1,781 research outputs found
A possible mechanism for multiple changing look phenomenon in Active Galactic Nuclei
Changing-look phenomenon observed now in a growing number of active galaxies
challenges our understanding of the accretion process close to a black hole. We
propose a simple explanation for the sources where multiple semi-periodic
outbursts are observed, and the sources are operating at a few per cent of the
Eddington limit. The outburst are caused by the radiation pressure instability
operating in the narrow ring between the standard gas-dominated outer disk and
the hot optically thin inner Advection-Dominated Accretion Flow. The
corresponding limit cycle is responsible for periodic outbursts, and the
timescales are much shorter than the standard viscous timescale due to the
narrowness of the unstable radial zone. Our toy model gives quantitative
predictions and works well for multiple outbursts like those observed in NGC
1566, NGC 4151, NGC 5548 and GSN 069, although the shapes of the outbursts are
not yet well modeled, and further development of the model is necessary.Comment: 10 pages, 10 figures. Accepted for publication in A&A. arXiv admin
note: text overlap with arXiv:1904.0676
The First Spectroscopically Resolved Sub-parsec Orbit of a Supermassive Binary Black Hole
One of the most intriguing scenarios proposed to explain how active galactic
nuclei are triggered involves the existence of a supermassive binary black hole
system in their cores. Here we present an observational evidence for the first
spectroscopically resolved sub-parsec orbit of a such system in the core of
Seyfert galaxy NGC 4151. Using a method similar to those typically applied for
spectroscopic binary stars we obtained radial velocity curves of the
supermassive binary system, from which we calculated orbital elements and made
estimates about the masses of components. Our analysis shows that periodic
variations in the light and radial velocity curves can be accounted for an
eccentric, sub-parsec Keplerian orbit of a 15.9-year period. The flux maximum
in the lightcurve correspond to the approaching phase of a secondary component
towards the observer. According to the obtained results we speculate that the
periodic variations in the observed H{\alpha} line shape and flux are due to
shock waves generated by the supersonic motion of the components through the
surrounding medium. Given the large observational effort needed to reveal this
spectroscopically resolved binary orbital motion we suggest that many such
systems may exist in similar objects even if they are hard to find. Detecting
more of them will provide us with insight into black hole mass growth process.Comment: 29 pages, 10 figures, published in ApJ, 759, 11
Exploring possible relations between optical variability time scales and broad emission line shapes in AGN
Here we investigate the connection of broad emission line shapes and
continuum light curve variability time scales of type-1 Active Galactic Nuclei
(AGN). We developed a new model to describe optical broad emission lines as an
accretion disk model of a line profile with additional ring emission. We
connect ring radii with orbital time scales derived from optical light curves,
and using Kepler's third law, we calculate mass of central supermassive black
hole (SMBH). The obtained results for central black hole masses are in a good
agreement with {other methods. This indicates that the variability time scales
of AGN may not be stochastic, but rather connected to the orbital time scales
which depend on the central SMBH mass.Comment: 13 pages, 3 figures, Accepted on 11 May 2018 Front. Astron. Space Sc
Quasars: from the Physics of Line Formation to Cosmology
Quasars accreting matter at very high rates (known as extreme Population A
[xA] or super-Eddington accreting massive black holes) provide a new class of
distance indicators covering cosmic epochs from the present-day Universe up to
less than 1 Gyr from the Big Bang. The very high accretion rate makes it
possible that massive black holes hosted in xA quasars radiate at a stable,
extreme luminosity-to-mass ratio. This in turns translates into stable physical
and dynamical conditions of the mildly ionized gas in the quasar low-ionization
line emitting region. In this contribution, we analyze the main optical and UV
spectral properties of extreme Population A quasars that make them easily
identifiable in large spectroscopic surveys at low-z (z < 1) and intermediate-z
(2 < z < 2.6), and the physical conditions that are derived for the formation
of their emission lines. Ultimately, the analysis supports the possibility of
identifying a virial broadening estimator from low-ionization line widths, and
the conceptual validity of the redshift-independent luminosity estimates based
on virial broadening for a known luminosity-to-mass ratio.Comment: 13 pages, 5 figures. Invited lecture at SPIG 2018, Belgrade. To
appear in Ato
Black hole mass estimates in quasars - A comparative analysis of high- and low-ionization lines
The inter-line comparison between high- and low-ionization emission lines has
yielded a wealth of information on the quasar broad line region (BLR) structure
and dynamics, including perhaps the earliest unambiguous evidence in favor of a
disk + wind structure in radio-quiet quasars. We carried out an analysis of the
CIV 1549 and Hbeta line profiles of 28 Hamburg-ESO high luminosity quasars and
of 48 low-z, low luminosity sources in order to test whether the
high-ionization line CIV 1549 width could be correlated with Hbeta and be used
as a virial broadening estimator. We analyze intermediate- to high-S/N,
moderate resolution optical and NIR spectra covering the redshifted CIV and
H over a broad range of luminosity log L ~ 44 - 48.5 [erg/s] and
redshift (0 - 3), following an approach based on the quasar main sequence. The
present analysis indicates that the line width of CIV 1549 is not immediately
offering a virial broadening estimator equivalent to H. At the same time
a virialized part of the BLR appears to be preserved even at the highest
luminosities. We suggest a correction to FWHM(CIV) for Eddington ratio (using
the CIV blueshift as a proxy) and luminosity effects that can be applied over
more than four dex in luminosity. Great care should be used in estimating
