HR 2727 : a double-line binary containing a magnetic AP star.

Bonsack, W. K.

doi:10.1086/154704

Cited by 18 publications

(21 citation statements)

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“…This star is remarkable, because it is only the fifth SB2 system known among magnetic Ap stars, after HD 55719 (Bonsack 1976), HD 98088 (Abt et al 1968;Wolff 1974), HD 59435 (Wade et al 1996) and HD 174016-7 (Ginestet et al 1999); HD 59435 had also been studied in the course of this survey, while a sixth case (HD 22128, see below) was discovered with ELODIE. Although HgMn stars are frequently seen in SB2 systems, this is exceptional among Si and SrCrEu stars.…”

Section: A1 Hd 5550 (= Bd +65 • 115 = Renson 1470)mentioning

confidence: 78%

“…For the coolest Ap stars, as well as for the HgMn stars, this rate behaves in the same way as for normal stars. Moreover, the magnetic Ap stars show a strong deficit of SB2 binaries: only two SB2's containing a magnetic Ap star had been well studied before the CORAVEL observations: HD 55719 (Bonsack 1976) and HD 98088 (Abt et al 1968;Wolff 1974). On the other hand, HgMn stars, which generally have no significant magnetic field (see, however, Mathys & Hubrig 1995), are often found in SB2 systems, and their companion seems to be always an Am star when its effective temperature is below 10 000 K (Ryabchikova 1998).…”

Section: Introductionmentioning

confidence: 99%

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Multiplicity among chemically peculiar stars

Carrier¹,

North²,

Babel³

2002

A&A

100

114

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Abstract. We present new orbits for sixteen Ap spectroscopic binaries, four of which might in fact be Am stars, and give their orbital elements. Four of them are SB2 systems: HD 5550, HD 22128, HD 56495 and HD 98088. The twelve other stars are: HD 9996, HD 12288, HD 40711, HD 54908, HD 65339, HD 73709, HD 105680, HD 138426, HD 184471, HD 188854, HD 200405 and HD 216533. Rough estimates of the individual masses of the components of HD 65339 (53 Cam) are given, combining our radial velocities with the results of speckle interferometry and with Hipparcos parallaxes. Considering the mass functions of 74 spectroscopic binaries from this work and from the literature, we conclude that the distribution of the mass ratio is the same for cool Ap stars and for normal G dwarfs. Therefore, the only differences between binaries with normal stars and those hosting an Ap star lie in the period distribution: except for the case of HD 200405, all orbital periods are longer than (or equal to) 3 days. A consequence of this peculiar distribution is a deficit of null eccentricities. There is no indication that the secondary has a special nature, like e.g. a white dwarf.

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Section: A1 Hd 5550 (= Bd +65 • 115 = Renson 1470)mentioning

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Multiplicity among chemically peculiar stars

Carrier¹,

North²,

Babel³

2002

A&A

100

114

View full text Add to dashboard Cite

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“…MHLLM could not definitely establish the value of the rotation period, but 847 or 775 days appear as most plausible. Nevertheless, it seems unavoidable that 2 or 3 of Bonsack's (1976) measurements are bound to be inconsistent with the bulk of his data, regardless of what the rotation period is (they were already discrepant with Bonsack's preferred period values). Except for these discrepant values, all of Bonsack's (1976) H z data are larger than our 3 measurements.…”

Section: Hd 55719mentioning

confidence: 82%

“…Nevertheless, it seems unavoidable that 2 or 3 of Bonsack's (1976) measurements are bound to be inconsistent with the bulk of his data, regardless of what the rotation period is (they were already discrepant with Bonsack's preferred period values). Except for these discrepant values, all of Bonsack's (1976) H z data are larger than our 3 measurements. If the interpretation proposed by MHLLM that the rotation period is longer than 2 years is correct, this hints at the existence of systematic differences betwen Bonsack's (1976) and our longitudinal field determinations.…”

Section: Hd 55719mentioning

confidence: 82%

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Spectropolarimetry of magnetic stars

Mathys

Hubrig

1997

Astron. Astrophys. Suppl. Ser.

175

133

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Abstract. New determinations of the mean longitudinal magnetic field, of the crossover, and of the mean quadratic magnetic field of Ap stars are presented. They are based on spectra recorded simultaneously in both circular polarizations at ESO with the CASPEC spectrograph fed by the 3.6 m telescope. This paper discusses 95 observations of 44 stars. A major result of this study is the discovery that HD 137509 has a predominantly quadrupolar magnetic field, a strucuture previously found in only a couple of stars. Improvement or revision of the determination of the rotation period has been achieved for 3 stars. The stars studied in this work include 14 rapidly oscillating Ap stars (for 6 of which no previous attempt to detect a magnetic field had ever been made) and 21 Ap stars with spectral lines resolved into their magnetically split components when observed at high enough dispersion in unpolarized light (for 9 of these stars, no determination of the longitudinal field had been performed before).The observations discussed in this paper have been performed between 1989 and 1994, a period during which CASPEC and its Zeeman analyzer have progressively undergone various configuration changes. The results reported here demonstrate that the polarimetric performance of the instrument has remained unaltered through these modifications. Thanks to the latter, the achieved resolving power was increased, which resulted in improved magnetic measurement accuracies.

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Giant CP Stars?

Lodén

Sundman²

1989

J Astrophys Astron

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HR 2727 : a double-line binary containing a magnetic AP star.

Cited by 18 publications

References 0 publications

Multiplicity among chemically peculiar stars

Multiplicity among chemically peculiar stars

Spectropolarimetry of magnetic stars

Giant CP Stars?

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