Fermi-type Particle Acceleration from Magnetic Reconnection at the Termination Shock of a Relativistic Striped Wind
Astrophysical Journal, ISSN: 1538-4357, Vol: 908, Issue: 2
2021
- 11Citations
- 8Captures
Metric Options: Counts1 Year3 YearSelecting the 1-year or 3-year option will change the metrics count to percentiles, illustrating how an article or review compares to other articles or reviews within the selected time period in the same journal. Selecting the 1-year option compares the metrics against other articles/reviews that were also published in the same calendar year. Selecting the 3-year option compares the metrics against other articles/reviews that were also published in the same calendar year plus the two years prior.
Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
Citation Benchmarking is provided by Scopus and SciVal and is different from the metrics context provided by PlumX Metrics.
Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
Citation Benchmarking is provided by Scopus and SciVal and is different from the metrics context provided by PlumX Metrics.
Article Description
An oblique-rotating pulsar generates a relativistic striped wind in a pulsar wind nebula (PWN). The termination shock of the PWN compresses the Poynting-flux-dominated flow and drives magnetic reconnection. By carrying out particle-in-cell simulations of the termination shock of the PWN, we study the shock structure as well as the energy conversion processes and particle acceleration mechanisms. With the recent advances in the numerical methods, we extend the simulations to the ultrarelativistic regime with a bulk Lorentz factor of up to γ 0 = 106. Magnetic reconnection at the termination shock is highly efficient at converting magnetic energy to particle kinetic energy and accelerating particles to high energies. Similar to earlier studies, we find that the resulting energy spectra crucially depend on λ/d e (λ is the wavelength of the striped wind and d e is the relativistic plasma skin depth). When λ/d e is large (λ ⪆ 40d e ), the downstream particle spectra form a power-law distribution in the magnetically dominated relativistic wind regime. By analyzing particle trajectories and statistical quantities relevant to particle energization, we find that Fermi-type mechanism dominates the particle acceleration and power-law formation. We find that the results for particle acceleration are scalable as γ 0 and σ 0 increase to large values. The maximum energy for electrons and positrons can reach hundreds of TeV if the wind has a bulk Lorentz factor of γ 0 ≈ 106 and a magnetization parameter of σ 0 = 10, which can explain the recent observations of high-energy gamma rays from PWNe.
Bibliographic Details
http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=85102708079&origin=inward; http://dx.doi.org/10.3847/1538-4357/abd406; https://iopscience.iop.org/article/10.3847/1538-4357/abd406; https://dx.doi.org/10.3847/1538-4357/abd406; https://validate.perfdrive.com/fb803c746e9148689b3984a31fccd902/?ssa=24151c01-439a-4569-b7bc-80e672d6bed1&ssb=45898272638&ssc=https%3A%2F%2Fiopscience.iop.org%2Farticle%2F10.3847%2F1538-4357%2Fabd406&ssi=5440d9f1-8427-4f52-89ed-3b2a87162d81&ssk=support@shieldsquare.com&ssm=09861369252405940368560762639215174&ssn=fd26b6b7321e822795d8f8ed06ed6c39bf57a8b91149-14d5-48cc-ab0351&sso=e394dfda-70752116f6f660b721a5f21542ad62f8327119ded280913f&ssp=15222386221715427568171581892369563&ssq=40306797935450370570999121678249089743666&ssr=NTIuMy4yMTcuMjU0&sst=com.plumanalytics&ssu=&ssv=&ssw=&ssx=eyJfX3V6bWYiOiI3ZjYwMDBmMjJmYWMwYS02NDkyLTRkODQtYmQ3MS01MTRiMzhlODIwYTcxNzE1NDk5MTIxMzEyMzgwMjMyNzcxLWFlYzVlYmExZDBlM2NiOTYzNjg1NiIsInV6bXgiOiI3ZjkwMDA5ODhhYjdhYS1lNTVlLTQ5MGYtOTFkMS01N2M1NGU3OThkZDY1LTE3MTU0OTkxMjEzMTIzODAyMzI3NzEtMzA0MmM5MjVlZDM1OTk4NTM2ODUzIiwicmQiOiJpb3Aub3JnIn0=
American Astronomical Society
Provide Feedback
Have ideas for a new metric? Would you like to see something else here?Let us know