A Catalog of Magnetic Stars.

Babcock, Horace W.

doi:10.1086/190035

Cited by 387 publications

(328 citation statements)

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“…The Si star 108 Aqr is of interest because, according to Babcock (1958), a varying magnetic field is present. In addition, lines of Sr n are present and variable (Babcock 1958), and the lines of Tin vary markedly (Wolff and Wallerstein, unpublished).…”

Section: Observations and Resultsmentioning

confidence: 99%

Photometry of Three Peculiar A-Type Stars

Morrison¹,

Wolff²

1971

PASP

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Section: Observations and Resultsmentioning

confidence: 99%

Photometry of Three Peculiar A-Type Stars

Morrison¹,

Wolff²

1971

PASP

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“…21 "cold" Ap, with T e ff generally lower than 10000 K, were measured at OHP in april 1992 with Aurelie. The very peculiar Ca II K line profile observed on two objects, (3 CrB and HD 191742 (already noted as peculiar by Babcock 1958), are shown in Fig. 9.…”

Section: Uv Abundances Versus Visiblementioning

confidence: 78%

“…Since more than 30 years, the peculiarity of the Ca H K line (3933.7 A) profile in Ap stars, was noted by several authors (e.g. Babcock 1958 andWolff 1983). The results of the preceding sections lead us to investigate this problem in details, with high resolution and high signal-to-noise spectra.…”

Section: Uv Abundances Versus Visiblementioning

confidence: 82%

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Diffusion Models for Magnetic Ap Stars

Babel

1993

International Astronomical Union Colloquium

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Progress made in spectroscopy and in the diffusion theory permits now to make severe comparisons, based on line profiles, between theory and observation.We first review transport processes which are present in the atmospheric layers of Ap stars and discuss their relative importance. We then show that mass loss could play a key role for the creation of abundance maps. A mass loss model is proposed for 53 Cam and is compared, by spectrum synthesis, with visible and IUE high resolutions observations. The model accounts well for the line profiles of several elements with an exception for Ti. Furthermore, the abundance stratification predicted by this model gives close agreement with the large variation of the abundances of Cr and Fe found between the visible and UV domains. The diffusion-mass loss model finally permits to give a simple interpretation of the peculiar Ca II K lines observed in many Ap SrCrEu stars and in particular in 53 Cam, /? CrB and HD 191742.

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“…In his pioneering systematic search for magnetic fields in stars of various types, Babcock (1958) had observed a dozen Oe/Be stars. He had found no more than marginal evidence for the presence of magnetic fields in only two of them; these detections have never been confirmed since.…”

Section: Introductionmentioning

confidence: 99%

Can Magnetic Fields Be Detected in Be Stars?

Mathys

Smith

2000

International Astronomical Union Colloquium

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Abstract. The results of observations aimed at detecting magnetic fields in the Be star A Eri are reported. The observational data are analyzed both through application of an approximate analytical method and through computation of a number of simple numerical models in view of deriving constraints on the magnetic fields. General conclusions are drawn about future prospects for magnetic field detections in Be stars.

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A Catalog of Magnetic Stars.

Cited by 387 publications

References 0 publications

Photometry of Three Peculiar A-Type Stars

Photometry of Three Peculiar A-Type Stars

Diffusion Models for Magnetic Ap Stars

Can Magnetic Fields Be Detected in Be Stars?

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