high-L black hole masses from CIV 1549 line width. However, once corrected
FWHM(CIV) values are used, a CIV-based scaling law can yield unbiased MBH
values with respect to the ones based on H with sample standard
deviation ~ 0.3 dex.Comment: 43 pages, 15 Figures, submitted to A&
Periodic optical variability of AGN
Here we present the evidence for periodicity of an optical emission detected in several AGN. Significant periodicity is found in light curves and radial velocity curves. We discuss possible mechanisms that could produce such periodic variability and their implications. The results are consistent with possible detection of the orbital motion in proximity of the AGN central supermassive black holes
The Line Emission Region in III Zw 2: Kinematics and Variability
We have studied the Ly-al, Hbeta, Halpha and Mg II2798 line profiles of the
Seyfert 1 galaxy III Zw 2. The shapes of these broad emission lines show
evidence of a multicomponent origin and also features which may be identified
as the peaks due to a rotating disk. We have proposed a two-component Broad
Line Region (BLR) model consisting of an inner Keplerian relativistic disk and
an outer structure surrounding the disk. The results of the fitting of the four
Broad Emission Lines (BELs) here considered, are highly consistent in both the
inner and outer component parameters. Adopting a mass of approx. 2 E8 sollar
masses for the central object we found that the outer radius of the disk is
approximately equal for the four considered lines (approx 0.01 pc). However,
the inner radius of the disk is not the same: 0.0018 pc for Ly-alpha, 0.0027 pc
for Mg II, and 0.0038 pc for the Balmer lines. This as well as the relatively
broad component present in the blue wings of the narrow [OIII] lines indicate
stratification in the emission-line region. Using long-term Hbeta observations
(1972-1990, 1998) we found a flux variation of the BEL with respect to the
[OIII] lines.Comment: ApJ, accepted, 22 pages, 10 figure
Modeling of sodium nitrite and water transport in pork meat
Four models were used to simulate nitrite uptake and water loss during pork meat curing with sodium nitrite: three empirical ones (the Azuara, the Peleg and the Zugarramurdi and Lupin) and one theoretical (the diffusional).
By means of the Azuara and the Peleg models, the equilibrium moisture content and the equilibrium nitrite content were properly identified.
Zugarramurdi and Lupin's model did not provide information about process parameters.
The effective diffusivities of water (Dwe) and nitrite (DNe) were calculated. The activation energy (ENa and Ewa) was evaluated from the parameters of both the Peleg and the diffusional models. The results were similar; the Peleg model having the advantage of simplicity of calculation.
The effect of meat anisotropy was confirmed from the diffusional model; the perpendicular transport of nitrite is easier than the parallel.
This study highlighted the importance of choosing the most appropriate model depending on the objective to be achieved.info:eu-repo/semantics/acceptedVersio
Biomass and Seed Yields of Big Bluestem, Switchgrass, and Intermediate Wheatgrass in Response to Manure and Harvest Timing at Two Topographic Positions
A principle attribute of perennial grasses for biomass energy is the potential for high yields on marginal lands. Objectives of this study were to compare biomass and seed production of intermediate wheatgrass (Thinopyrum intermedium [Host] Barkworth and D.R. Dewey), big bluestem (Andropogon gerardii Vitman), and switchgrass (Panicum virgatum L.) as affected by harvest timing and manure application on two topographic positions (footslope and backslope). Footslope is the hillslope position that forms the inclined surface at the base of a slope and backslope forms the steepest, middle position of the hillslope. Grasses were harvested for biomass at anthesis (summer), after a killing frost (autumn), or the following spring after overwintering in the field. Seed was harvested at maturity during 2003 and 2004. Two rates of beef cattle (Bos taurus L.) manure (target rates of 0 and 150 kg total‐N ha−1) were surface applied annually. Maximum annual biomass yield ranged from 4.4 to 5.2, 2.7 to 4.2, and 3.7 to 5.6 Mg ha−1 for intermediate wheatgrass, big bluestem, and switchgrass, respectively. Biomass yields were not different between fall and spring harvest treatments. Biomass yields of big bluestem and switchgrass at the backslope position were 86% and 96% of biomass yields at the footslope position with normal precipitation, respectively. Manure application increased biomass yield approximately 30% during the second year on both topographic positions. The highest seed yield was obtained from intermediate wheatgrass, followed by switchgrass and big bluestem. Utilizing these management practices in our environment, it appears that switchgrass and big bluestem could be allowed to overwinter in the field without suffering appreciable loss of biomass
Contribution of a Disk Component to Single Peaked Broad Lines of Active Galactic Nuclei
We study the disk emission component hidden in the single-peaked Broad
Emission Lines (BELs) of Active Galactic Nuclei (AGN). We compare the observed
broad lines from a sample of 90 Seyfert 1 spectra taken from the Sloan Digital
Sky Survey with simulated line profiles. We consider a two-component Broad Line
Region (BLR) model where an accretion disk and a surrounding non-disk region
with isotropic cloud velocities generate the simulated BEL profiles. The
analysis is mainly based in measurements of the full widths (at 10%, 20% and
30% of the maximum intensity) and of the asymmetries of the line profiles.
Comparing these parameters for the simulated and observed H broad
lines, we {found} that the hidden disk emission {may} be present in BELs even
if the characteristic {of two peaked line profiles is} absent. For the
available sample of objects (Seyfert 1 galaxies with single-peaked BELs), our
study indicates that, {in the case of the hidden disk emission in single peaked
broad line profiles}, the disk inclination tends to be small (mostly
) and that the contribution of the disk emission to the total flux
should be smaller than the contribution of the surrounding region.Comment: 18 Figures, 1 Table, MNRAS-accepted. MNRAS-accepte
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