81 research outputs found
Synthesis and sorption properties of filled fibrous sorbents with immobilized hetarylformazan groups
New sorbents were prepared by immobilization of structurally different sulfur-containing hetaryl-formazans on nonwoven polyacrylonitrile fiber tilled with AV-17 anion exchanger. Sorption of some heavy metals on these materials was studied as influenced by various factors. Sorbents for selective recovery of copper(II) in the presence of nickel(II), zinc(II), and cadmium(II) cations were found
Synthesis and catalytic properties of copper(II) 1-aryl-5-benzothiazolylformazanates
New copper(II) benzothiazolylformazane complexes were synthesized and immobilized on AN-18 anion exchanger. The influence of the composition of the coordination core of copper(II) benzthiazolylformazanates and temperature on their catalytic properties in decomposition of H2O2 and oxidation of Na2S in aqueous solution was studied
Synthesis and spectroscopic features of iron(II) 1-aryl-5-benzothiazol-2- ylformazanates
New iron(II) coordination compounds with 1-aryl-5-(benzothiazol-2-yl) formazans were prepared. Their compositions and structures were determined by electronic spectroscopy, mass spectrometry, single crystal X-ray diffraction analysis, and magnetochemical measurements. © 2008 Pleiades Publishing, Ltd.Russian Foundation for Basic Researc
Synthetic approaches to 2-aryl/hetaryl- and 2-(hetaryl)ylidene derivatives of fluorinated 1,3-benzothiazin-4-ones
A series of 2-hetaryl- and 2-(hetaryl)ylidene substituted 5-fluoro-8-nitro-1,3-benzothiazin-4-ones was synthesized by interaction of 2,6-difluoro-3-nitrobenzoylisothiocyanate with C-nucleophiles. Cyclocondensation of polyfluorobenzoylchlorides with aryl and hetaryl thioamides represents new approach to 1,3-benzothiazin-4-ones. Some compounds proved to be promising for further development of tuberculostatic agents
Evolution of accretion disks around massive black holes: constraints from the demography of active galactic nuclei
Observations have shown that the Eddington ratios (the ratio of the
bolometric luminosity to the Eddington luminosity) in QSOs/active galactic
nuclei (AGNs) cover a wide range. In this paper we connect the demography of
AGNs obtained by the Sloan Digital Sky Survey with the accretion physics around
massive black holes and propose that the diversity in the Eddington ratios is a
natural result of the long-term evolution of accretion disks in AGNs. The
observed accretion rate distribution of AGNs (with host galaxy velocity
dispersion sigma~70-200 km/s) in the nearby universe (z<0.3) is consistent with
the predictions of simple theoretical models in which the accretion rates
evolve in a self-similar way. We also discuss the implications of the results
for the issues related to self-gravitating disks, coevolution of galaxies and
QSOs/AGNs, and the unification picture of AGNs.Comment: 18 pages, 2 figures; revised, main conclusions not changed; to appear
in ApJ, Oct., 200
Synthesis of 7-cycloalkylimino substituted 3-amino-6-fluoro-2-methyl-3H- quinazolin-4-ones
A versatile pathway for the synthesis of 7-cycloalkylimino substituted 3-amino-6-fluoro-2-methyl-3H-quinazolin-4-ones from 4,5-difluoroanthranylic acid has been advanced. Nucleophilic amination-defluorination reaction of the 6,7-difluoro derivative of 3-amino-2-methyl-3H-quinazolin-4-one has been established to occur at position 7, as shown by X-ray crystallographic analysis. © 2012 Elsevier B.V
Optical polarization observations with the MASTER robotic net
We present results of optical polarization observations performed with the
MASTER robotic net for three types of objects: gamma-ray bursts, supernovae,
and blazars. For the Swift gamma-ray bursts GRB100906A, GRB110422A, GRB121011A,
polarization observations were obtained during very early stages of optical
emission. For GRB100906A it was the first prompt optical polarization
observation in the world. Photometry in polarizers is presented for Type Ia
Supernova 2012bh during 20 days, starting on March 27, 2012. We find that the
linear polarization of SN 2012bh at the early stage of the envelope expansion
was less than 3%. Polarization measurements for the blazars OC 457, 3C 454.3,
QSO B1215+303, 87GB 165943.2+395846 at single nights are presented. We infer
the degree of the linear polarization and polarization angle. The blazars OC
457 and 3C 454.3 were observed during their periods of activity. The results
show that MASTER is able to measure substantially polarized light; at the same
time it is not suitable for determining weak polarization (less than 5%) of dim
objects (fainter than 16). Polarimetric observations of the optical
emission from gamma-ray bursts and supernovae are necessary to investigate the
nature of these transient objects.Comment: 31 pages, 12 figures, 4 tables; Exposure times in Table 2 have been
correcte
Can Thin Disks Produce Anomalous X-Ray Pulsars?
