16 research outputs found

    ΠŸΡ€Π°Π²ΠΎΠ²Ρ– ΠΏΡ€ΠΎΠ±Π»Π΅ΠΌΠΈ попСрСдТСння ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΎΠ³ΠΎ СкстрСмізму Π² Π£ΠΊΡ€Π°Ρ—Π½Ρ–

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    Π ΠΎΠ·Π³Π»ΡΠ΄Π°ΡŽΡ‚ΡŒΡΡ основні ΠΏΡ€ΠΎΠ±Π»Π΅ΠΌΠΈ ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠ³ΠΎ попСрСдТСння ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΎΠ³ΠΎ СкстрСмізму виходячи як Π· вітчизняного, Ρ‚Π°ΠΊ Ρ– ΠΌΡ–ΠΆΠ½Π°Ρ€ΠΎΠ΄Π½ΠΎΠ³ΠΎ досвіду. Π£ дослідТСнні Π°ΠΊΡ†Π΅Π½- Ρ‚ΡƒΡ”Ρ‚ΡŒΡΡ ΡƒΠ²Π°Π³Π° Π½Π° ΠΏΡ€ΠΎΠ±Π»Π΅ΠΌΠ°Ρ… ΠΏΠΎΡˆΡƒΠΊΡƒ Ρ‡Ρ–Ρ‚ΠΊΠΎΡ— ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΎΡ— Ρ– ΡŽΡ€ΠΈΠ΄ΠΈΡ‡Π½ΠΎΡ— Ρ‚Π΅Ρ€ΠΌΡ–Π½ΠΎΠ»ΠΎΠ³Ρ–Ρ— поняття Β«ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΈΠΉ СкстрСмізм». Автор ΡƒΠΊΠ°Π·ΡƒΡ” Π½Π° Π½Π΅ΠΎΠ±Ρ…Ρ–Π΄Π½Ρ–ΡΡ‚ΡŒ позиціонування символічного Ρ– Ρ€Π΅Π°Π»ΡŒΠ½ΠΎΠ³ΠΎ ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΎΠ³ΠΎ СкстрСмізму, Π½Π° ваТливості Π΄ΠΈΡ„Π΅Ρ€Π΅Π½Ρ†Ρ–Π°Ρ†Ρ–Ρ— ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΡ— Π±ΠΎΡ€ΠΎΡ‚ΡŒΠ±ΠΈ Π· СкстрСмізмом Ρ– ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠ³ΠΎ обмСТСння Π΄Ρ–ΡΠ»ΡŒΠ½ΠΎΡΡ‚Ρ– ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΎΡ— ΠΎΠΏΠΎΠ·ΠΈΡ†Ρ–Ρ—. ΠšΠ»ΡŽΡ‡ΠΎΠ²Ρ– слова: ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½ΠΈΠΉ СкстрСмізм, Ρ‚Π΅Ρ€ΠΎΡ€ΠΈΠ·ΠΌ, ΠΏΠΎΠ»Ρ–Ρ‚ΠΈΡ‡Π½Π° систСма, ΠΏΡ€Π°Π²ΠΎΠ²Π΅ Ρ€Π΅Π³ΡƒΠ»ΡŽΠ²Π°Π½Π½Ρ, ΠΌΠ°Π½Ρ–ΠΏΡƒΠ»ΡŽΠ²Π°Π½Π½Ρ, опозиція.Π Π°ΡΡΠΌΠ°Ρ‚Ρ€ΠΈΠ²Π°ΡŽΡ‚ΡΡ основныС ΠΏΡ€ΠΎΠ±Π»Π΅ΠΌΡ‹ ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠ³ΠΎ упрСТдСния политичСского экстрСмизма исходя ΠΊΠ°ΠΊ ΠΈΠ· отСчСствСнного, Ρ‚Π°ΠΊ ΠΈ ΠΌΠ΅ΠΆΠ΄ΡƒΠ½Π°Ρ€ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΠΎΠΏΡ‹Ρ‚Π°. Π’ исслСдовании акцСнтируСтся Π²Π½ΠΈΠΌΠ°Π½ΠΈΠ΅ Π½Π° ΠΏΡ€ΠΎΠ±Π»Π΅ΠΌΠ°Ρ… поиска Ρ‡Π΅Ρ‚ΠΊΠΎΠΉ политичСской ΠΈ ΡŽΡ€ΠΈΠ΄ΠΈΡ‡Π΅ΡΠΊΠΎΠΉ Ρ‚Π΅Ρ€ΠΌΠΈΠ½ΠΎΠ»ΠΎΠ³ΠΈΠΈ понятия «политичСский экстрСмизм». Автор ΡƒΠΊΠ°Π·Ρ‹Π²Π°Π΅Ρ‚ Π½Π° Π½Π΅ΠΎΠ±Ρ…ΠΎΠ΄ΠΈΠΌΠΎΡΡ‚ΡŒ позиционирования символичСского ΠΈ Ρ€Π΅Π°Π»ΡŒΠ½ΠΎΠ³ΠΎ политичСского экстрСмизма, Π½Π° ваТности Π΄ΠΈΡ„Ρ„Π΅Ρ€Π΅Π½Ρ†ΠΈΠ°Ρ†ΠΈΠΈ ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠΉ Π±ΠΎΡ€ΡŒΠ±Ρ‹ с экстрСмизмом ΠΈ ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠ³ΠΎ ограничСния Π΄Π΅ΡΡ‚Π΅Π»ΡŒΠ½ΠΎΡΡ‚ΠΈ политичСской ΠΎΠΏΠΏΠΎΠ·ΠΈΡ†ΠΈΠΈ. ΠšΠ»ΡŽΡ‡Π΅Π²Ρ‹Π΅ слова: политичСский экстрСмизм, Ρ‚Π΅Ρ€Ρ€ΠΎΡ€ΠΈΠ·ΠΌ, политичСская систСма, ΠΏΡ€Π°Π²ΠΎΠ²ΠΎΠ΅ Ρ€Π΅Π³ΡƒΠ»ΠΈΡ€ΠΎΠ²Π°Π½ΠΈΠ΅, ΠΌΠ°Π½ΠΈΠΏΡƒΠ»ΠΈΡ€ΠΎΠ²Π°Π½ΠΈΠ΅, оппозиция.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

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    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 FalseΒ Widow\textit{False Widow} Link Between Neutron Star X-ray Binaries and Spider Pulsars

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    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; Swift\textit{Swift} J1858.6βˆ’-0814 and EXO 0748βˆ’-676. 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, falseΒ widows\textit{false widows}, 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

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    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

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    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 (≳2\gtrsim 2 Hz) QPO frequency, and decreasing with energy for observations with a low (≲2\lesssim 2 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 55 - 1010 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

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    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
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