KONFLIK RUSIA-UKRAINA TAHUN 2014-2022

Konflik Rusia-Ukraina dimulai pada tahun 2014 hingga saat ini. Pada tahun 2014, Rusia berupaya mencaplok wilayah Donbas dan Krimea. Upaya aneksasi Rusia dilakukan melalui serangan siber. Pada tahun 2022 Ukraina akan didukung penuh oleh senjata NATO. Penelitian ini bertujuan untuk menjelaskan mengapa Rusia melanjutkan serangannya dari penggunaan operasi siber hingga penggunaan militer penuh. Peneliti menggunakan analisis perspektif realisme ofensif, teori kekuatan besar dengan konsep “kekuasaan”, untuk mengelola konflik secara transformatif. Temuan dalam penelitian ini adalah upaya penguatan kekuatan militer Rusia juga dipengaruhi oleh kehadiran NATO yang mempunyai kepentingan di Ukraina. Dalam perebutan wilayah pengaruh antara dua aktor adidaya, NATO sebagai kekuatan besar berkepentingan menjadikan Ukraina sebagai benteng militer terdekat untuk membendung pengaruh Rusia di kawasan Balkan. Sebaliknya, Rusia sebagai kekuatan besar di kawasan Balkan berkepentingan menjadikan Ukraina sebagai buffer zone untuk mengantisipasi kemungkinan tekanan terhadap NATO Rusia dalam segala aspek, terutama secara militer

On the Ratio of Periods of the Fundamental Harmonic and First Overtone of Magnetic Tube Kink Oscillations

We study kink oscillations of thin magnetic tubes. We assume that the density inside and outside the tube (and possibly also the cross-section radius) can vary along the tube. This variation is assumed to be of such a form that the kink speed is symmetric with respect to the tube centre and varies monotonically from the tube ends to the tube centre. Then we prove a theorem stating that the ratio of periods of the fundamental mode and first overtone is a monotonically increasing function of the ratio of the kink speed at the tube centre and the tube ends. In particular, it follows from this theorem that the period ratio is lower than two when the kink speed increases from the tube ends to its centre, while it is higher than two when the kink speed decreases from the tube ends to its centre. The first case is typical for non-expanding coronal magnetic loops, and the second for prominence threads. We apply the general results to particular problems. First we consider kink oscillations of coronal magnetic loops. We prove that, under reasonable assumptions, the ratio of the fundamental period to the first overtone is lower than two and decreases when the loop size increases. The second problem concerns kink oscillations of prominence threads. We consider three internal density profiles: generalised parabolic, Gaussian, and Lorentzian. Each of these profiles contain the parameter (Formula presented.) that is responsible for its sharpness. We calculate the dependence of the period ratio on the ratio of the mean to the maximum density. For all considered values of (Formula presented.) we find that a formula relating the period ratio and the ratio of the mean and maximum density suggested by Soler, Goossens, and Ballester (Astron. Astrophys.575, A123, 2015) gives a sufficiently good approximation to the exact dependence

Search for Supersymmetry in pp Collisions at root s=13 TeV in the Single-Lepton Final State Using the Sum of Masses of Large-Radius Jets

Peer reviewe

VizieR Online Data Catalog: HD 284149 SPHERE/IFS spectrum (Bonavita+, 2017)

HD 284149 was observed with SPHERE in IRDIFS mode on 2015-10-25 and with IRDIFS_EXT mode on 2015-11-27 as part of the SHINE (SpHere INfrared survey for Exoplanet) GTO campaign. (1 data file)

The bright optical afterglow of the long GRB 001007

We present optical follow up observations of the long GRB 001007 between 6.14 hours and ~468 days after the event. An unusually bright optical afterglow (OA) was seen to decline following a steep power law decay with index α = -2.03 ± 0.11, possibly indicating a break in the light curve at t - t0 < 3.5 days, as found in other bursts. Upper limits imposed by the LOTIS alerting system 6.14 hours after the gamma ray event provide tentative (1.2σ) evidence for a break in the optical light curve. The spectral index β of the OA yields -1.24 ± 0.57. These values may be explained both by several fireball jet models and by the cannonball model. Fireball spherical expansion models are not favoured. Late epoch deep imaging revealed the presence of a complex host galaxy system, composed of at least two objects located 1.2 arcsec (1.7σ) and 1.9 arcsec (2.7σ) from the afterglow position. Based on observations collected: at the European Southern Observatory, in La Silla and Paranal (Chile), ESO Large Programmes 165.H-0464(G), 165.H-0464(I) and 265.D-5742(A), granted to the GRACE Team; with the Livermore Optical Transient Imaging System's 0.11 m telephoto lenses, at the Lawrence Livermore National Laboratory, in California (USA); with the Instituto de Astrofísica de Canarias's 0.82 m telescope, at the Observatorio del Teide, in the island of Tenerife (Spain); with the Danish 1.54 m telescope, at the European Southern Observatory, in La Silla (Chile); and with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos, of the Instituto de Astrofísica de Canarias

PANTHEON: SCADA for Precision Agriculture

info:eu-repo/semantics/publishe