Article ID | Journal | Published Year | Pages | File Type |
---|---|---|---|---|
1779619 | New Astronomy | 2010 | 7 Pages |
Abstract
We present ultraviolet spectra of the AE Aqr binary system taken by the International Ultraviolet Explorer (IUE) during the period from 1978 to 1993, to accomplish a large scale study of what happens to the ultraviolet fluxes of different emission lines during different orbital phases. Five profiles of AE Aqr binary system show variations of line fluxes at different orbital phases are presented. We concentrated on studying N V emission line at 1240Â Ã
, O I emission line at 1306Â Ã
, He II emission line at 1640Â Ã
, N III emission line at 1749Â Ã
and Si III emission line at 1892Â Ã
, produced in the line emitting gas (Eracleous et al., 1994; Eracleous and Horne, 1996), by calculating the line fluxes of these spectral lines. Our results show that there are spectral variations of line fluxes for the aforementioned emission lines at different times, similar to the light curves found for AE Aqr binary system by using ASCA, XMM - Newton and Chandra X-ray observations (Mauche, 2006). We attributed these spectral variations to the variations of the mass-transfer rate (Ikhsanov et al., 2004) and to the collisions between the compact blobs and the fluffy blobs, where the collisions are supersonic, shocking the gas, causing heating, then expansion (Eracleous et al., 1994; Eracleous and Horne, 1996; Horne, 2009).
Related Topics
Physical Sciences and Engineering
Physics and Astronomy
Astronomy and Astrophysics
Authors
M.R. Sanad,