CCD photometry and astrometry of visual double 
and multiple stars of the HIPPARCOS Catalogue

Cuypers, J.; Seggewiss, W.

doi:10.1051/aas:1999512

Cited by 12 publications

(9 citation statements)

References 8 publications

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“…4); our spectra refer to the primary component for which we detect Ca II K emission. Separate magnitudes and V − I colors (V = 6.57/10.28, V −I = 0.59/1.56) were obtained by Cuypers & Seggewiss (1999). HD 221402: listed as an unsolved variable in the Hipparcos catalogue; we detect Ca II K emission.…”

mentioning

confidence: 67%

Fast-rotating nearby solar-type stars

Cutispoto¹,

Pastori²,

Pasquini³

et al. 2002

A&A

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mentioning

confidence: 67%

Fast-rotating nearby solar-type stars

Cutispoto¹,

Pastori²,

Pasquini³

et al. 2002

A&A

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“…B − V colors are taken from Table 1. V − I of HD 30101 and HD 219542 are from Cuypers & Seggewiss (1999) and those of HD 108584/5 and HD 135101 are from the Hipparcos Catalog. Transformation to the Johnson photometric system was performed following Bessell (1983).…”

Section: Differential Analysis Of Secondariesmentioning

confidence: 99%

Abundance difference between components of wide binaries

Desidera

Gratton

Scuderi

et al. 2004

A&A

101

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Abstract. We present iron abundance analysis for 23 wide binaries with main sequence components in the temperture range 4900-6300 K, taken from the sample of the pairs currently included in the radial velocity planet search on going at the Telescopio Nazionale Galileo (TNG) using the high resolution spectrograph SARG. The use of a line-by-line differential analysis technique between the components of each pair allows us to reach errors of about 0.02 dex in the iron content difference. Most of the pairs have abundance differences lower than 0.02 dex and there are no pairs with differences larger than 0.07 dex. The four cases of differences larger than 0.02 dex may be spurious because of the larger error bars affecting pairs with large temperature difference, cold stars and rotating stars. The pair HD 219542, previously reported by us to have a different composition, here is shown to be normal. For non-rotating stars warmer than 5500 K, characterized by a thinner convective envelope and for which our analyis appears to be of higher accuracy, we are able to exclude in most cases the consumption of more than 1 Earth Mass of iron (about 5 Earth masses of meteoritic material) during the main sequence lifetime of the stars, placing more stringent limits (about 0.4 Earth masses of iron) in five cases of warm stars. This latter limit is similar to the estimates of rocky material accreted by the Sun during its main sequence lifetime. Combining the results of the present analysis with those for the Hyades and Pleiades, we conclude that the hypothesis that pollution by planetary material is the only mechanism responsible for the highest metallicity of the stars with planets may be rejected at more than 99% level of confidence if the incidence of planets in these samples is as high as 8% and similar to the field stars included in current radial velocity surveys. However, the significance of this result drops considerably if the incidence of planets around stars in binary systems and clusters is less than a half of that around normal field stars.

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“…While each of these methods has its pro's and con's, on the whole the agreement between these various sets of temperatures Table 3. Temperature differences between components obtained using various methods: Second column: ionization equilibrium for Fe; Third column: excitation equilibrium for Fe I; Fourth column: temperatures from Hipparcos B − V colours, using the temperature calibration by Kurucz (1995); Fifth column: temperatures obtained from the difference in magnitude between the components, times the slope of the zero age main sequence; Sixth column: temperatures from V − I colours (Cuypers & Seggewiss 1999) using the calibration by Alonso et al (1996) (Cousins V − I colours were transformed into Johnson V − I colours using the calibration by Bessel 1983). Note that Hipparcos B − V colours are not very accurate because our systems are not resolved by the Hipparcos photometric beam; and temperatures from the difference in magnitude between the two components assume that they are unevolved, and are then upper limits to the actual temperature differences.…”

Section: Abundance Analysismentioning

confidence: 99%

Non-interacting main-sequence binaries with different chemical compositions: Evidences of infall of rocky material?

Gratton

Bonanno

Claudi

et al. 2001

A&A

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Abstract. We performed a careful differential abundance analysis of individual components of six main sequence binaries with separations of a few hundreds of AU. To reduce analysis concerns, we selected systems with almost equal mass components. We were able to derive differential abundances of several elements with errors down to 0.01 dex in the best cases. We found that in four systems the two components have the same chemical composition, within these very severe limits. However, clear differences were found for the two remaining systems (HD 219542 and HD 200466), in both cases the primaries being more Fe-rich than the secondaries, by 0.091 ± 0.009 and 0.053 ± 0.024 dex respectively. Similar differences were found for most of the elements considered in our analysis; however, we found no appreciable difference for volatile elements and a trend for increasing abundance differences with increasing condensation temperature for individual elements, a result similar to that found for some single stars with planets by Smith et al. (2001). Finally, we note that HD 219542A has a Li-abundance comparable to those of Li-rich stars in old open clusters, while no Li is detected in the slightly cooler HD 219542B. We suggest that the primaries of these two systems have accreted rocky planets or the inner dust-rich part of a protoplanetary disk, likely due to gravitational perturbation caused by the presence of the companion.

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CCD photometry and astrometry of visual double and multiple stars of the HIPPARCOS Catalogue

Cited by 12 publications

References 8 publications

Fast-rotating nearby solar-type stars

Fast-rotating nearby solar-type stars

Abundance difference between components of wide binaries

Non-interacting main-sequence binaries with different chemical compositions: Evidences of infall of rocky material?

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