2011A&A...532A.148B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:50:30

2011A&A...532A.148B - Astronomy and Astrophysics, volume 532A, 148-148 (2011/8-1)

A large Hα line forming region for the massive interacting binaries β Lyrae and υ Sagitarii.

BONNEAU D., CHESNEAU O., MOURARD D., BERIO P., CLAUSSE J.M., DELAA O., MARCOTTO A., PERRAUT K., ROUSSEL A., SPANG A., STEE Ph., TALLON-BOSC I., McALISTER H., TEN BRUMMELAAR T., STURMANN J., STURMANN L., TURNER N., FARRINGTON C. and GOLDFINGER P.J.

Abstract (from CDS):

This study aims at constraining the properties of two interacting binary systems by measuring their continuum-forming region in the visible and the forming regions of some emission lines, in particular Hα, using optical interferometry. We have obtained visible medium (R∼1000) spectral resolution interferometric observations of {beta} Lyr and of {upsilon} Sgr using the VEGA instrument of the CHARA array. For both systems, visible continuum (520/640nm) visibilities were estimated and differential interferometry data were obtained in the Hα emission line at several epochs of their orbital period. For {beta} Lyr, dispersed visibilities and phases were also obtained in the Hβ and the HeI 6678Å lines. As expected, for baselines shorter than 60 m, the system of {beta} Lyr is unresolved in the visible continuum, but the source associated with the Hα, the Hβ and the HeI 6678 Å lines appears to be well resolved at any orbital phase. The differential visibilities through these lines are lower during eclipses, indicating that significant emission originates close to the stars. The Hα line forming region appears to be made up of a compact source located near the orbital plane (possibly linked with the ``hot point'') and an extended source (i.e. ≥2mas, i.e. 125R) out of the orbital plane (possibly associated to the ``jet-like feature''). The {upsilon} Sgr continuum visibilities are at a similar level for short (20-25m) and long (90-110m) baselines. This is interpreted as the presence of an extended structure surrounding a compact bright source. No binary signal was detected, excluding a flux ratio between the stellar components of the system larger than 0.1 from 500 to 700nm. The radius of the brightest star is estimated to be 0.33±0.16mas, i.e. 21±10R using the latest Hipparcos distance. By contrast, the Hα line forming region is very extended (i.e. ≥6mas, i.e. 400R) and found to be off-center from the brightest star, following the orbital motion of the hidden companion. In both cases, the extension of the Hα line forming region is much larger than the size of the system, which is indicative of a non-conservative evolution. Although a large circumbinary disk surrounds the evolved system {upsilon} Sgr, storing a considerable part of the lost material, a substantial part of the Hα, Hβ, and the HeI 6678Å line emission derives from regions perpendicular to the orbital plane of {beta} Lyr.

Abstract Copyright:

Journal keyword(s): stars: emission-line, Be - binaries: close - circumstellar matter - stars: mass-loss - stars: individual: β Lyrae - stars: individual: υ Sagittarii

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * l Pup sg* 07 43 48.4687222 -28 57 17.372015 4.06 4.09 3.93 3.68 3.50 A4Iabe 175 0
2 * gam02 Sgr PM* 18 05 48.4880988 -30 25 26.723458 4.77 4.00 2.99 2.26 1.75 K0+III 129 0
3 * gam Sct * 18 29 11.8538827 -14 33 56.931865   4.739 4.675     A1IV/V 103 0
4 * bet Lyr bL* 18 50 04.7952472 +33 21 45.609978 2.85 3.42 3.42 3.31 3.29 B8.5Ib-II 886 0
5 * gam Lyr * 18 58 56.6224137 +32 41 22.400295 3.140 3.200 3.250 3.27 3.28 B9III 266 0
6 * ups Sgr Be* 19 21 43.6228354 -15 57 18.062473 4.18 4.71 4.61 4.34 4.21 B2Vp_sh 284 0
7 * nu. Cap * 20 20 39.8156206 -12 45 32.684421 4.61 4.72 4.76 4.75 4.81 B9IV 256 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:50:30

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