2011A&A...532A..80M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:21:24

2011A&A...532A..80M - Astronomy and Astrophysics, volume 532A, 80-80 (2011/8-1)

The binary Be star δ Scorpii at high spectral and spatial resolution. I. Disk geometry and kinematics before the 2011 periastron.

MEILLAND A., DELAA O., STEE P., KANAAN S., MILLOUR F., MOURARD D., BONNEAU D., PETROV R., NARDETTO N., MARCOTTO A., ROUSSEL A., CLAUSSE J.M., PERRAUT K., McALISTER H., TEN BRUMMELAAR T., STURMANN J., STURMANN L., TURNER N., RIDGWAY S.T., FARRINGTON C. and GOLDFINGER P.J.

Abstract (from CDS):

Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar disk that is responsible for the observed IR-excess and emission lines. The influence of binarity on these phenomena remains controversial. δ Sco is a binary system whose primary suddenly began to exhibit the Be phenomenon at the last periastron in 2000. We want to constrain the geometry and kinematics of its circumstellar environment. We observed the star between 2007 and 2010 using spectrally-resolved interferometry with the VLTI/AMBER and CHARA/VEGA instruments. We found orbital elements that are compatible with previous estimates. The next periastron should take place around July 5, 2011 (±4 days). We resolved the circumstellar disk in the Hα (FWHM=4.8±1.5mas), Brγ (FWHM=2.9±0.5mas), and the 2.06µm HeI (FWHM=2.4±0.3mas) lines, as well as in the K band continuum (FWHM≃2.4mas). The disk kinematics are dominated by the rotation, with a disk expansion velocity on the order of 0.2km/s. The rotation law within the disk is compatible with Keplerian rotation. As the star probably rotates at about 70% of its critical velocity, the ejection of matter does not seem to be dominated by rotation. However, the disk geometry and kinematics are similar to the previously studied quasi-critically rotating Be stars, α Ara, ψ Per and 48 Per.

Abstract Copyright:

Journal keyword(s): techniques: high angular resolution - techniques: interferometric - stars: emission-line, Be - stars: mass-loss - circumstellar matter - stars: individual: δ Sco

Simbad objects: 9

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Number of rows : 9

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 * gam Cas Be* 00 56 42.5317 +60 43 00.265 1.18 2.29 2.39 2.32 2.40 B0.5IVpe 1137 2
2 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 445 0
3 * psi Per Be* 03 36 29.3798227 +48 11 33.478941 3.60 4.17 4.23     B5Ve 396 0
4 * c Per Be* 04 08 39.6921578 +47 42 45.042937 3.45 4.00 4.03 3.91 3.93 B3Ve 365 0
5 * zet Tau Be* 05 37 38.6854231 +21 08 33.158804 2.22 2.84 3.03 3.06 3.15 B1IVe_shell 695 0
6 * kap CMa Be* 06 49 50.4593263 -32 30 30.522482 2.73 3.68 3.89 3.91 4.05 B1.5Ve 270 0
7 * del Cen Be* 12 08 21.4976373 -50 43 20.738614 1.51 2.39 2.52 2.48 2.62 B2Vne 293 0
8 * del Sco SB* 16 00 20.00528 -22 37 18.1431 1.30 2.20 2.32 2.36 2.49 B0.3IV 692 0
9 * alf Ara Be* 17 31 50.4915282 -49 52 34.122041 2.09 2.78 2.95 3.05 3.29 B2Vne 245 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:21:24

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