16 research outputs found
ΠΡΠ°Π²ΠΎΠ²Ρ ΠΏΡΠΎΠ±Π»Π΅ΠΌΠΈ ΠΏΠΎΠΏΠ΅ΡΠ΅Π΄ΠΆΠ΅Π½Π½Ρ ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΎΠ³ΠΎ Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌΡ Π² Π£ΠΊΡΠ°ΡΠ½Ρ
Π ΠΎΠ·Π³Π»ΡΠ΄Π°ΡΡΡΡΡ ΠΎΡΠ½ΠΎΠ²Π½Ρ ΠΏΡΠΎΠ±Π»Π΅ΠΌΠΈ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠ³ΠΎ ΠΏΠΎΠΏΠ΅ΡΠ΅Π΄ΠΆΠ΅Π½Π½Ρ ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΎΠ³ΠΎ Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌΡ Π²ΠΈΡ
ΠΎΠ΄ΡΡΠΈ ΡΠΊ Π· Π²ΡΡΡΠΈΠ·Π½ΡΠ½ΠΎΠ³ΠΎ, ΡΠ°ΠΊ Ρ ΠΌΡΠΆΠ½Π°ΡΠΎΠ΄Π½ΠΎΠ³ΠΎ Π΄ΠΎΡΠ²ΡΠ΄Ρ. Π£ Π΄ΠΎΡΠ»ΡΠ΄ΠΆΠ΅Π½Π½Ρ Π°ΠΊΡΠ΅Π½- ΡΡΡΡΡΡΡ ΡΠ²Π°Π³Π° Π½Π° ΠΏΡΠΎΠ±Π»Π΅ΠΌΠ°Ρ
ΠΏΠΎΡΡΠΊΡ ΡΡΡΠΊΠΎΡ ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΎΡ Ρ ΡΡΠΈΠ΄ΠΈΡΠ½ΠΎΡ ΡΠ΅ΡΠΌΡΠ½ΠΎΠ»ΠΎΠ³ΡΡ ΠΏΠΎΠ½ΡΡΡΡ Β«ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΈΠΉ Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌΒ». ΠΠ²ΡΠΎΡ ΡΠΊΠ°Π·ΡΡ Π½Π° Π½Π΅ΠΎΠ±Ρ
ΡΠ΄Π½ΡΡΡΡ ΠΏΠΎΠ·ΠΈΡΡΠΎΠ½ΡΠ²Π°Π½Π½Ρ ΡΠΈΠΌΠ²ΠΎΠ»ΡΡΠ½ΠΎΠ³ΠΎ Ρ ΡΠ΅Π°Π»ΡΠ½ΠΎΠ³ΠΎ ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΎΠ³ΠΎ Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌΡ, Π½Π° Π²Π°ΠΆΠ»ΠΈΠ²ΠΎΡΡΡ Π΄ΠΈΡΠ΅ΡΠ΅Π½ΡΡΠ°ΡΡΡ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΡ Π±ΠΎΡΠΎΡΡΠ±ΠΈ Π· Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌΠΎΠΌ Ρ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠ³ΠΎ ΠΎΠ±ΠΌΠ΅ΠΆΠ΅Π½Π½Ρ Π΄ΡΡΠ»ΡΠ½ΠΎΡΡΡ ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΎΡ ΠΎΠΏΠΎΠ·ΠΈΡΡΡ.
