| dc.creator | Dai, Zhibin | |
| dc.creator | Qian, Shengbang | |
| dc.creator | Fernández Lajús, Eduardo | |
| dc.date | 2009 | |
| dc.date | 2019-10-04T17:54:16Z | |
| dc.identifier | http://sedici.unlp.edu.ar/handle/10915/82785 | |
| dc.identifier | issn:0004-637X | |
| dc.description | We presented three new CCD observations of light minima of Z Chamaeleonis. All 187 available times of light minimum including 37 photographic data are compiled, and a new orbital period analysis is made by means of the standard O - C technique. The O - C diagram of Z Chamaeleonis presents a cyclical periodic change of 32.57 yr with a high significance level. We attempted to apply two plausible mechanisms (i.e., Applegate's mechanism and light travel-time effect) to explain the cyclical variations of orbital period shown in the O-C diagram. Although the previous works suggested that solar-type magnetic cycles in the red dwarf are the best explanation, the analysis of Applegate's mechanism in this paper presents a negative result. Accordingly, a light travel-time effect is proposed, and a brown dwarf as a tertiary component orbiting around dwarf nova Z Chamaeleonis is derived with a significance level of ≳81.6%, which may be a plausible explanation of the periodic variation in the systemic velocity of Z Chamaeleonis in superoutburst. | |
| dc.description | Facultad de Ciencias Astronómicas y Geofísicas | |
| dc.format | application/pdf | |
| dc.format | 109-113 | |
| dc.language | en | |
| dc.rights | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
| dc.rights | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
| dc.subject | Ciencias Astronómicas | |
| dc.subject | Binaries:eclipsing | |
| dc.subject | Cataclysmic variables | |
| dc.subject | Novae | |
| dc.subject | Stars:individual (Z Chamaeleonis) | |
| dc.title | Evidence of a brown dwarf in the eclipsing dwarf nova Z Chamaeleonis | |
| dc.type | Articulo | |
| dc.type | Articulo | |
