A wavelet analysis method is introduced to study the possible periods of PKS 1510-089 in radio bands. By compiling the radio light curve of PKS 1510-089 at frequencies of 22 and 37 GHz from 1990 to 2005, and using the...A wavelet analysis method is introduced to study the possible periods of PKS 1510-089 in radio bands. By compiling the radio light curve of PKS 1510-089 at frequencies of 22 and 37 GHz from 1990 to 2005, and using the wavelet analysis method, the evidence of quasi-periodic activity in PKS 1510-089 was obtained. The results indicate that: (1) There are two stable outburst periods of T1=(1.80±0.06) yr and T2= (0.90±0.07) yr presenting in the isoplethal map of PKS 1510-089 at the radio band 37 GHz; (2) there is an outburst period of T1=(1.80±0.06) yr presenting at the radio band 22 GHz; (3) by the continuum of the isograms map, we find the primary period of PKS 1510-089 is T1=(1.80±0.06) yr, and the period of T2= (0.90±0.07) yr may be the half period. The above results are consistent with the reports of Xie et al. (2004, 2005, 2008), Wu et al. (2005) and Liu & Fan (2007), using the other methods. We can expect that the next burst will be in January 2011.展开更多
Observations of PKS 1510-089 indicate the existence of a deep flux minimum with a timescale of -35 min and an interval of about 336 ± 14 d. A binary black hole system is proposed to be at the nucleus of this obje...Observations of PKS 1510-089 indicate the existence of a deep flux minimum with a timescale of -35 min and an interval of about 336 ± 14 d. A binary black hole system is proposed to be at the nucleus of this object. The secondary black hole orbits around the primary black hole. The minimum is caused by the periodic eclipse of the primary black hole by the secondary black hole. Based on the observations of PKS 1510-089, we estimate the parameters of the binary black hole system. The masses for the primary and secondary black holes are 1.37 × 10^9M⊙（M⊙ is the solar mass） and 1.37 × 10^7M⊙, and the major axis for this pair being about 0.1 parsec（pc）.展开更多
基金Supported by the National Natural Science Foundation of China (Grant Nos. 10821061, 10763002, and 10663002)the National Basic Research Program of China (Grant No. 2007CB815103)the Natural Science Foundation of Yunnan Province (Grant No. 2008CC011)
文摘A wavelet analysis method is introduced to study the possible periods of PKS 1510-089 in radio bands. By compiling the radio light curve of PKS 1510-089 at frequencies of 22 and 37 GHz from 1990 to 2005, and using the wavelet analysis method, the evidence of quasi-periodic activity in PKS 1510-089 was obtained. The results indicate that: (1) There are two stable outburst periods of T1=(1.80±0.06) yr and T2= (0.90±0.07) yr presenting in the isoplethal map of PKS 1510-089 at the radio band 37 GHz; (2) there is an outburst period of T1=(1.80±0.06) yr presenting at the radio band 22 GHz; (3) by the continuum of the isograms map, we find the primary period of PKS 1510-089 is T1=(1.80±0.06) yr, and the period of T2= (0.90±0.07) yr may be the half period. The above results are consistent with the reports of Xie et al. (2004, 2005, 2008), Wu et al. (2005) and Liu & Fan (2007), using the other methods. We can expect that the next burst will be in January 2011.
基金Project supported by State Key Development Program for Basic Research of China （Grant No 19990754）, the National Science Foundation for 0utstanding Young Scientists of China （Grant No 10125313）, the National Natural Science Foundation of China （Grant No 10573005）, and the Fund for Top Scholars of Guangdong Province, China （Grant No 02114）. Acknowledgments The authors wish to thank the referee for the comments and suggestions, and are also grateful for useful discussion to Dr Wang Hong-Guang, Liu Yi, Zhou Ji- Liang, Chen Jian-Ling and Xu Shou-Xi.
文摘Observations of PKS 1510-089 indicate the existence of a deep flux minimum with a timescale of -35 min and an interval of about 336 ± 14 d. A binary black hole system is proposed to be at the nucleus of this object. The secondary black hole orbits around the primary black hole. The minimum is caused by the periodic eclipse of the primary black hole by the secondary black hole. Based on the observations of PKS 1510-089, we estimate the parameters of the binary black hole system. The masses for the primary and secondary black holes are 1.37 × 10^9M⊙（M⊙ is the solar mass） and 1.37 × 10^7M⊙, and the major axis for this pair being about 0.1 parsec（pc）.