ΠΠ»ΡΡΠΎΠ²Ρ ΡΠ»ΠΎΠ²Π°: ΠΏΠΎΠ»ΡΡΠΈΡΠ½ΠΈΠΉ Π΅ΠΊΡΡΡΠ΅ΠΌΡΠ·ΠΌ, ΡΠ΅ΡΠΎΡΠΈΠ·ΠΌ, ΠΏΠΎΠ»ΡΡΠΈΡΠ½Π° ΡΠΈΡΡΠ΅ΠΌΠ°, ΠΏΡΠ°Π²ΠΎΠ²Π΅ ΡΠ΅Π³ΡΠ»ΡΠ²Π°Π½Π½Ρ, ΠΌΠ°Π½ΡΠΏΡΠ»ΡΠ²Π°Π½Π½Ρ, ΠΎΠΏΠΎΠ·ΠΈΡΡΡ.Π Π°ΡΡΠΌΠ°ΡΡΠΈΠ²Π°ΡΡΡΡ ΠΎΡΠ½ΠΎΠ²Π½ΡΠ΅ ΠΏΡΠΎΠ±Π»Π΅ΠΌΡ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠ³ΠΎ ΡΠΏΡΠ΅ΠΆΠ΄Π΅Π½ΠΈΡ ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠΊΡΡΡΠ΅ΠΌΠΈΠ·ΠΌΠ° ΠΈΡΡ
ΠΎΠ΄Ρ ΠΊΠ°ΠΊ ΠΈΠ· ΠΎΡΠ΅ΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ³ΠΎ, ΡΠ°ΠΊ ΠΈ ΠΌΠ΅ΠΆΠ΄ΡΠ½Π°ΡΠΎΠ΄Π½ΠΎΠ³ΠΎ ΠΎΠΏΡΡΠ°. Π ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠΈ Π°ΠΊΡΠ΅Π½ΡΠΈΡΡΠ΅ΡΡΡ Π²Π½ΠΈΠΌΠ°Π½ΠΈΠ΅ Π½Π° ΠΏΡΠΎΠ±Π»Π΅ΠΌΠ°Ρ
ΠΏΠΎΠΈΡΠΊΠ° ΡΠ΅ΡΠΊΠΎΠΉ ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΈ ΡΡΠΈΠ΄ΠΈΡΠ΅ΡΠΊΠΎΠΉ
ΡΠ΅ΡΠΌΠΈΠ½ΠΎΠ»ΠΎΠ³ΠΈΠΈ ΠΏΠΎΠ½ΡΡΠΈΡ Β«ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΈΠΉ ΡΠΊΡΡΡΠ΅ΠΌΠΈΠ·ΠΌΒ». ΠΠ²ΡΠΎΡ ΡΠΊΠ°Π·ΡΠ²Π°Π΅Ρ Π½Π° Π½Π΅ΠΎΠ±Ρ
ΠΎΠ΄ΠΈΠΌΠΎΡΡΡ ΠΏΠΎΠ·ΠΈΡΠΈΠΎΠ½ΠΈΡΠΎΠ²Π°Π½ΠΈΡ ΡΠΈΠΌΠ²ΠΎΠ»ΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΈ ΡΠ΅Π°Π»ΡΠ½ΠΎΠ³ΠΎ ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠΊΡΡΡΠ΅ΠΌΠΈΠ·ΠΌΠ°, Π½Π°
Π²Π°ΠΆΠ½ΠΎΡΡΠΈ Π΄ΠΈΡΡΠ΅ΡΠ΅Π½ΡΠΈΠ°ΡΠΈΠΈ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠΉ Π±ΠΎΡΡΠ±Ρ Ρ ΡΠΊΡΡΡΠ΅ΠΌΠΈΠ·ΠΌΠΎΠΌ ΠΈ ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠ³ΠΎ ΠΎΠ³ΡΠ°Π½ΠΈΡΠ΅Π½ΠΈΡ
Π΄Π΅ΡΡΠ΅Π»ΡΠ½ΠΎΡΡΠΈ ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΎΠΏΠΏΠΎΠ·ΠΈΡΠΈΠΈ.
