Slim Disk Model for Soft X-Ray Excess and Variability of Narrow-Line Seyfert 1 Galaxies

Narrow-line Seyfert 1 galaxies (NLS1s) exhibit extreme soft X-ray excess and large variability. We argue that both features can be basically accounted for by the slim disk model. We assume that a central black-hole mass in NLS1 is relatively small, $M sim 10^{5-7}M_odot$, and that a disk shines nearly at the Eddington luminosity, $L_{rm E}$. Then, the disk becomes a slim disk and exhibits the following distinctive signatures: (1) The disk luminosity (particularly of X-rays) is insensitive to mass-flow rates, $dot M$, since the generated energy is partly carried away to the black hole by trapped photons in accretion flow. (2) The spectra are multi-color blackbody. The maximum blackbody temperature is $T_{rm bb} simeq 0.2(M/10^5 M_odot)^{-1/4}$ keV, and the size of the blackbody emitting region is small, $r_{rm bb} lsim 3 r_{rm S}$ (with $r_{rm S}$ being Schwarzschild radius) even for a Schwarzschild black hole. (3) All the ASCA observation data of NLS1s fall onto the region of $dot M/(L_{rm E}/c^2)>10$ (with $L_{rm E}$ being the Eddington luminosity) on the ($r_{rm bb},T_{rm bb}$) plane, supporting our view that a slim disk emits soft X-rays at $sim L_{rm E}$ in NLS1s. (4) Magnetic energy can be amplified, at most, up to the equipartition value with the trapped radiation energy which greatly exceeds radiation energy emitted from the disk. Hence, energy release by consecutive magnetic reconnection will give rise to substantial variability in soft X-ray emission.