BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Anisotropy in the TeV Cosmic Rays: A Challenge for Interpretation DTSTART:20111028T210000Z DTEND:20111028T211500Z DTSTAMP:20260610T034300Z UID:indico-contribution-2363@events.icecube.wisc.edu DESCRIPTION:Speakers: Segev BenZvi (University of Wisconsin-Madison)\n\nTo measure the per-mille anisotropy in the TeV cosmic rays with a\nground-ba sed experiment\, it is necessary to estimate the exposure of the\ndetector to cosmic ray air showers. The estimate must account for drifts\nthat oc cur in the detector during the course of the measurement\, as well\nas cha nges in the shower signal at ground level caused by atmospheric\ncondition s. Due to the difficulty of the exposure calculation\, all\nexperiments f ollow a similar procedure in which the exposure is calculated\nin small ti me steps using real events. Using this method\, the exposure\ncan be esti mated with sufficient accuracy to measure per-mille effects in\nthe data. However\, calculating the exposure using the data themselves\nalso introd uces significant and surprising artifacts into the resulting\nsky maps. U sing simulated events\, we will demonstrate the difficulty of\ninterpretin g the cosmic ray anisotropy in light of these artifacts.\n\nhttps://events .icecube.wisc.edu/event/39/contributions/2363/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2363/ END:VEVENT BEGIN:VEVENT SUMMARY:An explanation for the cosmic ray anisotropies at multiple scales DTSTART:20111028T221000Z DTEND:20111028T223000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2364@events.icecube.wisc.edu DESCRIPTION:Speakers: Gwenael Giacinti (NTNU Trondheim and APC Paris)\n\nW e propose an explanation for the origin of the observed cosmic ray anisotr opies at multiple scales. We discuss its implications\, and future perspec tives.\n\nhttps://events.icecube.wisc.edu/event/39/contributions/2364/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2364/ END:VEVENT BEGIN:VEVENT SUMMARY:Acceleration of cosmic ray by reconnection in realistically turbul ent environments DTSTART:20111028T162000Z DTEND:20111028T164000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2365@events.icecube.wisc.edu DESCRIPTION:Speakers: Alex Lazarian (UW-)\n\nMagnetic reconnection in real istically turbulent astrophysical environments does not depend on electric conductivity of plasma\, but instead is controlled by the degree of turbu lent stochasticity of magnetic field lines. Such a reconnection can induce the first order Fermi acceleration of energetic particles. I will show th at this acceleration is different in 2D and 3D reconnection with 3D reconn ection being more efficient in the particle acceleration. I shall discuss the importance of plasma effect both for magnetic reconnection and for par ticle acceleration.\n\nhttps://events.icecube.wisc.edu/event/39/contributi ons/2365/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2365/ END:VEVENT BEGIN:VEVENT SUMMARY:The origin of the cosmic ray positron/electron excess and beyond DTSTART:20111028T224000Z DTEND:20111028T230000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2366@events.icecube.wisc.edu DESCRIPTION:Speakers: Hasan Yuksel (LANL)\n\nThe spectra of cosmic electro ns and positrons should have contributions from known sources such as part icles accelerated in supernova remnants and from interactions of cosmic an d interstellar protons. Any evidence for an additional component\, as rep orted by PAMELA\, Fermi and HESS experiments\, may carry hints of a new ph enomenon. I will examine the implications of the recent detection of exte nded\, multi-TeV gamma-ray emission from Geminga pulsar wind nebula by Mil agro experiment\, which reveals the existence of an ancient/nearby cosmic ray accelerator that can also plausibly account for all these observations .\n\nhttps://events.icecube.wisc.edu/event/39/contributions/2366/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2366/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray anisotropy from AMANDAs point of view DTSTART:20111028T193000Z DTEND:20111028T195000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2367@events.icecube.wisc.edu DESCRIPTION:Speakers: Maria Gurtner (University of Wuppertal)\n\nThe AMAND A detector has been operated at the South Pole until 2006 and recorded a t otal ~9·10^9 muons above ~1 TeV between 2000 and 2006. With a data set o f this size\, it is possible to probe the southern sky for per-mil anisotr opy on all angular scales in the arrival direction distribution of cosmic rays thereby extending anisotropy measurements performed with IceCube. \nT he data presented here were collected with the AMANDA MuonDAQ. Great care has been taken to apply proper data selection cuts and to account for temp oral instabilities during data taking. We shall describe the analysis incl uding corrections for spatial asymmetries of the detector and for down tim es of data taking. For each single year we find asymmetries in the distrib ution of right ascension with amplitudes of about 5x10-4 and phases around 50 degree\, well in agreement with earlier results from IceCube. No signi ficant long term variation is found in the data.