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Using high resolution data to investigate the variabilityOf gg carinae system

GG Carinae is a peculiar emission line object classified as a B[e] star. Using high resolution data we confirm that GG Carinae is at same time a binary system and a variable star. GG Carinae was classified by Lamers et al. (1998) as a B[e] star and also is pointed out as a binary system. So, any investigation to determine its parameters requires an detailed analysis in order to know and to separate the effects of each component. Gosset et al. (1984) used Fourrier Analysis in the data obtained from photoeletric photometry of both the standard UBV and Strongren system and calculated a period of 31.02. According the authors there are two possible scenarios for GG Carinae: i) GG Carinae has an assymetrical atmosphere where the P Cygni profiles are formed and the brightness variation would be caused by extintion due it is moving inside a nebulae; ii) the companion of GG Carinae must have a intense hydrogen-rich hot spot which orientation respect to observer would be responsible by the light variation. It is important to note that there is no conclusion about its binary nature as well as to the physical structure of his envelope. This unconclusive scenarium and the desire to take GG Carinae in account in our investigation about massive stars motivated us to analyse this star. In this work we present recent optical high resolution observations taken over the lightcurve of GG Carinae obtained by Gosset et al. (1985). These spectra show new aspects about the binary nature of GG Car and in special about the intrisic variability of the main star wich has been predicted by Kruytbosch (1930). The high resolution data were taken with the Fiber-fed Extended Range Optical Spectrograph (FEROS) that is a Echelle spectrograph with a spectral resolving power of R = 48 000 corresponding to 2.2 pixels of 15μm and with a wavelength coverage from 3600Å to 9200Å. The main aspects observed on the spectra of GG Carinae were: