Speaker
Description
The search for sources of ultra high energy cosmic rays (UHECR) remains one of the main unsolved problems in modern astrophysics. Galactic magnetars are promising candidates for the UHECR accelerators due to their ability to generate relativistic plasma flows and shock waves during magnetar giant flares. Such energetic processes in plasma also occurs during a Supernova ejecta energisation and a magnetar wind nebulae (MWNe) formation by newborn millisecond magnetars. In both cases, typical signatures of particle acceleration are neutrino and broad-band (from the radio to gamma-ray ) non-thermal emission. This non-thermal emission is either the result of hadronic or leptonic mechanism. In the first case, radiation is the outcome of proton-proton collisions $pp \rightarrow \pi_0 \pi^+ \pi^- + all $, with the subsequent decay of neutral pions into gamma-rays $\pi_0 \rightarrow \gamma \gamma$ and charged pions into neutrinos $\pi^+ \pi^- \rightarrow \nu_{\mu} \nu_{e} + all$. Leptonic emission is the result of synchrotron radiation and energy transfer to background photons from ultrarelativistic electrons (the inverse Compton scattering). In this work we show that high-energy and very high-energy gamma-ray emission from the magnetar SGR1900+14 region can be explained by the acceleration of cosmic rays in the magnetar-connected Supernova remnant and/or MWN. Moreover, detected by Auger and Telescope Array positionally coincident triplet of UHECR with $E>10^{20}$ eV, can be accelerated in giant flare of the SGR1900+14. To achieving necessary energy reserve, the SGR1900+14 progenitor must be the newborn millisecond magnetar with initial rotational energy $E_{rot} \sim 10^{52}$ erg.
Details
Vadym Voitsekhovskyi, PhD student, Kyiv National University, Ukraine
| Is this abstract from experiment? | No |
|---|---|
| Name of experiment and experimental site | N/A |
| Is the speaker for that presentation defined? | Yes |
| Internet talk | Yes |