\n\nhttps://events.icecube .wisc.edu/event/39/contributions/2367/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2367/ END:VEVENT BEGIN:VEVENT SUMMARY:The Elemental Composition of Galactic Cosmic Rays DTSTART:20111029T170000Z DTEND:20111029T172000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2368@events.icecube.wisc.edu DESCRIPTION:Speakers: Jörg Hörandel (Radboud University Nijmegen)\n\nOne of the key observables to understand the origin and the sources of Galact ic cosmic rays is their elemental composition. The abundance of elements i s measured directly with detectors above the atmosphere on balloons and sa tellites. At energies exceeding 10^14 eV information on the composition is derived from the observation of extensive air showers. Results of recent measurements will be reviewed and the implications on our current understa nding of the origin of Galactic cosmic rays will be discussed.\n\nhttps:// events.icecube.wisc.edu/event/39/contributions/2368/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2368/ END:VEVENT BEGIN:VEVENT SUMMARY:Trying to Understand the Interstellar Transport and Resulting Anis otropies of Galactic Cosmic Rays DTSTART:20111028T172000Z DTEND:20111028T174000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2369@events.icecube.wisc.edu DESCRIPTION:Speakers: J.R. (Randy) Jokipii (University of Arizona)\n\nThe observed interstellar anisotropies of galactic cosmic rays\, and \ntheir e nergy dependence\, are a major source of information concerning \ntheir or igin and transport in the galaxy. They also present significant \nchalleng es to our understanding. I will discuss possible \ninterpretations of som e of the anisotropies in terms of interstellar \ntransport in the interste llar magnetic field and some of the resulting \nimplications for our under standing of interstellar turbulence.\n\nhttps://events.icecube.wisc.edu/ev ent/39/contributions/2369/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2369/ END:VEVENT BEGIN:VEVENT SUMMARY:Introduction DTSTART:20111028T134500Z DTEND:20111028T140000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2370@events.icecube.wisc.edu DESCRIPTION:Speakers: Paolo Desiati (UW-Madison)\n\nhttps://events.icecube .wisc.edu/event/39/contributions/2370/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2370/ END:VEVENT BEGIN:VEVENT SUMMARY:A needlet-based approach to directional data analysis DTSTART:20111028T203000Z DTEND:20111028T205000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2371@events.icecube.wisc.edu DESCRIPTION:Speakers: Roberto Iuppa (INFN\, Roma 2)\n\nEAS array dataset c ontains signal laying on different angular\nscales: point-like and extende d gamma-ray sources\, as well as large and\nintermediate scale cosmic-ray anisotropies. The separation of all these\ncontributions is crucial\, most ly when they overlap with each other.\nIn recent years\, the needlet trans form has proved to be an effective tool\nin the analysis of cosmological a nd astrophysical data\, because of the\neasiness of implementation and the remarkable double-localization\nproperties (in real and harmonic domain). Nevertheless\, it has been never\nused in cosmic-ray and very high energy gamma-ray physics so far.\nHere the results of the application of this te chnique to the whole\nARGO-YBJ dataset are presented\, pointing out the ad vantages of this new\napproach\nwith respect to the standard methods of an alysis employed in astroparticle\nphysics.