1,613 research outputs found
Magnetic Coupling of a Rotating Black Hole with Advection-Dominated Accretion Flows
A model of magnetic coupling (MC) of a rotating black hole (BH) with
advection- dominated accretion flow (MCADAF) is proposed. It turns out that
MCADAF providers a natural explanation for the transition radius between ADAF
and SSD, and could be used to interpret the highest luminosity of GX 339-4 in
hard-state. A very steep emissivity index can be produced in the innermost part
of the MCADAF,which is consistent with the recent XMM-Newton observations of
the nearby bright Seyfert 1 galaxy MCG-6-30-15 and with two X-ray binaries
(XRBs): XTE J1655-500 and GX 339-4. In addition, we estimate the BH spins in
Seyfert 1 galaxy MCG-6-30-15 and in the two XRBs based on this model.Comment: 18 pages, 9 figures,acceptted by New Astronom
Does dichotomy of active galactic nuclei only depend on black hole spins?
A toy model for jet powers and radio loudness of active galactic nuclei
(AGNs) is proposed based on the coexistence of the Blandford-Znajek (BZ) and
magnetic coupling (MC) processes (CEBZMC) in black hole (BH) accretion disc. It
turns out that both the jet powers and radio-loudness of AGNs are controlled by
more than one physical parameter besides the BH spin. The observed dichotomy
between radio-loud and radio-quiet AGNs is well interpreted by the two
parameters, the BH spin and the power-law index of the variation of the
magnetic field on the disc. Furthermore, we discuss the correlation of jet
powers with radio loudness of AGNs in terms of the two parameters. It is found
that the contours of radio loudness are approximately in accord with those of
jet powers for several 3CR radio sources, implying roughly that the stronger
jet power corresponds to stronger radio loudness. In addition we discuss the
correlation of the jet powers and radio-loudness of AGNs with the position of
the inner edge of an accretion disc. These results imply that the spin paradigm
for radio loudness of AGNs might be modified by a scenario containing more
physical parameters.Comment: 7 pages, 9 figures. accepted by MNRA
A Toy Model for Magnetic Connection in Black-Hole Accretion Disc
A toy model for magnetic connection in black hole (BH) accretion disc is
discussed based on a poloidal magnetic field generated by a single electric
current flowing around a Kerr black hole in the equatorial plane. We discuss
the effects of the coexistence of two kinds of magnetic connection (MC) arising
respectively from (1) the closed field lines connecting the BH horizon with the
disc (henceforth MCHD), and (2) the closed field lines connecting the plunging
region with the disc (henceforth MCPD). The magnetic field configuration is
constrained by conservation of magnetic flux and a criterion of the screw
instability of the magnetic field. Two parameters and are introduced to
describe our model instead of resolving the complicated MHD equations. Compared
with MCHD, energy and angular momentum of the plunging particles are extracted
via MCPD more effectively, provided that the BH spin is not very high. It turns
out that negative energy can be delivered to the BH by the plunging particles
without violating the second law of BH thermodynamics, however it cannot be
realized via MCPD in a stable way.Comment: 11 pages, 9 figures, accepted by MNRA
Correlation between 3:2 QPO pairs and Jets in Black Hole X-ray Binaries
We argue, following our earlier works (the "CEBZMC model"), that the
phenomenon of twin peak high frequency quasi-periodic oscillations (QPOs)
observed in black hole X-ray binaries is caused by magnetic coupling (MC)
between accretion disk and black hole (BH). Due to MC, two bright spots occur
at two separate radial locations r_{in} and r_{out} at the disk surface,
energized by a kind of the Blandford-Znajek mechanism (BZ). We assume,
following the Kluzniak-Abramowicz QPO resonance model, that Keplerian
frequencies at these two locations are in the 3:2 ratio. With this assumption,
we estimate the BH spins in several sources, including GRO J1655-40, GRS
1915+105, XTE J1550-564, H1743-322 and Sgr A*. We give an interpretation of the
"jet line" in the hardness-intensity plane discussing the parameter space
consisting of the BH spin and the power-law index for the variation of the
large-scale magnetic field in the disk. Furthermore, we propose a new scenario
for the spectral state transitions in BH X-ray binaries based on fluctuation in
densities of accreting plasma from a companion star.Comment: 17 pages, 6 figures, accepted by AP
Enhanced sensing of optomechanically induced nonlinearity by linewidth suppression and optical bistability in cavity-waveguide systems
We study enhanced sensing of optomechanically induced nonlinearity (OMIN) in
a cavity-waveguide coupled system. The Hamiltonian of the system is anti-PT
symmetric with the two involved cavities being dissipatively coupled via the
waveguide. When a weak waveguide-mediated coherent coupling is introduced, the
anti-PT symmetry may break down. However, we find a strong bistable response of
the cavity intensity to the OMIN near the cavity resonance, benefiting from
linewidth suppression caused by the vacuum induced coherence. The joint effect
of optical bistability and the linewidth suppression is inaccessible by the
anti-PT symmetric system involving only dissipative coupling. Due to that, the
sensitivity is greatly enhanced by two orders of magnitude compared to that for
the anti-PT symmetric model. Moreover, the sensitivity shows resistances to a
reasonably large cavity decay and robustness to fluctuations in the
cavity-waveguide detuning. Based on the integrated optomechanical
cavity-waveguide systems, the scheme can be used for sensing different physical
quantities related to the single-photon coupling strength, and has potential
applications in high-precision measurements with physical systems involving
Kerr-type nonlinearity.Comment: 9 pages, 5 figure
Two new lignan-iridoid glucoside diesters from the leaves of Vaccinium bracteatum and their relative and absolute configuration determination by DFT NMR and TDDFT-ECD calculation
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