Abstract
As suggested by recent observations, we explore the influences of large-scale magnetic fields on the dynamics of slim disks. The magnetic fields are assumed to be self-similar and be a fixed fraction of the total pressure at the footpoint. The global solutions show that the radial velocity increases and the disk temperature decreases with enhancing magnetic fields. The ratio of the jet kinetic power to disk luminosity is less than 0.1, which indirectly support the argument that radio-loud (RL) narrow-line Seyfert 1 galaxies (NLS1s) are similar to blazars, with jets pointing to us.
Highlights
Radio and GeV γ-ray observations have shown that relativistic jets may exist in RL narrow-line Seyfert 1 galaxies (NLS1s).1–3 As well known, NLS1s are characterized by high accretion rate at sub or super Eddington rate, and the accretion disks can be described by slim model
Due to the torque exerted by the magnetic field lines, the angular momentum get removed more efficiently
Since the mass loss rate is very small compared to the accretion rate, the specific angular momentum changes only slightly
Summary
Radio and GeV γ-ray observations have shown that relativistic jets may exist in RL NLS1s.1–3 As well known, NLS1s are characterized by high accretion rate at sub or super Eddington rate, and the accretion disks can be described by slim model. Re-use and distribution is strictly not permitted, except for Open Access articles. The quantity Fz is the radiative cooling rate per unit surface area, M (r) is the accretion rate and mw(r) is the mass loss rate per unit area at radius r.
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