Research On The Accretion Disk-jet Connection For The ?-ray-loud Narrow-Line Seyfert 1 Galaxy

The accretion disk-jet connection of AGNs is an important question of AGNs.We have used the Yunnan Faint Object Spectrograph and Camera (YFOSC) mounted on the 2.4m Telescope of Lijiang Observatory of Yunnan Observatories to monitor the y-ray-loud narrow-line Seyfert 1 galaxy 1H 0323+342 for more than two months. Si-multaneous ?-ray light curve has been extracted from the Fermi data archive. We have found that the increment of the continuum from the accretion disk is simultaneous with the enhancement of the jet activity within several days. Based on the optical-corona X-ray correlation, the increment of the continuum from the accretion disk indicates the corona X-ray could increase. If the increment of the corona X-ray is due to increment of the accretion rate in the inner disk, the increment of accretion rate could lead to the enhancement of the jet activity.We have used the reverberation mapping to find the time lag between the H? and the g' light curves is 14.8-2.7+3.9 days in the rest frame. The measured black hole mass is M. = 3.4-0.6+0.9 × 107M?, and the dimensionless accretion rate is M = 1.11-0.47+0.69, in which M=M./LEddc-2,and M, is the mass accretion rate. We have also detected variations of optical Fe ? emissions and found that they have a lag of 15.0-4.1+7.4 days with respect to the g' light curve. The optical Fe ?, and the H,3 emissions have similar lags, indicating that they originate from an identical region.We have also used the lm Telescope and the 2.4m Telescope of Yunnan Observa-tories to monitor 1H 0323+342 photometrically from 2006 to 2410 in order to constrain the variability mechanism. The total observation nights are 41 days. The intraday vari-abilities (IDVs) are detected in the light curves. The calculated duty cycle is 28.3%,which could be underestimated because of the short observation durations of the nights.The mechanism for IDVs could be 'shock in jet' model, or 'jets in a jet' model. From 2006 to 2009, 1H 0323+342 has been observed using the lm Telescope. The over-all magnitude changes are AB = 0m.68, ?V = 1m.16, AR = 0m.22, ?I = 0m.50.From 2009 to 2010, it has been observed using the 2.4m Telescope. The overall mag-nitude changes are AB = 0m.16, ?V = 0m.35, AR = 0-.24, Al = 0m.32. In the color-magnitude diagram, there are bluer-when-brighter (BWB) chromatic trend for the intraday and long-term timescales, which could be explained by the 'shock in jet'model, and also possible due to two distinct components (one variable flatter compo-nent and one stable steeper component) or accretion disc model.