Understanding the multiwavelength observation of Geminga’s TeV halo: the role of anisotropic diffusion of particles. (arXiv:1904.11536v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Liu_R/0/1/0/all/0/1">Ruo-Yu Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_H/0/1/0/all/0/1">Huirong Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_H/0/1/0/all/0/1">Heshou Zhang</a>
In this letter we demonstrate that the X-ray and the TeV observations in the
vicinity of Geminga can be understood in the framework of anisotropic diffusion
of injected electrons/positrons. This interpretation only requires the
turbulence in the vicinity of Geminga to be sub-Alfv{‘e}nic with the local
mean magnetic field direction approximately aligned with our line of sight
towards Geminga, without invoking extreme conditions for the environment, such
as an extremely small diffusion coefficient and a weak magnetic field of
strength $<1mu$G as suggested in previous literature.
In this letter we demonstrate that the X-ray and the TeV observations in the
vicinity of Geminga can be understood in the framework of anisotropic diffusion
of injected electrons/positrons. This interpretation only requires the
turbulence in the vicinity of Geminga to be sub-Alfv{‘e}nic with the local
mean magnetic field direction approximately aligned with our line of sight
towards Geminga, without invoking extreme conditions for the environment, such
as an extremely small diffusion coefficient and a weak magnetic field of
strength $<1mu$G as suggested in previous literature.
http://arxiv.org/icons/sfx.gif