\n\nhttps://events.icecube.wisc. edu/event/39/contributions/2371/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2371/ END:VEVENT BEGIN:VEVENT SUMMARY:Direction of the Interstellar Magnetic Field in the Solar Vicinity DTSTART:20111029T213000Z DTEND:20111029T215000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2389@events.icecube.wisc.edu DESCRIPTION:Speakers: Priscilla Frisch (University of Chicago)\n\nSimilar directions are obtained for the local interstellar magnetic\nfield (ISMF) by comparing diverse data that sample five orders of\nmagnetic in spatial scales. The direction of the ISMF that shapes the\nheliosphere\, and that is traced by the ribbon of energetic neutral\natoms discovered by the Int erstellar Boundary Explorer (IBEX) mission\,\nis compared to the ISMF dire ction obtained from linearly polarized\nlight from nearby stars\, the ISMF of the Loop I superbubble that has\nexpanded to the solar vicinity\, and the ISMF direction towards pulsars\nwithin 100-300 pc. Together these dat a suggest that the local ISMF\ndirection is correlated over spatial scales of about 100 pc\, such as\nwould be expected for the interarm region of t he galaxy.\n\nhttps://events.icecube.wisc.edu/event/39/contributions/2389/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2389/ END:VEVENT BEGIN:VEVENT SUMMARY:Angular distribution of energetic particles scattered by strongly anisotropic MHD turbulence: understanding Milagro/IceCube results DTSTART:20111028T165000Z DTEND:20111028T171000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2372@events.icecube.wisc.edu DESCRIPTION:Speakers: Mikhail Malkov (University of California\, San Diego )\n\nBoth the acceleration of cosmic rays (CR) in supernova remnant shocks \nand their subsequent propagation through the random magnetic field\nof t he Galaxy deem to result in an almost isotropic CR spectrum. Yet\nthe MILA GRO TeV observatory and the IceCube discovered sharp\n(~10 deg)\narrival a nisotropies of CR nuclei. We suggest a mechanism for producing\nsuch a CR beam which operates en route to the observer. The key assumption\nis that CRs are scattered by a strongly anisotropic Alfven wave spectrum\nformed b y the turbulent cascade across the local field direction.\nThe strongest p itch-angle scattering occurs for particles moving almost\nprecisely along the field line. Partly because this direction is also\nthe direction of mi nimum of the large scale CR angular distribution\,\nthe enhanced scatterin g results in a weak but narrow particle excess.\nThe width\, the fractiona l excess and the maximum momentum of the beam\nare calculated from a syste matic transport theory depending on a single\nscale l which can be associa ted with the longest Alfven wave\,\nefficiently\nscattering the beam. The best match to all the three characteristics\nof the beam is achieved at l~ 1 pc. The distance to a possible\nsource of the beam is estimated to be wi thin a few 100pc. Possible\napproaches to determination of the scale l fro m the characteristics\nof the source are discussed. The beam related\nlarg e scale anisotropic CR component is found to be energy independent\nwhich is also consistent with the observations. The beam splitting\nmechanism to explain the combined Milagro and IceCube observations is\nsuggested.\n\nh ttps://events.icecube.wisc.edu/event/39/contributions/2372/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2372/ END:VEVENT BEGIN:VEVENT SUMMARY:Interaction of the solar wind with the interstellar medium: struct ure and implications for galactic cosmic rays DTSTART:20111029T150000Z DTEND:20111029T152000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2373@events.icecube.wisc.edu DESCRIPTION:Speakers: Gary Zank (University of Alabama in Huntsville)\n\nT he solar wind interacts with the local interstellar medium via both\nioniz ed and neutral gases. The primary coupling mechanism\, charge\nexchange be tween protons and interstellar hydrogen\, plays a critical\nrole in determ ining the local structure\, as does the interstellar\nmagnetic field. We w ill describe the basic physical processes\nunderlying the interaction betw een the solar wind and local\ninterstellar medium\, discuss the overall st ructure itself\, with\nparticular emphasis on magnetic structures in the i nner heliosheath\,\nthe heliotail\, and associated turbulence. We will als o illustrate how\nIBEX measurements yield an estimate of the strength and orientation of\nthe local interstellar magnetic field. Finally\, we will i llustrate the\neffect of heliospheric boundaries and structure on the entr ance of\ngalactic cosmic rays into the heliosphere.