Optical emission variability in the intermediate polars FO Aquarii, V1223 Sagittarii and AO PISCIUM

Details Optical emission variability in the intermediate polars FO Aquarii, V1223 Sagittarii and AO PISCIUM Optical emission variability in the intermediate polars FO Aquarii, V1223 Sagittarii and AO PISCIUM

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phdt........12m&link_type=abstract

Ph.D. Thesis Ohio State Univ., Columbus.

Computer Science

Balmer Series, Emission Spectra, Stellar Spectra, Stellar Winds, X Ray Spectra, X Ray Stars, Accretion Disks, H Beta Line, Helium Isotopes, Light Emission, Phase Shift, Radial Velocity, Sagittarius Constellation, Time Functions, Variability, Velocity Modulation

Scientific paper

The 1806 time resolved spectra of the intermediate polars FO Aqr, V1223 Sgr and AO Psc were obtained using the Ohio State Intensified Image Dissector Scanner attached to the Perkins 1.8 m telescope of the Ohio State and Ohio Wesleyan Univs. The spectra are flux calibrated and span the range of approx. 4250 to 5050A. FO Aqr exhibits two He II lambda 4686 flux components which vary on the 21 min period of this system and have large negative radial velocities. The phase shift of the two components is consistent with emission sources which lie at the secondary star and near the expected stream impact site at the outer edge of the He II lambda 4686 emission is due to reprocessing of x rays in hot winds at these two sites. V1223 Sgr also shows evidence of winds, as the H beta line, when phased on the orbital period, shows a strong radial velocity modulation on the redward side of the line, while the blueward side appears to be unmodulated in radial velocity. AO Psc exhibits deep flux modulation in the Balmer lines on the orbit period, a circumstance not unlike that found in FO Aqr. Furthermore, He I lambda 4471 goes into absorption in the line core over a span of approx. 0.25 of the orbit cycle.

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