Speckle interferometry of nearby multiple stars

Балега, И. И.; Balega, Yu. Yu.; Hofmann, K.-H.; Максимов, А. Ф.; Pluzhnik, Eugene; Schertl, D.; Shkhagosheva, Z. U.; Weigelt, G.

doi:10.1051/0004-6361:20020005

Cited by 122 publications

(101 citation statements)

References 18 publications

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“…Those stellar companions cited in the literature include only distant companions, whose radial velocity effects would be undetectable in our data. Balega et al (2002) found a companion to HD 15013 with a separation of 127 mas. Gaidos (1998) suggest that HD 96064 has a probable M dwarf companion at 270 AU.…”

Section: Other Nearby Young Starsmentioning

confidence: 99%

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Paulson¹,

Yelda

2006

PUBL ASTRON SOC PAC

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ABSTRACT. Radial velocity searches for substellar-mass companions have focused primarily on stars older than 1 Gyr. Increased levels of stellar activity in young stars hinders the detection of solar system analogs, and therefore until recently there has been a prejudice against inclusion of young stars in radial velocity surveys. Adaptive optics surveys of young stars have given us insight into the multiplicity of young stars, but only for massive, distant companions. Understanding the limit of the radial velocity technique, restricted to high-mass, close-orbiting planets and brown dwarfs, we began a survey of young stars of various ages. While the number of stars needed to carry out full analysis of the problems of planetary and brown dwarf population and evolution is large, the beginning of such a sample is included here. We report on 61 young stars ranging in age from the b Pictoris association (∼12 Myr) to the Ursa Major association (∼300 Myr). This initial search resulted in no stars showing evidence of companions larger than ∼1M Jup -2M Jup in short-period orbits at the 3 j level. We also present derived stellar parameters, as most have unpublished values. The chemical homogeneity of a cluster, and presumably of an association, may help to constrain true membership, so we present [Fe/H] abundances for the stars in our sample.

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Section: Other Nearby Young Starsmentioning

confidence: 99%

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Paulson¹,

Yelda

2006

PUBL ASTRON SOC PAC

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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%

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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“…A few years ago this system was resolved by Schoeller et al (1998) and Balega et al (2002) by means of speckle interferometry. Because the previous orbit shows a very strong disagreement with these observations, we have calculated a visual orbit (see Table 7) taking into account the spectroscopic elements and the speckle measurements.…”

Section: Bag 10 Aamentioning

confidence: 99%

A Methodology for the Description of Multiple Stellar Systems with Spectroscopic Subcomponents

Docobo

Andrade

2006

ApJ

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We propose a methodology for analyzing triple stellar systems that include a visual double star wherein one of the components is a single-or double-lined spectroscopic binary. By using this methodology, we can calculate the most probable values of the spectroscopic binary's inclination, the angular separation between its components, and its stellar masses, and we can even estimate the spectral types. For a few W UMaYtype eclipsing binaries, stellar radii are also determined. Moreover, we present new formulae for calculating stellar masses depending on spectral type. In this way we have studied 61 triple systems, five of them W UMaYtype eclipsing binaries with low-mass subcomponents. In addition, we study nine quadruple systems, applying the same methodology and considering them twice as a triple system. With the aim of having more accurate orbital elements, we have taken advantage of the occasion to calculate and improve orbits. In this way we have used a new speckle measurement to improve the orbital elements for the binary Hu 506 AB. Also, new visual orbits are calculated for the binaries BAG 10 Aa and LAB 6 Aa. Finally, we give a list of five spectroscopic binaries with more than 0B1 for the maximum angular separation; these should be easily observable as visual binaries by means of interferometric techniques.

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Speckle interferometry of nearby multiple stars

Cited by 122 publications

References 18 publications

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Reaching the boundary between stellar kinematic groups and very wide binaries

A Methodology for the Description of Multiple Stellar Systems with Spectroscopic Subcomponents

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