\n\nhttps://events.icec ube.wisc.edu/event/39/contributions/2373/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2373/ END:VEVENT BEGIN:VEVENT SUMMARY:TeV and PeV CR anisotropy as observed with IceCube and IceTop DTSTART:20111028T153000Z DTEND:20111028T155000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2374@events.icecube.wisc.edu DESCRIPTION:Speakers: Marcos Santander (University of Wisconsin-Madison)\n \nThe IceCube Neutrino Observatory\, located at the geographic South Pole\ , employs a km3 of Antarctic ice as a particle detector to search for sour ces of astrophysical neutrinos across the southern sky. The high rate of C R events in the detector has allowed to search for anisotropy in this data sample at the per-mille level. I'll report on the observation of CR aniso tropy in the 20 TeV to 1 PeV range observed across a wide range of angular scales.\nThe IceTop air shower array\, sitting on top of the IceCube dete ctor on the ice surface\, has also observed an anisotropy in the PeV range that is compatible with that observed with the in-ice detector.\n\nhttps: //events.icecube.wisc.edu/event/39/contributions/2374/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2374/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Anisotropy at TeV energies with ARGO-YBJ DTSTART:20111028T150000Z DTEND:20111028T152000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2375@events.icecube.wisc.edu DESCRIPTION:Speakers: Roberto Iuppa (INFN\, Roma 2)\, Giuseppe Di Sciascio (INFN\, Roma 2)\n\nThe ARGO-YBJ experiment\, located at the Yangbajing Co smic Ray Laboratory\n(Tibet\, 4300 m asl\, 606 g/cm2)\, is an EAS-array ex ploiting the full\ncoverage approach at high altitude. We analyzed the dat a taken since\nNovember 2007 looking for anisotropies in the arrival direc tions of\ncosmic rays on different angular scales. The results of the anal ysis are\nreported and compared with other experiments.\n\nhttps://events. icecube.wisc.edu/event/39/contributions/2375/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2375/ END:VEVENT BEGIN:VEVENT SUMMARY:The small-scale anisotropy of the cosmic radiation: results from M ilagro DTSTART:20111028T140000Z DTEND:20111028T142000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2376@events.icecube.wisc.edu DESCRIPTION:Speakers: John Pretz (LANL)\n\nThe presence of a large-scale a nisotropy in the cosmic radiation has been known for several decades. Ear lier experiments lacked the statistical power to observe small-scale aniso tropies in the cosmic radiation and there were good reasons to expect that on small scales the cosmic radiation would be smooth. The Milagro extens ive air shower array discovered the presence of at least two small (of ord er 5-10 degrees) regions with significant excess (with respect to the expe ctations from the large-scale anisotropy) in the cosmic radiation near 10 TeV. The observed fractional excess is roughly 5x10$^{-4}$ - about one or der of magnitude smaller than the large-scale anisotropy. Because the Lar mor radius of a 10 TeV proton is 0.005 pc explanations of these observatio ns are difficult\, however they seem to imply a relatively nearby source a nd non-standard diffusion of cosmic rays in the solar neighborhood. In th is talk I will discuss the results from Milagro and several potential expl anations of these observations.\n\nhttps://events.icecube.wisc.edu/event/3 9/contributions/2376/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2376/ END:VEVENT BEGIN:VEVENT SUMMARY:Features in cosmic-ray elemental spectra DTSTART:20111029T160000Z DTEND:20111029T162000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2377@events.icecube.wisc.edu DESCRIPTION:Speakers: Eun-Suk Seo (University of Maryland)\n\nAdditional i nformation: http://iopscience.iop.org/2041-8205/714/1/L89/\n\nhttps://even ts.icecube.wisc.edu/event/39/contributions/2377/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2377/ END:VEVENT BEGIN:VEVENT SUMMARY:The cosmic ray anisotropy measured by the ARGO-YBJ experiment and the status of the LHASSO project DTSTART:20111028T143000Z DTEND:20111028T145000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2378@events.icecube.wisc.edu DESCRIPTION:Speakers: Songzhan Chen (Institute of High Energy Physics (IHE P))\n\nThe ARGO-YBJ experiment is located at Yang Ba Jing (P.R. China)\, a t 4300 m a.s.l. and atmospheric depth of 606 g/cm^2. It is an air shower d etector array with a fully covered layer of Resistive Plate Chambers. It i s designed to detect EAS in the primary energy range between few hundred G eV and a few PeV. It has been continuously operated with a duty cycle abov e 86% since November 2007 observing about 4x10^11 air showers. With such u nprecedented statistics\, it is very suitable for the study of anisotropy. Here we will report its result for cosmic ray anisotropy. \nThe LHASSO p roject is designed for greatly boost the capability of current YBJ observa tory with a large complex air shower detector array in an area of 1km^2. H ybrid detection with multi-techniques will allow a good discrimination bet ween different types of primary particles. Here we will report its status and future capabilities for the anisotropy studies.