We investigate whether young neutron stars with fall-back disks can produce
Anomalous X-Ray Pulsars (AXPs) within timescales indicated by the ages of
associated supernova remnants. The system passes through a propeller stage
before emerging as an AXP or a radio pulsar. The evolution of the disk is
described by a diffusion equation which has self-similar solutions with either
angular momentum or total mass of the disk conserved. We associate these two
types of solutions with accretor and propeller regimes, respectively. Our
numerical calculations of thin disk models with changing inner radius take into
account the super-critical accretion at the early stages, and electron
scattering and bound-free opacities with rich metal content. Our results show
that, assuming a fraction of the mass inflow is accreted onto the neutron star,
the fall-back disk scenario can produce AXPs for acceptable parameters.Comment: 16 pages, 4 Figures, to be published in Astrophysical Journal Vol.
599, Dec. 1
Toward precise constraints on growth of massive black holes
Growth of massive black holes (MBHs) in galactic centers comes mainly from
gas accretion during their QSO/AGN phases. In this paper we apply an extended
Soltan argument, connecting the local MBH mass function with the time-integral
of the QSO luminosity function, to the demography of MBHs and QSOs from recent
optical and X-ray surveys, and obtain robust constraints on the luminosity
evolution (or mass growth history) of individual QSOs (or MBHs). We find that
the luminosity evolution probably involves two phases: an initial exponentially
increasing phase set by the Eddington limit and a following phase in which the
luminosity declines with time as a power law (with a slope of -1.2--1.3) set by
a self-similar long-term evolution of disk accretion. Neither an evolution
involving only the increasing phase with a single Eddington ratio nor an
exponentially declining pattern in the second phase is likely. The period of a
QSO radiating at a luminosity higher than 10% of its peak value is about
(2-3)x10^8 yr, during which the MBH obtains ~80% of its mass. The
mass-to-energy conversion efficiency is , with the
latter error accounting for the maximum uncertainty due to Compton-thick AGNs.
The expected Eddington ratios in QSOs from the constrained luminosity evolution
cluster around a single value close to 0.5-1 for high-luminosity QSOs and
extend to a wide range of lower values for low-luminosity ones. The Eddington
ratios for high luminosity QSOs appear to conflict with those estimated from
observations (~0.25) by using some virial mass estimators for MBHs in QSOs
unless the estimators systematically over-estimate MBH masses by a factor of
2-4. We also infer the fraction of optically obscured QSOs ~60-80%. Further
applications of the luminosity evolution of individual QSOs are also discussed.Comment: 25 pages, 13 figures, ApJ in pres
An Extreme Case of a Misaligned Highly Flattened Wind in the Wolf-Rayet Binary CX Cephei
CX Cep (WR 151) is the WR+O binary (WN5+O5V) with the second shortest period
known in our Galaxy. To examine the circumstellar matter distribution and to
better constraint the orbital parameters and mass-loss rate of the WR star, we
obtained broadband and multi-band (i.e. UBVRI) linear polarization observations
of the system. Our analysis of the phase-locked polarimetric modulation
confirms the high orbital inclination of the system (i.e. ). Using the
orbital solution of Lewis et al. (1993) we obtain masses of
and for the O and WR stars respectively, which agree with
their spectral types. A simple polarimetric model accounting for finite stellar
size effects allowed us to derive a mass-loss rate for the WR star of
. This result was remarkably independent of
the model's input parameters and favors an earlier spectral type for the WR
component (i.e. WN4). Finally, using our multi-band observations, we fitted and
subtracted from our data the interstellar polarization. The resulting constant
intrinsic polarization of is misaligned in relation to the orbital plane
(i.e. vs. ) and is the highest intrinsic
polarization ever observed for a WR star. This misalignment points towards a
rotational (or magnetic) origin for the asymmetry and contradicts the most
recent evolutionary models for massive stars (Meynet & Maeder 2003) which
predict spherically symmetric winds during the WR phase (i.e. ).Comment: 26 pages, 4 figures. Astrophysical Journal (submited
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