 |
RSS feeds |
|
|||||
| Issue 12, 2024 |
|
||||||
|
|
|
||||||
Extracts from the Internet | ||
Resonant event on IceCube1 April 2021The resonant interaction of an electron antineutrino anti-νe with an electron via W−-boson was first registered using the IceCube neutrino telescope [1]. This process is called the Glashow resonance after Glashow who suggested recording muons born in anti-νe + e− → W− → anti-νμ + μ− reaction assuming the mass of a boson – the interaction carrier - to be ≈ 1 GeV [2]. Later, on the basis of the Weinberg-Salam model, which had not yet been experimentally confirmed, V.S. Berezinskii and A.Z. Gazizov formulated a theory of 30– to 100-GeV W− decay in the hadron channel. This process is an analog of the Glashow resonance, but differs from it in the end product. Decays into quark-antiquark pairs with allowance for color were considered. It was shown in [3, 4] that the resonance width and, therefore, the expected number of cascades is much larger than it had been believed before. The resonance peak must be distinguished against the background of nonresonant processes of neutrino scattering by nucleons. V.S. Berezinskii and A.Z. Gazizov proposed to seek a resonant W−-boson in a DUMAND type underwater experiment. At the present time, the IceCube telescope scans a cubic kilometer of Antarctic ice at depths of 1.45–2.45 km. Photomultipliers register Vavilov-Cherenkov radiation generated by secondary charged particles, and machine learning algorithms are used in search for neutrino events. The particle anti-νe induced a cascade of particles with a total measured energy of 6.05 ± 0.72 PeV, which is consistent with the predicted value of 6.32 PeV and is classified with 5σ significance as an astrophysical antineutrino. The event registered with IceCube with allowance for the currently known W−-boson mass agrees with the calculations [3, 4]. High- and superhigh-energy neutrinos might be born in active galactic nuclei [5], in pregalactic stars [6], or be cosmogeneous [7]. Observation of anti-νe limits the models of possible cosmic sources of these particles, since in some models the birth of antineutrinos, unlike neutrinos, is hardly probable. PeV-scale (1015 eV) astrophysical neutrino observation makes it possible to investigate particle interaction at energies now inaccessible on accelerators. For experiments in neutrino astrophysics, see [8-10]. [1] Aartsen M G et al. Nature 591 220 (2021) [2] Glashow S L Phys. Rev. 118 316 (1960) [3] Beresinsky V S, Gazizov A Z Pisma v ZhETF 25 276 (1977) [4] Beresinsky V S, Gazizov A Z Yadernaia fizika 29 1589 (1979); 33 230 (1981) [5] Berezinskii V S, Zatsepin G T Sov. Phys. Usp. 20 361 (1977); UFN 122 3 (1977) [6] Berezinsky V, P. Blasi P Phys. Rev. D 85 123003 (2012) [7] Beresinsky V S, Zatsepin G T Physics Letters B 28 423 (1969) [8] Spiering Ch Phys. Usp. 57 470 (2014); UFN 184 510 (2014) [9] Petrukhin A A Phys. Usp. 58 486 (2015); UFN 185 521 (2015) [10] Dzhilkibaev Ja-A M, Domogatsky G V, Suvorova O V Phys. Usp. 58 495 (2015); UFN 185 531 (2015) Quantum entanglement in a double waveguide1 April 2021E. Borselli (Vienna Center for Quantum Science and Technology, Austria) and their co-authors realized experimentally a new type of quantum entanglement, namely, quantum entanglement of atoms in the state of their motion in double beams [11]. In a transverse direction of a quasi-one-dimensional atomic trap, a potential appeared in the form of two potential wells separated by a barrier. A Bose-Einstein condensate of 600 to 2000 atoms was immersed in this double waveguide. In a pair collision, two excited atoms could acquire oppositely directed momenta along the waveguides and get into one of them. Thus, alternative four atomic states occurred with a possible interference among them. In the experiment, atoms were observed using fluorescence, and their momentum distribution was measured after the trap potential was off. The second-order correlation functions showed the presence of the expected interference pattern. [11] Borselli E et al. Phys. Rev. Lett. 126 083603 (2021) Maxwell’s demon strategy1 April 2021G. Manzano (The International Center for Theoretical Physics (ICTP), Italy and the Institute for