The magnetic field of Sigma Orionis E

Landstreet, J. D.; Borra, E. F.

doi:10.1086/182746

Cited by 170 publications

(172 citation statements)

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“…But despite the importance of σ Ori E for our understanding of the hot-star magnetospheres, relatively little emphasis was put on collecting precise information about its magnetic field and the stellar surface structures. σ Ori E is known to have ∼ 10 kG dipolar-like magnetic field (Landstreet & Borra 1978) and high-contrast surface abundance inhomogeneities (Reiners et al 2000), yet the previous analyses of these surface structures did not proceed beyond simple parametric models of abundance spots (Veto et al 1991) and dipolar fits to the longitudinal magnetic field measurements (Townsend et al 2005). We have collected high-resolution, wide wavelength coverage circular polarization spectra of σ Ori E with the ESPaDOnS and NARVAL polarimeters.…”

Section: σ Ori Ementioning

confidence: 99%

Magnetic Doppler imaging of early-type stars

et al. 2010

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Abstract. Doppler imaging of early-type magnetic stars is the most advanced method to interpret their line profile variations. DI allows us to study directly a complex interplay between chemical spots, magnetic fields, and the mass loss. Here we outline the general principles of the surface mapping of stars, discuss adaption of this technique to early-type stars and present several recent examples of the abundance and magnetic mapping performed for rapidly rotating early-B stars. In particular, we present the first Doppler images for the very fast rotating He-rich star HR 7355 and a reconstruction of magnetic field for the well-known Bp star σ Ori E. We also present new magnetic maps for the He-strong star HD 37776, which possesses one of the most complex magnetic field topologies among the upper main sequence stars.

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Section: σ Ori Ementioning

confidence: 99%

Magnetic Doppler imaging of early-type stars

et al. 2010

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“…2). Subsequent investigations (see Groote & Hunger 1982, and references therein) revealed corresponding rotational modulation in a panoply of observables, and their detection of a ∼ 10 kG dipole magnetic field led Landstreet & Borra (1978) to conclude that the star's variability arises from 'hot gas [. .…”

Section: Circumstellar Structurementioning

confidence: 99%

“…Given the richness of the observational data, it is straightforward to determine empirically that the magnetospheric plasma around σ Ori E is predominantly confined into a pair of co-rotating clouds situated above the intersections between magnetic and rotational equators (e.g., Landstreet & Borra 1978;Groote & Hunger 1982). But what is the physical reason for such a plasma distribution?…”

Section: Rigid-field Modelsmentioning

confidence: 99%

Modeling the winds and magnetospheres of active OB stars

Townsend

2010

Proc. IAU

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Abstract. After briefly reviewing the theory behind the radiative line-driven winds of OB stars, I examine the processes that can generate structure in them; these include both intrinsic instabilities, and surface perturbations such as pulsation and rotation. I then delve into wind channeling and confinement by magnetic fields as a mechanism for forming longer-lived circumstellar structures. With a narrative that largely follows the historical progression of the field, I introduce the key insights and results that link the first detection of a magnetosphere, over three decades ago, to the recent direct measurement of magnetic braking in a number of active OB stars.

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“…Six of the seven stars have variable magnetic fields and one a static field (Landstreet and Borra, 1978;Borra and Landstreet, 1979;Borra et al 1983;). Five have v sini cs 150 kms , with periods P <• 2d, and three have v sini <r 30 kms" , with P > 9d (Walborn, 1983).…”

Section: Statistics Rotationmentioning

confidence: 99%

Intermediate Helium Stars: Atmospheric Parameters, Oblique Rotators and Shells

Hunger

1985

International Astronomical Union Colloquium

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Intermediate helium stars are defined bynHe/nH being the number ratio of He over H. The upper bound which separates the intermediates from the extremes is well-defined (see Sect. 7), whereas the lower bound is rather soft.The first intermediate helium star discovered was Sigma Ori E (Greenstein and Wallerstein, 1956). Since then, 23 intermediates with V ≤ 1lm have been found (see the list of Walborn, 1983 and also the Annex), mostly through surveys such as that by McConnell et al. (1970) and McConnell (1972). (To this list, the newly discovered object SB 939, Langhans and Heber, 1985, should be added.) It is anticipated that a substantial fraction has as yet escaped detection. The spectral type centres around B2V while nHe/nH is typically of the order of unity.

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The magnetic field of Sigma Orionis E

Cited by 170 publications

References 0 publications

Magnetic Doppler imaging of early-type stars

Magnetic Doppler imaging of early-type stars

Modeling the winds and magnetospheres of active OB stars

Intermediate Helium Stars: Atmospheric Parameters, Oblique Rotators and Shells

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