期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 710, 期 2, 页码 L126-L131出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/710/2/L126
关键词
gamma rays: general; polarization; quasars: individual (PKS 1510-089); radio continuum: galaxies; X-rays: galaxies
资金
- NASA [NNX08AJ64G, NNX08AV65G]
- NSF [AST-0907893, AST-0607523]
- Russian RFBR [09-02-0092]
- Spanish Ministerio de Ciencia e Innovacion [AYA2007-67626-C03-03]
- Academy of Finland
- University of Michigan
- Georgian National Science Foundation [GNSF/ST08/4-404]
- Smithsonian Institution
- Academia Sinica
- UK Science and Technology Facilities Council
- STFC [ST/G009465/1, ST/G003084/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G003084/1, ST/G009465/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0907893] Funding Source: National Science Foundation
We present results from monitoring the multi-waveband flux, linear polarization, and parsec-scale structure of the quasar PKS 1510-089, concentrating on eight major gamma-ray flares that occurred during the interval 2009.0-2009.5. The gamma-ray peaks were essentially simultaneous with maxima at optical wavelengths, although the flux ratio of the two wave bands varied by an order of magnitude. The optical polarization vector rotated by 720 degrees during a five-day period encompassing six of these flares. This culminated in a very bright, similar to 1 day, optical and gamma-ray flare as a bright knot of emission passed through the highest-intensity, stationary feature (the core) seen in 43 GHz Very Long Baseline Array images. The knot continued to propagate down the jet at an apparent speed of 22c and emit strongly at gamma-ray energies as a months-long X-ray/radio outburst intensified. We interpret these events as the result of the knot following a spiral path through a mainly toroidal magnetic field pattern in the acceleration and collimation zone of the jet, after which it passes through a standing shock in the 43 GHz core and then continues downstream. In this picture, the rapid gamma-ray flares result from scattering of infrared seed photons from a relatively slow sheath of the jet as well as from optical synchrotron radiation in the faster spine. The 2006-2009.7 radio and X-ray flux variations are correlated at very high significance; we conclude that the X-rays are mainly from inverse Compton scattering of infrared seed photons by 20-40 MeV electrons.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据