Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

Балега, И. И.; Balega, Yu. Yu.; Максимов, А. Ф.; Малоголовец, Е. В.; Растегаев, Д. А.; Shkhagosheva, Z. U.; Weigelt, G.

doi:10.1134/s1990341307040050

Cited by 62 publications

(46 citation statements)

References 23 publications

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“…The presence of the third component has been confirmed by speckle interferometry (Mason et al 1998). More speckle measurements were published by Gorda et al (2007) and Balega et al (2007). These speckle measurements detected an orbital motion for the tertiary component but one that is extended long enough in time to cover only a small arc of the overall orbit.…”

Section: Introductionmentioning

confidence: 91%

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

Tamajo

Munari

Siviero

et al. 2012

A&A

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We present a spectroscopic and photometric analysis of the multiple system and early-type eclipsing binary SZ Cam (O9 IV + B0.5 V), which consists of an eclipsing SB2 pair of orbital period P = 2.7 days in a long orbit (∼55 yrs) around a non-eclipsing SB1 pair of orbital period P = 2.8 days. We have reconstructed the spectra of the individual components of SZ Cam from the observed composite spectra using the technique of spectral disentangling. We used them together with extensive and accurate BV I C CCD photometry to obtain an orbital solution. Our photometry revealed the presence of a β Cep variable in the SZ Cam hierarchical system, probably located within the non-eclipsing SB1 pair. The pulsation period is (0.33265 ± 0.00005) days and the observed total amplitude in the B band is (0.0105 ± 0.0005) mag. NLTE analysis of the disentangled spectra provided atmospheric parameters for all three components, consistent with those derived from orbital solution.

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Section: Introductionmentioning

confidence: 91%

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

Tamajo

Munari

Siviero

et al. 2012

A&A

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“…It was first resolved by the Hipparcos mission (ρ = 0.711 ± 0.011 arcsec, ΔH P = 1.87 ± 0.04 mag). Afterwards, it has been astrometrically followed up by several authors (Mason et al 1999;Balega et al 2002Balega et al , 2004Balega et al , 2007Richichi et al 2007). …”

Section: Wds 01024+0504 (Hd 6101 Ab and G 1-45 Ab)mentioning

confidence: 99%

“…On the other hand, G 210-44 AB, of combined spectral type M1V, is another close binary first resolved by Hipparcos (ρ = 0.334 ± 0.023 arcsec, ΔH P = 1.30 ± 0.27 mag -see also Balega et al 2004Balega et al , 2007. Using the theoretical models of Baraffe et al (1998) Table 4).…”

Section: Wds 20599+4016 (Hd 200077 Ae-d and G 210-44 Ab)mentioning

confidence: 99%

Reaching the boundary between stellar kinematic groups and very wide binaries

Caballero¹

2009

A&A

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Aims. I look for and characterise very wide binaries and multiple systems with projected physical separations larger than s = 0.1 pc, which is generally believed to be a sharp upper limit to the distribution of wide binary semimajor axes. Methods. I investigated in detail 30 Washington double stars with angular separations of ρ > 1000 arcsec. I discarded 23 of them as probably unbound systems based on discordant astrometry, photometry, spectral types, and radial velocities. The remaining seven systems were subject to a comprehensive data compilation and derivation (multi-wavelength photometry, heliocentric distance, multiplicity, age, mass, metallicity, membership in a young kinematic group). Results. Of the seven very wide systems, six have projected physical separations greater than the hypothetical cutoff at s = 0.1 pc and four have separations s > 0.2 pc. Although there are two systems in young kinematic groups (namely HD 136654 and BD+32 2572 in the Hyades Supercluster, and AU Mic and AT Mic AB in the β Pictoris moving group), there is no clear prevalence of young systems (τ < 1 Ga) among these very wide binaries. Finally, I compare the binding energies of the seven systems with those of other weakly bound systems in the field.

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“…New measurements, because they will be performed after the system passed through the periastron, could contribute to a more accurate determination of the orbital elements. In Balega et al (2007Balega et al ( , 2013 we find that the position angles from 2003.9275 and 2004.8237 have 180…”

Section: Individual Systemsmentioning

confidence: 99%

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Cvetković

Pavlović

Ninković

2014

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In this paper, we analyze new orbital elements and the quantities that follow from them for eight binaries: WDS 00101+3825 = HDS 23Da,Db, WDS 00321−1218 = HDS 71, WDS 04287+2613 = HDS 576, WDS 04389−1207 = HDS 599, WDS 16206+4535 = HDS 2309, WDS 17155+1052 = HDS 2440, WDS 22161−0705 = HDS 3158, and WDS 23167+3441 = HDS 3315. For seven of them, the orbital elements are calculated for the first time. Binaries, denoted as HDS, were discovered during the Hipparcos mission, and their first observational epoch is 1991.25, the same as the mean epoch of the Hipparcos catalog. We found all other measurements of these binaries in databases. They were obtained in the last 15 yr using the speckle interferometric technique. All studied pairs are close, and all measured separations are less than 0. 4. The resulting orbital periods fall within 26 and 80 yr. In addition to the orbital elements, we also give (O − C) residuals in θ and ρ, masses, dynamical parallaxes, absolute magnitudes, spectral types, and ephemerides for the next 5 yr.

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Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

Cited by 62 publications

References 23 publications

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

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

Reaching the boundary between stellar kinematic groups and very wide binaries

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

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