\n\nhttps://events.icec ube.wisc.edu/event/39/contributions/2378/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2378/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-Ray Measurements with the PAMELA Experiment DTSTART:20111029T163000Z DTEND:20111029T165000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2379@events.icecube.wisc.edu DESCRIPTION:Speakers: Mirko Boezio (INFN Trieste)\n\nAfter five years of d ata taking in space\, the PAMELA experiment has presented new results on t he energy spectra of protons\, helium nuclei\, electrons and positrons tha t might change our current understanding of the mechanisms of production\, acceleration and propagation of cosmic rays in the Galaxy. In addition\, PAMELA measurements of cosmic antiproton and positron fluxes are setting s trong constraints to the nature of Dark Matter. PAMELA is also searching f or primordial antinuclei (anti-helium) and studying the acceleration and p ropagation models through precision studies of light nuclei and their isot opes. This talk illustrates the most recent scientific results obtained by the PAMELA experiment.\n\nhttps://events.icecube.wisc.edu/event/39/contri butions/2379/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2379/ END:VEVENT BEGIN:VEVENT SUMMARY:The Anisotropy of TeV Cosmic Rays: an interpretation DTSTART:20111029T220000Z DTEND:20111029T221500Z DTSTAMP:20260610T034300Z UID:indico-contribution-2382@events.icecube.wisc.edu DESCRIPTION:Speakers: Rasha Abbasi (University of Wisconsin-Madison)\, Arn old Wolfendale (Durham University)\, Anatoliy Erlykin (Lebedev Institute\, Moscow\, Russia)\n\nThe history of anisotropy measurements has a long his tory and some attempts at interpretations have already been made. \n The early measurements are important in view of giving a check on the validity of the contemporary exciting measurements. So far they seem to confirm an d complement them\, at least for the large scale anisotropies.\n The smal l scale anisotropies\, forming 'striations' perpendicular to the Ecliptic Plane\, pose a challenge and may indicate new features of the Local Inters tellar Medium.\n An attempt will be made to give an explanation of the fe atures and predictions will be given as to what to expect next.\n\nhttps:/ /events.icecube.wisc.edu/event/39/contributions/2382/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2382/ END:VEVENT BEGIN:VEVENT SUMMARY:A measurement of the cosmic ray anisotropy at and above 10^14 eV DTSTART:20111028T200000Z DTEND:20111028T202000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2383@events.icecube.wisc.edu DESCRIPTION:Speakers: Piera Luisa Ghia (LPNHE (CNRS))\n\nThe EAS-TOP Exten sive Air Shower array was located at Campo Imperatore (2005 m a.s.l.\, lat itude 42◦27N\, longitude 13◦34E\, INFN Gran Sasso National Laboratory) . It took cosmic ray data in the energy range 10^13 eV-10^16 eV from the e nd of 1980s up to 2000. A first data-set (including 4 years of data) was e xploited for the measurement of the cosmic ray anisotropy at E≈10^14 eV (Ap. J. 470\, 1996\, 501). At this energy\, the EAS-TOP results demonstrat ed that the main features of the anisotropy (i.e.\, of cosmic-ray propagat ion) are similar to those measured at lower energies (10^11–10^14 eV)\, both with respect to amplitude ((3–6) ~ 10^−4) and phase ((0–4) hr l ocal sidereal time (LST)). Thanks to the final data-set (spanning over 8 y ears) the EAS-TOP measurement could be extended to higher energy\, about 4 x10^14 eV. The observed anisotropy shows an amplitude larger than at 10^14 eV and a different phase (ApjL 692\, 2009\, 130). Different checks of sta bility of the detector and consistency of the data are presented. The sign ificance of the observation for the understanding of cosmic-ray propagatio n is discussed.