The Interpretation of ε Aurigae

Kuiper, G. P.; Struve, Otto; Strömgren, Bengt

doi:10.1086/143888

Cited by 48 publications

(25 citation statements)

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“…In the high-mass model (Kuiper et al 1937;Struve 1956;Carroll et al 1991), the F-supergiant primary is a more or less normal Based on observations with the VEGA/CHARA spectrointerferometer.…”

Section: Introductionmentioning

confidence: 99%

A high angular and spectral resolution view into the hidden companion ofεAurigae

Mourard¹,

Harmanec²,

Stencel³

et al. 2012

A&A

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The enigmatic binary, ε Aur, is yielding its parameters as a result of new methods applied to the recent eclipse, including optical spectro-interferometry with the VEGA beam combiner at the CHARA Array. VEGA/CHARA visibility measurements from 2009 to 2011 indicate the formation of emission wings of Hα in an expanding zone almost twice the photospheric size of the F star, namely, in a stellar wind. These may be caused by shocks in the atmosphere from large scale convective or multi-periodic pulsation modes emerging from the star. During the total eclipse phase in 2010, when the disk was in the line of sight, we saw broadening of the Hα absorption and a less steep drop of the visibility curve, consistent with the addition of neutral hydrogen in the line of sight but extended above and below the plane of the interferometrically imaged disk itself. This provides a unique constraint on the scale height of the gaseous component of the disk material, and, based on some additional assumptions, points to a mass of the central object being 2.4 to 5.5 M for a distance of 650 pc or 3.8 to 9.1 M for a distance of 1050 pc. These results can be tested during coming observing seasons as the star moves from eclipse phase toward quadrature.

show abstract

Section: Introductionmentioning

confidence: 99%

A high angular and spectral resolution view into the hidden companion ofεAurigae

Mourard¹,

Harmanec²,

Stencel³

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…The radial velocity of the emission may be constant, or slightly variable. The profiles of lines in the red region also differ from those reported by Sahade (1964). The cores of the non-metastable lines of Hei >U5876 and 6678 vary in quadrature with the orbital velocity curve; while the metastable line of Hei k5016 shows an almost constant velocity of -120 km s" 1 .…”

Section: O C Wilsonmentioning

confidence: 50%

“…Are these chromospheric features that you describe in the spectrum of s Aur the same ones that were described by Kuiper, Struve, and Stromgren (1937)? They described satellite lines that appeared around primary eclipse.…”

Section: R E Wilsonmentioning

confidence: 82%

“…For these extended atmospheres, very simple physical arguments show that a scattering theory is much more relevant to the under standing of transfer than is an absorption one, and I think that practically all microturbulence results are figured out with reference to the absorption-type curve of growth. All this has been pointed out by Menzel (1939).…”

mentioning

confidence: 85%

“…Biermann: Iben's pre-main-sequence tracks are a bit out of date. Larson (1969) showed that there is no Hayashi phase of any importance in the pre-main-sequence evolution of higher-mass stars.…”

Section: O C Wilsonmentioning

confidence: 99%

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