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Gamma Cas Stars as Be + White Dwarf Binary Systems
Douglas Gies, Luqian Wang, Robert Klement
The origin of the bright and hard X-ray emission flux among the gamma Cas subgroup of B-emission line (Be) stars may be caused by gas accretion onto an orbiting white dwarf (WD) co…
CHARA/SPICA: a 6-telescope visible instrument for the CHARA Array
Denis Mourard, Philippe Berio, Cyril Pannetier +25
With a possible angular resolution down to 0.1-0.2 millisecond of arc using the 330 m baselines and the access to the 600-900 nm spectral domain, the CHARA Array is ideally configu…
Dynamical masses of the primary Be star and the secondary sdB star in the single-lined binary kappa Dra (B6 IIIe)
R. Klement, D. Baade, Th. Rivinius +16
Because many classical Be stars may owe their nature to mass and angular-momentum transfer in a close binary, the present masses, temperatures, and radii of their components are of…
Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel +18
We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obta…
ARMADA II: Further Detections of Inner Companions to Intermediate Mass Binaries with Micro-Arcsecond Astrometry at CHARA and VLTI
Tyler Gardner, John D. Monnier, Francis C. Fekel +18
We started a survey with CHARA/MIRC-X and VLTI/GRAVITY to search for low mass companions orbiting individual components of intermediate mass binary systems. With the incredible pre…
Design of the new CHARA instrument SILMARIL: pushing the sensitivity of a 3-beam combiner in the H- and K-bands
Cyprien Lanthermann, Theo ten Brummelaar, Peter Tuthill +5
Optical interferometry is a powerful technique to achieve high angular resolution. However, its main issue is its lack of sensitivity, compared to other observation techniques. Eff…