Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832304h&link_type=abstract
American Astronomical Society, AAS Meeting #218, #323.04; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The eclipsing binary system 31 Cygni (K4 Ib + B3 V) was observed at several phases with the Far Ultraviolet Spectrosocopic Explorer (FUSE) satellite. During total eclipse, a rich emission spectrum was observed, produced by scattering of hot star photons in the extended wind of the K supergiant. The system was observed during deep chromospheric eclipse, and 2.5 months after total eclipse ended. We present an atlas of line identifications in these spectra.
During total eclipse, emission features from C II , C III, N I, N II, N III, O I, Si II, P II, P III, S II, S III, Ar I, Cr III, Fe II, Fe III, and Ni II were detected. The strongest emission features arise from N II. These lines appear strongly in absorption during chromospheric eclipse, and even 2.5 months after total eclipse, the absorption bottoms out on the underlying emission seen during total eclipse. The second strongest features in the emission spectrum arise from Fe III. Any chromospheric Fe III absorption is buried within strong chromospheric absorption from other species, mainly Fe II. The emission profiles of most of the doubly-ionized species are red-shifted relative to the systemic velocity, with asymmetric profiles with a steeper long-wavelength edge. Emission profiles from singly-ionized species tend to be more symmetric and centered near the systemic velocity.
In deep chromospheric eclipse, absorption features are seen from neutral and singly-ionized species, arising from lower levels up to 3 eV. Many strong chromospheric features are doubled in the observation obtained during egress from eclipse. The 31 Cygni spectrum taken 2.5 months after total eclipse ended ws compared to single-star B spectra from the FUSE archives. There was still some additional chromospheric absorption from strong low-excitation Fe II, O I and Ar I.
Bennett David P.
Hagen Bauer Wendy
No associations
LandOfFree
Line Identifications in the Far Ultraviolet Spectrum of the Eclipsing Binary System 31 Cygni does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Line Identifications in the Far Ultraviolet Spectrum of the Eclipsing Binary System 31 Cygni, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Line Identifications in the Far Ultraviolet Spectrum of the Eclipsing Binary System 31 Cygni will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1742589