Search

Abstract: In this paper, we collect the redshift, bolometric luminosity, the full- width at half maximum of the H β emission line, the monochromatic luminosity at 5100Å and the radio loudness for the sample of 117 quasars, including 20 radio-quiet quasars (RQQs) and 97 radio-loud quasars (RLQs). With the reverberation mapping method we calculate the black hole mass and Eddington ratio for this sample, as well as the radio luminosity from the total 5GHz flux density. By analyzing the correlations among them, we obtain the following conclusions: (1) The black hole mass has weak correlations with the bolometric luminosity, radio loudness and radio luminosity for the RQQs, and has strong correlations with the bolometric luminosity, radio loudness and radio luminosity for the RLQs; (2) For the RQQs, the bolometric luminosity has weak correlations with the radio luminosity and 5 100Å monochromatic luminosity, and for the RLQs, the bolometric luminosity has strong correlations with the radio luminosity and 5 100Å monochromatic luminosity; (3) The RQQs and RLQs differ in the distributions of the black hole mass, emission line width and Eddington ratio. Based on these results, we suggest: the difference of emission line width between RQQs and RLQs is probably caused by the difference of black hole mass; the fundamental difference between RQQs and RLQs is caused by the difference of their intrinsic physical nature; the black hole mass, black hole spin, Eddington ratio, and host galaxy morphology are the important parameters to explain the origin of radio loudness and the double-peaked distribution; and the radio jet is closely related with the accretion rate of disk. [Copyright &y& Elsevier]

In many X-ray binaries (XRBs) at the low/hard state exists a fairly good correlation between the radio and X-ray luminosities. Dong et al. also found this relation in radio quiet quasars (RQQs), and its expression has a definite similarity with the expression for the fundamental plane of the XRBs in the low/hard state. The collected radio loud quasars (RLQs) are analyzed to see whether such a relation also exists in the RLQs or not, and these sources include 255 RLQs. The analyzed results show that (1) such a correlation exists not only between the black hole mass and radio/X-ray luminosity, but also between the Eddington ratio of radio luminosity and that of X-ray luminosity in the 255 RLQs, which has a definite similarity with the expression for the fundamental plane derived by Dong et al. from the black hole binaries at the bright/hard state and RLQs, but still exists a certain difference; (2) the expressions for the fundamental plane of the XRBs at the low/hard state and that of RLQs can be unified to be L R = 0.998 − 0.045 + 0.045   lg   L X + 0.592 − 0.049 + 0.049   lg   M B H − 6.56 − 1.605 + 1.605 ( L R is the radio luminosity, L X is the X-ray luminosity, and M BH is the black hole mass); (3) the fundamental plane expression composed of the radio and X-ray luminosities and black hole mass has a high universality, it can be used not only for the XRBs at the low/hard state and RQQs, but also for RLQs. [ABSTRACT FROM AUTHOR]

The formation of jets is closely related with the black hole mass and black hole spin, to study the correlations of jet power with the black hole mass and black hole spin is of significant importance for understanding the jet formation and structure. We have collected 65 radio loud quasars from the literature. The sample includes 35 Steep Spectrum Radio Quasars (SSRQs) and 30 Flat Spectrum Radio Quasars (FSRQs) with the redshifts ranging from about zero to two. We present here the correlation analysis of jet power with the black hole mass and back hole spin based on the sample data. Our conclusions are as follows: (1) The black hole mass has a strong correlation with the jet power; (2) The black hole spin is also strongly correlated with the jet power, especially for the magnetic field strength B = B EDD , where B EDD is the Eddington magnetic field strength, and the correlation coefficient is higher than that between black hole mass and jet power; (3) There are certain differences between the distributions of spin data of SSRQs and FSRQs; (4) This study has further confirmed that the jet energy is related not only with the black hole mass, but also with the spin energy of the black hole. The formation of black hole jet may be very possibly resulted by the joint effect of black hole mass and black hole spin. These results are consistent with the previous results obtained by other methods. [ABSTRACT FROM AUTHOR]

We have collected the 37 GHz radio data of PKS 1510-089 from 1990 to 2005, and obtained its long-term light curve after making data processing. From the light curve we can find that the activity in PKS 1510-089 is very strong. In this paper, the Period04 method is used for the first time to analyze the light periodicity of PKS 1510-089. The result indicates that its radio emission at 37 GHz has the periods of (1.87±0.13) yr and (0.87±0.07) yr. This result is consistent with the results obtained by Xie et al. in 2004, 2005, 2008, and Wu et al. in 2005 with other methods of data analysis. [ABSTRACT FROM AUTHOR]

Abstract: Correlation between the polarizations in the near-infrared and optical wavebands is studied with simultaneous observational data of blazars. It is found that the degree and angle of polarization in the near-infrared are correlated strongly with those in the optical. And so are the radiation fluxes at the two wavebands. It follows that the near-infrared radiation and polarization of blazars are mainly from synchrotron radiation of relativistic electrons, and come from the same region as the optical waveband. Correlations between the three near-infrared color indices J-H, H-K and J-K are also studied using the 2MASS data. It is found that both J-H and H-K are strongly correlated with J-K, while there is no correlation between J-H and H-K. Lastly, we studied the color index magnitude relationship and found that the near-infrared spectrum gets flatter as the source gets brighter. [Copyright &y& Elsevier]