Results. The mass and radius of DW Car A are M A = 11.34 ± 0.12 M and R A = 4.558 ± 0.045 R . The values for DW Car B are M B = 10.63 ± 0.14 M and R B = 4.297 ± 0.055 R . Strömgren photometric calibrations give effective temperatures of T eff A = 27 900 ± 1000 K and T eff B = 26 500 ± 1000 K, and a reddening of E b−y = 0.18 ± 0.02, where the quoted uncertainties include a contribution from the intrinsic uncertainty of the calibrations. The membership of DW Car in Cr 228 allows us to measure the distance, age and chemical composition of the cluster. We have used empirical bolometric corrections to calculate a distance modulus of 12.24 ± 0.12 mag for DW Car, which is in agreement with, and more accurate than, literature values. A comparison between the properties of DW Car and the predictions of recent theoretical evolutionary models is undertaken in the mass-radius and mass-T eff diagrams. The model predictions match the measured properties of DW Car for an age of about 6 Myr and a fractional metal abundance of Z ≈ 0.01.

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Section: Collinder 228mentioning

confidence: 99%

Absolute dimensions of eclipsing binaries

Southworth

Clausen

2006

A&A

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“…One of the most plausible causes of these line changes is the difference of the orbital phase in the compact binaries between both spectra (see, e.g., Figures 1 and 2 in Taylor et al 2011). Variability of the spectral features in the visible part of the spectrum of HD 93206A was also reported by Morrison & Conti (1979) and Mayer et al (2001), associating it with the double tight-binary nature of the source.…”

Section: Discussionmentioning

confidence: 77%

“…The spectroscopic analysis of the system (Leung et al 1979;Morrison & Conti 1980;Stickland & Lloyd 2000;Mayer et al 2001) indicates the existence of two periods of 20.7 and 6 days for components Aa and Ac, respectively. Therefore, from the spectroscopic point of view, HD93206Aa-Ac is a quadruple system that can be subdivided into two short-period binary systems, Aa1, Aa2, and Ac1, Ac2, in a long-period orbit of ∼50years around each other.…”

Section: The Source: Hd 93206amentioning

confidence: 99%

“…Although the primary Ac1 is the brightest component, it seems to be less massive than the secondary Ac2 (possibly O9 V, but its signature on the integrated spectrum is weak), which suggests case-B mass transfer within this binary. The whole system has an estimated total mass of ∼90M e (Leung et al 1979;Morrison & Conti 1980;Mayer et al 2001). X-ray observations of the quadruple Aa-Ac Townsley et al 2011) revealed an excess in X-ray emission (average ∼7×10 −13 erg s…”

Section: The Source: Hd 93206amentioning

confidence: 99%

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GRAVITY Spectro-interferometric Study of the Massive Multiple Stellar System HD 93206 A

Sánchez-Bermúdez

Alberdi

Barbá

et al. 2017

ApJ

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Characterization of the dynamics of massive star systems and the astrophysical properties of the interacting components are a prerequisite for understanding their formation and evolution. Optical interferometry at milliarcsecond resolution is a key observing technique for resolving high-mass multiple compact systems. Here, we report on Very Large Telescope Interferometer/GRAVITY, Magellan/Folded-port InfraRed Echellette, and MPG2.2 m/FEROS observations of the late-O/early-B type system HD93206A, which is a member of the massive cluster Collinder 228 in the Carina nebula complex. With a total mass of about M 90  , it is one of the most compact massive quadruple systems known. In addition to measuring the separation and position angle of the outer binary Aa-Ac, we observe Brγ and He I variability in phase with the orbital motion of the two inner binaries. From the differential phase (D f ) analysis, we conclude that the Brγ emission arises from the interaction regions within the components of the individual binaries, which is consistent with previous models for the X-ray emission of the system based on wind-wind interaction. With an average 3σ deviation of 15 D~ f , we establish an upper limit of p∼0.157 mas (0.35 au) for the size of the Brγ line-emitting region. Future interferometric observations with GRAVITY using the 8 m Unit Telescopes will allow us to constrain the line-emitting regions down to angular sizes of 20 μas (0.05 au at the distance of the Carina nebula).

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“…A notable example is the quadruple system QZ Car (Mayer et al 2001), composed of binaries A (O9.7 I+b2 v, P A = 21 d) and B (O8 III+o9 v, P B = 6 d). It presents several differences with HD 64315: the primaries in the two binaries within QZ Car are evolved stars, and the secondaries are rather less massive.…”

Section: Astrophysical Contextmentioning

confidence: 99%

The massive multiple system HD 64315

Lorenzo

Negueruela

Vilardell

et al. 2017

A&A

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Context. The O6 Vn star HD 64315 is believed to belong to the star-forming region known as NGC 2467, but previous distance estimates do not support this association. Moreover, it has been identified as a spectroscopic binary, but existing data support contradictory values for its orbital period. Aims. We explore the multiple nature of this star with the aim of determining its distance, and understanding its connection to NGC 2467. Methods. A total of 52 high-resolution spectra have been gathered over a decade. We use their analysis, in combination with the photometric data from All Sky Automated Survey and Hipparcos catalogues, to conclude that HD 64315 is composed of at least two spectroscopic binaries, one of which is an eclipsing binary. We have developed our own program to fit four components to the combined line shapes. Once the four radial velocities were derived, we obtained a model to fit the radial-velocity curves using the Spectroscopic Binary Orbit Program (SBOP). We then implemented the radial velocities of the eclipsing binary and the light curves in the Wilson-Devinney code iteratively to derive stellar parameters for its components. We were also able to analyse the non-eclipsing binary, and to derive minimum masses for its components which dominate the system flux. Results. HD 64315 contains two binary systems, one of which is an eclipsing binary. The two binaries are separated by ∼ 0.09 arcsec (or ∼ 500 AU) if the most likely distance to the system, ∼ 5 kpc, is considered. The presence of fainter companions is not excluded by current observations. The non-eclipsing binary (HD 64315 AaAb) has a period of 2.70962901 ± 0.00000021 d. Its components are hotter than those of the eclipsing binary, and dominate the appearance of the system. The eclipsing binary (HD 64315 BaBb) has a shorter period of 1.0189569 ± 0.0000008 d. We derive masses of 14.6 ± 2.3 M ⊙ for both components of the BaBb system. They are almost identical; both stars are overfilling their respective Roche lobes, and share a common envelope in an overcontact configuration. The non-eclipsing binary is a detached system composed of two stars with spectral types around O6 V with minimum masses of 10.8 M ⊙ and 10.2 M ⊙ , and likely masses ≈ 30 M ⊙ . Conclusions. HD 64315 provides a cautionary tale about high-mass star isolation and multiplicity. Its total mass is likely above 90 M ⊙ , but it seems to have formed without an accompanying cluster. It contains one the most massive overcontact binaries known, a likely merger progenitor in a very wide multiple system.

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The early-type multiple system QZ Carinae

Cited by 23 publications

References 13 publications

Absolute dimensions of eclipsing binaries

Absolute dimensions of eclipsing binaries

GRAVITY Spectro-interferometric Study of the Massive Multiple Stellar System HD 93206 A

The massive multiple system HD 64315

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