ΠΠ»ΡΡΠ΅Π²ΡΠ΅ ΡΠ»ΠΎΠ²Π°: ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠΈΠΉ ΡΠΊΡΡΡΠ΅ΠΌΠΈΠ·ΠΌ, ΡΠ΅ΡΡΠΎΡΠΈΠ·ΠΌ, ΠΏΠΎΠ»ΠΈΡΠΈΡΠ΅ΡΠΊΠ°Ρ ΡΠΈΡΡΠ΅ΠΌΠ°,
ΠΏΡΠ°Π²ΠΎΠ²ΠΎΠ΅ ΡΠ΅Π³ΡΠ»ΠΈΡΠΎΠ²Π°Π½ΠΈΠ΅, ΠΌΠ°Π½ΠΈΠΏΡΠ»ΠΈΡΠΎΠ²Π°Π½ΠΈΠ΅, ΠΎΠΏΠΏΠΎΠ·ΠΈΡΠΈΡ.In this article the basic problems of the legal forestalling of political extremism are examined coming both from domestic and international experience. In research attention is accented on the problems of search of clear political and legal terminology of concept Β«Political
extremismΒ». The author specifies on the necessity of positioning of symbolic and real political
extremism, on importance of differentiation of legal fight against extremism and legal limitation of activity of political opposition.
Key words: political extremism, terrorism, political system, legal adjusting, manipulation,
opposition
A systematic study of the phase difference between QPO harmonics in black hole X-ray binaries
We perform a systematic study of the evolution of the waveform of black hole
X-ray binary low-frequency QPOs, by measuring the phase difference between
their fundamental and harmonic features. This phase difference has been studied
previously for small number of QPO frequencies in individual sources. Here, we
present a sample study spanning fourteen sources and a wide range of QPO
frequencies. With an automated pipeline, we systematically fit power spectra
and calculate phase differences from archival Rossi X-ray Timing Explorer
(RXTE) observations. We measure well-defined phase differences over a large
range of QPO frequencies for most sources, demonstrating that a QPO for a given
source and frequency has a persistent underlying waveform. This confirms the
validity of recently developed spectral-timing methods performing phase
resolved spectroscopy of the QPO. Furthermore, we evaluate the phase difference
as a function of QPO frequency. For Type-B QPOs, we find that the phase
difference stays constant with frequency for most sources. We propose a simple
jet precession model to explain these constant Type-B QPO phase differences.
The phase difference of the Type-C QPO is not constant but systematically
evolves with QPO frequency, with the resulting relation being similar for a
number of high inclination sources, but more variable for low-inclination
sources. We discuss how the evolving phase difference can naturally arise in
the framework of precession models for the Type-C QPO, by considering the
contributions of a direct and reflected component to the QPO waveform
The Link Between Neutron Star X-ray Binaries and Spider Pulsars
The discovery of transitional millisecond pulsars (tMSPs) provided conclusive
proof that neutron star (NS) low-mass X-ray binaries (LMXBs) comprise part of
the evolutionary pathway towards binary millisecond pulsars (MSPs). Redback and
black widow `spider' pulsars are a sub-category of binary MSPs that `devour'
their companions through ablation - the process through which material is
lifted from the stellar surface by a pulsar wind. In addition to reducing the
companion star's mass, ablation introduces observable characteristics like
extended, energy-dependent and asymmetric eclipse profiles in systems observed
at a sufficiently high inclination. Here, we present a detailed study and
comparison of the X-ray eclipses of two NS LMXBs;
J1858.60814 and EXO 0748676. Some of the X-ray eclipse characteristics
observed in these two LMXBs are similar to the radio eclipse characteristics of
eclipsing redback and black widow pulsars, suggesting that they may also host
ablated companion stars. X-ray irradiation or a pulsar wind could drive the
ablation. We conduct orbital phase-resolved spectroscopy for both LMXBs to map
the column density, ionization and covering fraction of the material outflow.
From this, we infer the presence of highly ionized and clumpy ablated material
around the companion star in both systems. We term LMXBs undergoing ablation,
, and speculate that they may be the progenitors of
redback pulsars under the assumption that ablation begins in the LMXB stage.
