Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.344..123f&link_type=abstract
In ESA, Solar Physics and Astrophysics at Interferometric Resolution p 123-130 (SEE N93-10901 01-90)
Astronomy and Astrophysics
Astronomy
Galactic Structure, High Resolution, Imaging Spectrometers, Interferometry, Spaceborne Astronomy, Stellar Activity, Binary Stars, Diameters, Emission Spectra, Line Spectra, Stellar Evolution, Stellar Magnetic Fields, Stellar Physics, Stellar Structure, Tomography
Scientific paper
The ability of the Solar Interferometric Mission for Ultrahigh Resolution Imaging and Spectroscopy (SIMURIS) instruments to access nonsolar objects, with an interesting resolution for several stellar programs in preparation for future long baseline interferometers in space or on the Moon is considered. Stellar angular diameters can be measured below the Rayleigh resolution of the Solar Ultraviolet Network (SUN) interferometer, by calibration of the point spread function and by differential interferometric centroid measurements in the blue and red wings of a given spectral line. Using both SUN spatial resolution and Imaging Fourier Transform Spectrometer (IFTS) spectral resolution, the separations and velocity curves of binary stars can be determined at several wavelengths. In particular, separations of binaries including cepheids or supergiants brighter than 12 and a hotter companion brighter than 15 at 180 nm can be obtained down to 0.1 arcsec up to 2 kpc in the galaxy, thus allowing the masses and distances of the components to be solved. Stellar magnetic activity phenomena can be traced ideally in the UV and XUV, through chromospheric, transition region, and coronal lines. Rotational modulation, Doppler tomography, and differential interferometric imaging can be combined to provide a map of active stars in different lines formed at different temperatures and height, giving a three dimensional view of the global activity phenomena on nearby stars and binaries. SIMURIS will also be able to address the diagnostics of stellar flares, extended coronal structures, or for their circumstellar environment and mass transfer phenomena.
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