Quantum Optics and Quantum Information, Austria) and his co-authors designed a facility, which is functionally close to “Maxwell’s demon”, but follows a given gambling strategy without knowing the particle velocities [12]. The strategy is aimed at obtaining the maximum energy gain while working with a stochastic system during a fixed time interval. The system stops operating either at the instant of time, when a defined gain is reached or goes on operating to the end of the time interval. This conception was experimentally demonstrated in a single-electron quantum well. The mathematical fluctuation relations derived by the authors and characterizing the facility’s operation were confirmed in experiment to an accuracy of ≈ 99.5 %. It has been shown that such a system can operate in a quantum regime, too. This study may appear to be important for constructing microscopic heat engines. [12] Manzano G Phys. Rev. Lett. 126 080603 (2021) A turbulent dynamo in experiment1 April 2021A.F.A. Bott (University of Oxford, United Kingdom and Princeton University, USA) and their co-authors obtained and experimentally studied turbulent plasma with magnetic Prandtle number Pm≥1 and confirmed the magnetic field growth with the help of “fluctuation dynamo” [13]. With fluctuation dynamo, plasma stochastic motions induce extension and summation of magnetic lines of force, which leads to a magnetic field amplification exponential in time. Earlier, laboratory investigations were limited by the regime Pm<1, where the amplification follows another law. Investigation of the case Pm≥1 is important for understanding magnetic field evolution in cosmic objects [14]. High-power laser pulses on the Omega Laser Facility at the University of Rochester evaporated a hydrocarbon foil, and the two plasma beams thus formed collided. Seed magnetic fields were generated by the “Biermann-battery” mechanism and then were amplified by a turbulent dynamo. The plasma’s magnetic field, temperature, density, and velocity were measured with a high time resolution. The magnetic field was increased by three orders of magnitude, the field growth rate exceeding substantially the anticipated one. [13] Bott A F A et al. PNAS 118 e2015729118 (2021) [14] Sokoloff D D, Stepanov R A, Frick P G Phys. Usp. 57 292 (2014); UFN 184 313 (2014) Search for a neutron star in the SN 1987A supernova remnant1 April 2021Upon the SN 1987A supernova explosion, which happened in Large Magellanic Cloud and was observed on the Earth on 23 February 1987, a neutrino flux was observed. This testified to a neutron star birth under the explosion [15]. However, this neutron star has not yet been reliably found hitherto. Only some ambiguous ALMA data on the existence of a compact object were obtained earlier. E. Greco (University of Palermo and Astronomical Laboratory of Palermo, Italy) and their co-authors presented a new convincing evidence of the presence of a neutron star in the supernova remnant [16]. Analysis of the data of Chandra and NuSTAR X-ray telescopes revealed a nonthermal component at 10 to 20 keV corresponding to synchrotron radiation, and magnetohydrodynamic modeling has shown that this component is most likely associated with radiation from the pulsar wind nebula (plerion) surrounding the neutron star, although the model of radiation generation in a shock wave cannot now be completely excluded. For pulsar magnetosphere and accretion to neutron stars, see [17, 18]. [15] Imshennik V S Phys. Usp. 53 1081 (2010); UFN 180 1121 (2010) [16] Greco E et al., arXiv:2101.09029 [astro-ph.HE] [17] Beskin V S Phys. Usp. 61 353 (2018); UFN 188 377 (2018) [18] Shakura N I et al. Phys. Usp. 62 1126 (2019); UFN 189 1202 (2019) |
The Extracts from the Internet is a section of Uspekhi Fizicheskih Nauk (Physics Uspekhi) — the monthly rewiew journal of the current state of the most topical problems in physics and in associated fields. The presented News is devoted to the fundamental discoveries of physics and astrophysics. Permanent editor is Yu.N. Eroshenko. It is compiled from a multitude of Internet sources. | |
|
© 1918–2024 Uspekhi Fizicheskikh Nauk Email: ufn@ufn.ru Editorial office contacts About the journal Terms and conditions |