Study of spectroscopic variabilities of star η Centauri
Full text
| |
| Author(s): |
Ronaldo Savarino Levenhagen
Total Authors: 1
|
| Document type: | Master's Dissertation |
| Press: | São Paulo. |
| Institution: | Universidade de São Paulo (USP). Instituto Astronômico e Geofísico (IAG/SBD) |
| Defense date: | 2000-08-14 |
| Examining board members: |
Nelson Vani Leister;
Augusto Damineli Neto;
Jean Kogovsek de Zorec
|
| Advisor: | Nelson Vani Leister |
| Abstract | |
The spectroscopy of Be stars carried out with high resolution and signal to noise relation allows to investigate quick time variations in line absorption profiles, usually due to non radial pulsations, among other mechanisms. The Be phenomenon is transitory for such stars. Indeed, their spectra may show characteristics of a normal B star, or a star with a "cold" circumstellar envelope (presence of sharp emission and absorption lines in visible spectrum). These stars are characterized by high speed rotation, however insufficient to explain high mass loss rates, whose mechanisms still remains misunderstood. In this work, we adopted the non-radial pulsation model (NRP) in order to explain the observed time series variations present in line profiles centered in HeI λ 667.8 nm. For this sake, it was used the CLEANEST method to carry out periodicity determinations, after some previous comparative tests of performance between this method and CLEAN. Both of them possess great efficiency in time analysis, however in average the CLEANEST method stood out both in determining frequencies and amplitudes. Besides, it were studied also other kinds of variability also present in these profiles, such as relative intensity variations in the wings of the profile and the variability in position of the central quasi-emission peak. The analyzed spectroscopic data constitute four sets of spectra obtained in 1995, 1996, 1997 and 1998 at the MCT/LNA. There is still one photometric data set coming from HIPPARCOS satellite spanning from 1990 to 1992. The spectroscopic and photometric data analysis have furnished results that agree with other works on η Centauri (AU) | |