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The predicted anisotropy depends on the cosmic-ray energy, pitch angle, and spatial dependence in the LISM, including contributions from young nearby sources. Mapping through magnetohydrodynamic heliosphere fields distorts large-scale dipolar and bidirectional patterns into many small observational structures, enabling estimates of density-gradient and pitch-angle anisotropies. The heliotail and related geometric regions dominate distortions, allowing inference of the LISM magnetic-field direction and polarity, while solar-cycle, coronal-field, and turbulence effects are minor and visible.",{"@graph":69,"@context":123},[70,84,106],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":40,"@type":76,"position":81},"https://docshare.wps.com/document/research-report/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/heliospheric-influence-on-the-anisotropy-of-tev-cosmic-rays/149052/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/heliospheric-influence-on-the-anisotropy-of-tev-cosmic-rays/149052.png","ImageObject",300,407,{"name":92,"@type":93},"Oliver Hayes","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-29","2026-08-27",true,{"@type":102,"interactionType":103,"userInteractionCount":105},"InteractionCounter",{"@type":104},"ViewAction",12,{"@type":107,"mainEntity":108},"FAQPage",[109,115,119],{"name":110,"@type":111,"acceptedAnswer":112},"这篇论文的核心方法是什么？","Question",{"text":113,"@type":114},"论文用 Liouville’s theorem 将 LISM 中粒子分布函数的各向异性映射到地球可观测的各向异性，并强调能量与螺距角等参数对结果的决定作用。","Answer",{"name":116,"@type":111,"acceptedAnswer":117},"各向异性受到哪些物理因素的影响？",{"text":118,"@type":114},"各向异性取决于 TeV 宇宙线在 LISM 中的能量、pitch angle 以及空间依赖，并且受年轻邻近源的年龄、距离和磁连接方式、扩散过程影响。",{"name":120,"@type":111,"acceptedAnswer":121},"太阳风/日球层的作用对观测会产生什么特征？",{"text":122,"@type":114},"通过磁流体模型的日球层磁场与电场映射，原本的大的尺度偶极与双向各向异性会被扭曲，形成观测中的许多小尺度结构；其中 heliotail、氢偏转平面及垂直于 LISM 磁场的平面尤其关键。","https://schema.org",{"og:url":83,"og:type":125,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":127,"canonical":83},"index,follow",{"doc_id":129,"site_id":62},149052,1787790779,{"code":4,"msg":5,"data":132},{"doc_id":129,"user_id":133,"nickname":92,"user_avatar":134,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":135,"file_id":136,"file_url":137,"file_type":138,"file_size":139,"view_count":105,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":140,"language":141,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":142,"faqs":143,"seo_title":144,"seo_description":67,"update_tm":130,"read_time":145,"preview_page_count":4},687207020761,"https://ap-avatar.wpscdn.com/davatar_155a257f0dc6eb9ab79c44ca47cae57d","The Astrophysical Journal, 790:5 (17pp), 2014 July 20 doi:10.1088/0004-637X/790/1/5  \n 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A.  \nHELIOSPHERIC INFLUENCE ON THE ANISOTROPY OF TeV COSMIC RAYS  \nMing Zhang 1 , Pingbing Zuo 1 , and Nikolai Pogorelov2  \n1 Department of Physics and Space Sciences, Florida Institute of Technology, Melbourne, FL 32901, USA; mzhang@fi[t.edu](t.edu)  \n2 Center for Space Plasma and Aeronomic Research and Department of Space Science, University of Alabama in Huntsville, AL 35899, USA  \nReceived 2014 April 9; accepted 2014 May 28; published 2014 June 26  \nABSTRACT  \nThis paper provides a theory of using Liouville’s theorem to map the anisotropy of TeV cosmic rays seen at Earth using the particle distribution function in the local interstellar medium (LISM) . The ultimate source of cosmic ray anisotropy is the energy, pitch angle, and spatial dependence of the cosmic ray distribution function in the LISM. Because