Therefore, the false widows could provide a link between LMXBs and spider
pulsars. The detection of radio pulsations during non-accreting states can
support this hypothesis.Comment: 21 pages, 15 figures. Accepted for publication in MNRAS. The full
version of Table 1 is available as online supplementary material from the
MNRAS websit
Evidence for a dynamic corona in the short-term time lags of black hole X-ray binary MAXI J1820+070
In X-ray observations of hard state black hole X-ray binaries, rapid
variations in accretion disc and coronal power-law emission are correlated and
show Fourier-frequency-dependent time lags. On short (~0.1 s) time-scales,
these lags are thought to be due to reverberation and therefore may depend
strongly on the geometry of the corona. Low-frequency quasi-periodic
oscillations (QPOs) are variations in X-ray flux that have been suggested to
arise because of geometric changes in the corona, possibly due to General
Relativistic Lense-Thirring precession. Therefore one might expect the
short-term time lags to vary on the QPO time-scale. We performed novel
spectral-timing analyses on NICER observations of the black hole X-ray binary
MAXI J1820+070 during the hard state of its outburst in 2018 to investigate how
the short-term time lags between a disc-dominated and a coronal
power-law-dominated energy band vary on different time-scales. Our method can
distinguish between variability due to the QPO and broadband noise, and we find
a linear correlation between the power-law flux and lag amplitude that is
strongest at the QPO frequency. We also introduce a new method to resolve the
QPO signal and determine the QPO-phase-dependence of the flux and lag
variations, finding that both are very similar. Our results are consistent with
a geometric origin of QPOs, but also provide evidence for a dynamic corona with
a geometry varying in a similar way over a broad range of time-scales, not just
the QPO time-scale.Comment: 19 pages, 14 figures, 3 tables, accepted for publication in MNRA
Probing the origin of quasi-periodic oscillations: the short-time-scale evolution of phase lags in GRS 1915+105
We present a model-independent analysis of the short-timescale energy
dependence of low frequency quasi-periodic oscillations (QPOs) in the X-ray
flux of GRS 1915+105. The QPO frequency in this source has previously been
observed to depend on photon energy, with the frequency increasing with energy
for observations with a high ( Hz) QPO frequency, and decreasing
with energy for observations with a low ( Hz) QPO frequency. As
this observed energy dependence is currently unexplained, we investigate if it
is intrinsic to the QPO mechanism by tracking phase lags on (sub)second
timescales. We find that the phase lag between two broad energy bands
systematically increases for - QPO cycles, after which the QPO becomes
decoherent, the phase lag resets and the pattern repeats. This shows that the
band with the higher QPO frequency is running away from the other band on short
timescales, providing strong evidence that the energy dependence of the QPO
frequency is intrinsic. We also find that the faster the QPO decoheres, the
faster the phase lag increases, suggesting that the intrinsic frequency
difference contributes to the decoherence of the QPO. We interpret our results
within a simple geometric QPO model, where different radii in the inner
accretion flow experience Lense-Thirring precession at different frequencies,
causing the decoherence of the oscillation. By varying the spectral shape of
the inner accretion flow as a function of radius, we are able to qualitatively
explain the energy-dependent behaviour of both QPO frequency and phase lag.Comment: 14 pages, 12 figures, accepted for publication in MNRA
Evidence for a dynamic corona in the short-term time lags of black hole X-ray binary MAXI J1820+070
In X-ray observations of hard state black hole X-ray binaries, rapid variations in accretion disc and coronal power-law emission are correlated and show Fourier-frequency-dependent time lags. On short (~0.1 s) time-scales, these lags are thought to be due to reverberation and therefore may depend strongly on the geometry of the corona. Low-frequency quasi-periodic oscillations (QPOs) are variations in X-ray flux that have been suggested to arise because of geometric changes in the corona, possibly due to General Relativistic Lense-Thirring precession. Therefore one might expect the short-term time lags to vary on the QPO time-scale. We performed novel spectral-timing analyses on NICER observations of the black hole X-ray binary MAXI J1820+070 during the hard state of its outburst in 2018 to investigate how the short-term time lags between a disc-dominated and a coronal power-law-dominated energy band vary on different time-scales. Our method can distinguish between variability due to the QPO and broadband noise, and we find a linear correlation between the power-law flux and lag amplitude that is strongest at the QPO frequency. We also introduce a new method to resolve the QPO signal and determine the QPO-phase-dependence of the flux and lag variations, finding that both are very similar. Our results are consistent with a geometric origin of QPOs, but also provide evidence for a dynamic corona with a geometry varying in a similar way over a broad range of time-scales, not just the QPO time-scale