title: Ð£ÑÐºÐ¾ÑÐµÐ½Ð¸Ðµ Ð¸ Ð¿ÐµÑÐµÐ½Ð¾Ñ ÑÐµÐ»ÑÑÐ¸Ð²Ð¸ÑÑÑÐºÐ¸Ñ ÑÐ°ÑÑÐ¸Ñ Ð² Ð´Ð²ÑÑ ÑÐ¾ÑÐ¾Ð²Ð¾Ð¹ Ð¿ÑÐ»ÑÑÐ°ÑÐ½Ð¾Ð¹ ÑÑÐ¼Ð°Ð½Ð½Ð¾ÑÑÐ¸
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¼Ð°Ð³Ð¸ÑÑÑÐ°
titleType: Subtitle
title: Acceleration and propagationÂ of nonthermal particles in double-torus pulsar wind nebulae
Creators: name: Ð¤ÑÑÑÐ¾Ð², ÐÐ»ÐµÐºÑÐ°Ð½Ð´Ñ
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2024
Subjects: Ð¢ÑÐ¼Ð°Ð½Ð½Ð¾ÑÑÐ¸

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description: The given work is devoted to the study of the radio disk of double torus pulsar wind nebulae. Observations show that pulsar wind nebulae with double-torus X-ray morphology have a specific radio morphology. Their radio images show two areas of enhanced emission, shaped as two lobes. These radio lobes have a similar orientation compared to the polar axis of the double torus. In the literature on pulsar wind nebulae, the lobes are considered as brightened regions of a thick radio disk surrounding the double-torus and locatedÂ at its equatorial latitudes. The nature of the disk is unknown, as is the origin of the nonthermal particles (electrons and positrons) responsible for the observed radio emission. In this work, we put forwardÂ  a scenario for the formation of a thick radio disk and then test it using numerical simulations.Â The scenario is based on a specific pattern of magnetic outflows, which is characteristic only of double-torus X-ray nebulae. To test the scenario, we injected monoenergetic test-paricles (radio electrons) with random velocity directions into the magnetohydrodynamic (MHD) model of the double-torus X-ray nebula. We then traced the evolution of the spatial and energy distributions of these electrons as they interacted with MHD flows of the model nebula. The simulation confirmed all the points of our scenario, including the main thing: nebulae that tend to create a double X-ray torusÂ also tend to create a thick radio disk around it. The condition for this is the injection of a noticeable population of radio electrons into the weakly magnetized equatorial belt of the double-torus. We emphasize that the need for injection of radio electrons into the equatorial belt does not eliminate the possibility of acceleration of radio electrons at other (non-equatorial) parts of of the windÂ  termination shock or in other parts of the X-ray nebula. However, such electrons, as follows from our simulation, will evelove on their own: they will not be able to get into the equatorial belt andÂ  participate in the creation of the radio disk. They will either be completely lost by the pulsar wind nebula, or noticeably accelerated in the magnetic outflows of the double-torus X-ray structure, causing their synchrÐ¾tron radiation to go beyond the radio band.