young nearby cosmic ray sources can make a special contribution to the cosmic ray anisotropy, the anisotropy depends on the source age, distance and magnetic connection, and particle diffusion of these cosmic rays, all of which make the anisotropy sensitive to the particle energy. When mapped through the magnetic and electric field of a magnetohydrodynamic model heliosphere, the large-scale dipolar and bidirectional interstellar anisotropy patterns become distorted if they are seen from Earth, resulting in many small structures in the observations. Best fits to cosmic ray anisotropy measurements have allowed us to estimate the particle density gradient and pitch angle anisotropies in the LISM. It is found that the heliotail, hydrogen deflection plane, and the plane perpendicular to the LISM magnetic field play a special role in distorting cosmic ray anisotropy. These features can lead to an accurate determination of the LISM magnetic field direction and polarity. The effects of solar cycle variation, the Sun’s coronal magnetic field, and turbulence in the LISM and heliospheric magnetic fields are minor but clearly visible ata level roughly equal to a fraction of the overall anisotropy amplitude. The heliospheric influence becomes stronger at lower energies. Below 1 TeV, the anisotropy is dominated by small-scale patterns produced by disturbances in the heliosphere.  \nKey words: cosmic rays – ISM: magnetic fields – Sun: heliosphere  \nOnline-only material: color figures  \n1. INTRODUCTION  \nRecently, a great wealth of information about the directional variation (which is commonly referred to as anisotropy) in the flux of cosmic rays arriving at Earth in the TeV to PeV energy range has been obtained by quite a number of air shower experiments. Among those that have achieved excellent data quality with large event statistics are Tibet (Amenomori et al. 2006, 2010) Milagro (Abdo et al. 2008, 2009), SuperKamiokande (Guilian et al. 2007), IceCube/EAS-Top (Abbasi et al. 2010, 2011, 2012), and ARGO-YGB (Di Sciascio et al. 2012) . The observational results are quite surprising and, to some extent, confusing. Although there is a general large-scale anisotropy pattern with an amplitude of the order of 10−3 , the data do not seem to fit any standard diffusion model of cosmic ray propagation through the interstellar medium with atypical magnetic field ofa fewμG and a large isotropic diffusion coefficient of ∼1028 cm2 s−1 . The Compton–Getting effect due to the motion of the heliosphere relative to the local interstellar medium (LISM) is almost completely invisible. The phase of the large-scale anisotropy pattern shifts between 20 TeV and 400 TeV (Abbasi et al. 2012), which has clearly ruled out the theory that the Compton–Getting effect is a major source of the anisotropy. A more surprising feature is that there is clear evidence for small-scale structures of tens of degrees in angular size in the anisotropy data. Small regions of enhanced cosmic ray flux are called hot spots in some re","cbCaik7CJGEeZzJ4","https://ap.wps.com/l/cbCaik7CJGEeZzJ4","pdf",5013858,17,"English","# Abstract\n# Introduction","[{\"question\":\"这篇论文的核心方法是什么？\",\"answer\":\"论文用 Liouville’s theorem 将 LISM 中粒子分布函数的各向异性映射到地球可观测的各向异性，并强调能量与螺距角等参数对结果的决定作用。\"},{\"question\":\"各向异性受到哪些物理因素的影响？\",\"answer\":\"各向异性取决于 TeV 宇宙线在 LISM 中的能量、pitch angle 以及空间依赖，并且受年轻邻近源的年龄、距离和磁连接方式、扩散过程影响。\"},{\"question\":\"太阳风/日球层的作用对观测会产生什么特征？\",\"answer\":\"通过磁流体模型的日球层磁场与电场映射，原本的大的尺度偶极与双向各向异性会被扭曲，形成观测中的许多小尺度结构；其中 heliotail、氢偏转平面及垂直于 LISM 磁场的平面尤其关键。\"}]","HELIOSPHERIC INFLUENCE ON THE ANISOTROPY OF TeV COSMIC RAYS | PDF",43]