\n\nhttps://events.icecube.wisc.edu/event/39/contributions/ 2383/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2383/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar Wind Interaction with the Local Interstellar Medium: Heliosh eath and Heliotail Flows DTSTART:20111029T210000Z DTEND:20111029T212000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2384@events.icecube.wisc.edu DESCRIPTION:Speakers: Nikolai Pogorelov (University of Alabama in Huntsvil le)\n\nThe Sun moves through the local interstellar medium (LISM) ejecting charged particles with velocities that eventually become greater\nthan th e fast magnetosonic velocity. A surface separating the LISM material from the solar wind (SW) plasma is called\nthe heliopause. The SW is decelerate d by the heliopause creating a heliospheric termination shock. A region of the\nSW plasma between the termination shock and the head of the heliopau se is called the inner heliosheath (IHS). The LISM plasma is also decelera ted by the heliopause creating a so-called outer heliosheath (OHS). The ta il of the SW-LISM interaction region can be very long\,\nextending to a fe w thousand astronomical units (AU). The LISM being partially ionized (abou t three times more neutral atoms than ions)\, \ncharge exchange plays a ma jor role in the heliospheric structure. I will describe the differences be tween purely MHD and\nMHD-neutral scenarios for different orientations and strengths of the interstellar magnetic field. The constraints on the\nLIS M properties derived from the Interstellar Boundary Explorer will be discu ssed. The peculiarities of the SW plasma flow\nin the heliotail will be an alyzed in the framework of a realistic model that takes into account solar cycle effects.\n\nhttps://events.icecube.wisc.edu/event/39/contributions/ 2384/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2384/ END:VEVENT BEGIN:VEVENT SUMMARY:Searches for Cosmic Ray Electron Anisotropies with the Fermi Large Area Telescope DTSTART:20111029T140000Z DTEND:20111029T142000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2385@events.icecube.wisc.edu DESCRIPTION:Speakers: Vlasios Vasileiou (Laboratoire Univers et Particules de Montpellier)\n\nThe Large Area Telescope on board the Fermi satellite detected more than 1.6 million cosmic-ray electrons/positrons with energie s above 60 GeV during its first year of operation. The arrival directions of these events were searched for anisotropies of angular scales from ~10d eg up to 90deg\, and of minimum energy extending from 60GeV up to 480GeV. Two independent techniques were used to search for anisotropies\, both res ulting in no detections. Upper limits on the anisotropy level for differen t energy ranges and angular scales were set. The analysis methods and the implications of the upper limits on the existence of nearby CRE sources an d on some classes of dark matter models will be discussed.\n\nhttps://even ts.icecube.wisc.edu/event/39/contributions/2385/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2385/ END:VEVENT BEGIN:VEVENT SUMMARY:Large scale distribution of arrival directions of cosmic rays abov e ~100 PeV DTSTART:20111028T214000Z DTEND:20111028T220000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2386@events.icecube.wisc.edu DESCRIPTION:Speakers: Olivier Deligny (Institut de Physique Nucléaire Ors ay)\n\nScrutiny of the large scale distribution of arrival directions of c osmic\nrays with energies above ~100 PeV is one important observable to pr ovide\nkey elements for understanding the end of Galactic cosmic rays\, an d for\nestablishing at which energy the flux of extragalactic cosmic rays starts\nto dominate the cosmic ray energy spectrum. Using the large amount of\ndata collected by the Pierre Auger Observatory\, upper limits on the\ ndipole component in the equatorial plane obtained in different energy\nra nges above ~100 PeV are presented\, being below 2% at 99% CL for EeV\nener gies. Even though the measured amplitudes are within the statistical\nfluc tuations\, an apparent consistency of the phases in adjacent energy\nbins is observed and discussed.\n\nhttps://events.icecube.wisc.edu/event/39/con tributions/2386/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2386/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Anisotropies DTSTART:20111029T173000Z DTEND:20111029T175000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2387@events.icecube.wisc.edu DESCRIPTION:Speakers: Pasquale Blasi (INAF/Osservatorio Astrofisico di Arc etri)\n\nI will discuss the role of anisotropy as a tool to discriminate a mong different scenarios for the origin of Galactic cosmic rays. The main aim of the presentation is that of stressing the need for a unified pictur e of acceleration\, propagation\, chemical composition and anisotropy. I w ill summarize the different contributions to cosmic ray anisotropies and t he problems with current observations\, especially with anisotropy on smal l angular scales.