Tracing the Dynamic Orbit of the Young, Massive High-Eccentricity Binary System θ1 Orionis C. First results from VLTI aperture-synthesis imaging and ESO 3.6-metre visual speckle interferometry

Details Tracing the Dynamic Orbit of the Young, Massive High-Eccentricity Binary System θ1 Orionis C. First results from VLTI aperture-synthesis imaging and ESO 3.6-metre visual speckle interferometry Tracing the Dynamic Orbit of the Young, Massive High-Eccentricity Binary System θ1 Orionis C. First results from VLTI aperture-synthesis imaging and ESO 3.6-metre visual speckle interferometry

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009msngr.136...44k&link_type=abstract

The Messenger, vol. 136, p. 44-47

Physics

3

Scientific paper

Located in the Orion Trapezium Cluster, θ1 Ori C is one of the youngest and nearest high-mass stars known. Besides its unique properties as an oblique magnetic rotator, the star happens to be a close (~20 milliarcseconds) binary system, which makes it an ideal laboratory to determine the fundamental parameters of young hot stars. In this article, we report on our 11-year interferometric monitoring campaign, which covers nearly the full dynamic orbit of the system and resulted in the first interferometric images obtained with the VLT interferometer (VLTI) in the infrared (~20 µm) and diffraction-limited bispectrum speckle interferometry at the ESO 3.6-metre telescope at visual (440 nm) wavelengths.

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