\n\nhttps://events.icecube.wisc.edu/event/39/contribution s/2387/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2387/ END:VEVENT BEGIN:VEVENT SUMMARY:GALPROP Code for Galactic Cosmic Ray Propagation and Associated Ph oton Emissions DTSTART:20111029T143000Z DTEND:20111029T145000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2388@events.icecube.wisc.edu DESCRIPTION:Speakers: Igor Moskalenko (Stanford University)\n\nResearch in many areas of modern physics such as\, e.g.\, indirect searches for dark matter and particle acceleration in supernova remnant shocks rely heavily on studies of cosmic rays (CRs) and associated diffuse emissions (radio\, microwave\, X-rays\, gamma rays). The numerical Galactic CR propagation co de GALPROP has been shown to reproduce simultaneously observational data o f many kinds related to CR origin and propagation. I will report on the la test updates of GALPROP and provide an overview of recent results.\n\nhttp s://events.icecube.wisc.edu/event/39/contributions/2388/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2388/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamics\, structure and signatures of the sector region in the ou ter heliosphere: a turbulent sea of bubbles DTSTART:20111029T200000Z DTEND:20111029T202000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2390@events.icecube.wisc.edu DESCRIPTION:Speakers: Merav Opher (Boston University)\, J.F. Drake (Univer sity of Maryland)\, M Swisdak (University of Maryland)\, K Schoeffler (Uni versity of Maryland)\n\nAll current global models of the heliosphere are b ased on the assumption that the magnetic field in the heliosheath connect s back to the Sun. In particular\, models of transports of galactic cosmic rays (GCR) assume the heliospheric current sheet is laminar as well. The sectored magnetic field due to the flapping of the heliospheric current sh eet compresses across the termination shock and may reconnect in the helio sheath\, driving the anomalous cosmic rays and producing a sea of elongate d magnetic bubbles. These magnetic islands/bubbles will be convected with ambient flows as the sector region is carried to higher latitudes filling the heliosheath. We present a three-dimensional MHD simulation with very h igh numerical resolution that captures the north-south boundaries of the s ector region.\nWe show that due to the high pressure of interstellar magne tic field a north-south asymmetry develops such that the disordered sector ed region fills a large portion of the northern part of the heliosphere wi th a smaller extension in the southern hemisphere. We present particle-in- cell simulations that capture the development and dynamics of the bubbles. A number of Voyager observations are consistent with the bubble picture o f the heliostheath\, including flow enhancements\, magnetic field compress ions\, and strongly-altered transport properties. The magnetic field outsi de the sector will be laminar connecting back to the Sun. We expect then t hat the diffusive nature will be very different inside vs outside the sect or region. Under this new scenario\, the heliopause will not be the tradit ional thought tangential discontinuity separating the heliosphere from the interstellar medium\, but more like a porous membrane. A porous heliosphe re might allow GCRs to enter more easily into the heliosphere. Once they e nter inside the sector region they get trapped in the magnetic bubbles slo wly making their way into the heliosphere. If they diffuse into the unipol ar region they quickly escape into the heliosphere.\n\nhttps://events.icec ube.wisc.edu/event/39/contributions/2390/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2390/ END:VEVENT BEGIN:VEVENT SUMMARY:A brief summary of IBEX observations of the heliospheric interacti on DTSTART:20111029T193000Z DTEND:20111029T195000Z DTSTAMP:20260610T034300Z UID:indico-contribution-2391@events.icecube.wisc.edu DESCRIPTION:Speakers: David McComas (Southwest Research Institute)\n\nThis talk summarizes the recent observations of the interaction of the heliosp here with the local interstellar medium as observed remotely by the Inters tellar Boundary Explorer (IBEX). IBEX observations have shown that the int eraction is far more complex and dynamic than previously anticipated and r aised many new questions about this important interaction.\n\nhttps://even ts.icecube.wisc.edu/event/39/contributions/2391/ LOCATION:309 (University of Wisconsin Pyle Center) URL:https://events.icecube.wisc.edu/event/39/contributions/2391/ END:VEVENT END:VCALENDAR