BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Heliospheric Boundary and the TeV Cosmic Ray Cosmic Ray Anisotropy DTSTART:20130928T170500Z DTEND:20130928T173000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3219@events.icecube.wisc.edu DESCRIPTION:Speakers: Paolo Desiati (University of Wisconsin - Madison)\, Alex Lazarian (University of Wisconsin)\n\nThe observation of a small but significant anisotropy in the cosmic ray distribution on Earth as a functi on of energy has initiated a series of discussions on the effects of parti cle propagation across the local interstellar magnetized medium. The sudde n topological change of the anisotropy above 100 TeV particle energy\, see ms to hint to a heliospheric scenario. A discussion on the effects of the heliosphere on cosmic ray transport with energy in excess of about 10 TeV is presented. Such effect may be responsible of the topological transition of the anisotropy and of some small scale features.\n\nhttps://events.ice cube.wisc.edu/event/48/contributions/3219/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3219/ END:VEVENT BEGIN:VEVENT SUMMARY:The Cosmic Ray - Anisotropy Connection DTSTART:20130926T184000Z DTEND:20130926T192000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3220@events.icecube.wisc.edu DESCRIPTION:Speakers: Pasquale Blasi (INAF/Arcetri Astrophysical Observato ry)\n\nI will illustrate the type of information that we can gather on acc eleration and propagation of cosmic rays from measurement of anisotropy. M ore specifically I will focus on two issues: 1) a discussion the the probl ems arising from the measured anisotropy when compared with the standard s upernova remnant paradigm for the origin of cosmic rays\; 2) a discussion of the implications of the Pierre Auger\, ICETOP and KASCADE-Grande measur ements for the transition from Galactic to extragalactic cosmic rays and h ow these implications confront the measured anisotropy in the EeV energy r ange.\n\nhttps://events.icecube.wisc.edu/event/48/contributions/3220/ LOCATION:Northwoods\, 3rd floor center (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3220/ END:VEVENT BEGIN:VEVENT SUMMARY:Numerical Modeling of the Heliotail DTSTART:20130928T142500Z DTEND:20130928T145500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3221@events.icecube.wisc.edu DESCRIPTION:Speakers: Nikolai Pogorelov (University of Alabama in Huntsvil le)\, Sergey Borovikov (University of Alabama in Huntsville)\, Jacob Heeri khuisen (University of Alabama in Huntsville)\n\nThe heliotail structure i s of interest for the analysis of the Lyman–alpha absorption in the dire ction of the nearby stars\, the energetic neutrals (ENA) production\, and possibly cosmi ray acceleration. Recent Interstellar Boundary Explorer (IB EX) observations revealed rather complex topology of the heliotail (McComa s et al. 2013). We performed 3D\, MHD-kinetic modeling of the solar wind i nteraction with the local interstellar medium to analyze the heliotail reg ion to distances up to 5000 AU downstream. We examined the role of the int erstellar magnetic field in shaping the heliopause. The heliospheric curre nt sheet behavior and the heliopause instability are analyzed. We determin ed that the heliopause is noticeably squeezed. We also show that there is no well-defined boundary between the solar wind and the local interstellar medium in at distances greater than 1500 AU.\n\nhttps://events.icecube.wi sc.edu/event/48/contributions/3221/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3221/ END:VEVENT BEGIN:VEVENT SUMMARY:Local interstellar magnetic field\, Loop I\, and interstellar clou ds DTSTART:20130927T134500Z DTEND:20130927T142500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3222@events.icecube.wisc.edu DESCRIPTION:Speakers: Priscilla Frisch (University of Chicago)\n\nBefore r eaching the Earth\, galactic cosmic rays must traverse nearby\npartially i onized low density interstellar clouds. The evolved\nsuperbubble known as Loop I appears to order the cloud kinematics and\nthe magnetic field of t he interstellar medium (ISM) within tens of parsecs.\nThe direction of the nearby interstellar magnetic field (ISMF) that is\nfound from starlight p olarized in the local interstellar medium is\napproximately parallel to th e local surface of the Loop I shell that dominates the northern hemisphere . Nearby\ninterstellar clouds flow through the local standard of rest wit h a\ndirection that is perpendicular to the ISMF direction\, to within the \nuncertainties. The direction of the ISMF helping to shape the\nheliosph ere is found from the center of the Ribbon of energetic\nneutral atoms dis covered by the Interstellar Boundary Explorer (IBEX)\nspacecraft\, and is close to the local field direction found from\npolarization data. Open qu estions remain. The structure of the\ndistant parts of Loop I is filamenta ry and there is evidence for\nfilamentary structure in the local ISM. The role of flux freezing in\nlocal gas is unknown. The polarity of the magne tic field is not clear.\n\nhttps://events.icecube.wisc.edu/event/48/contri butions/3222/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3222/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of cosmic ray energy spectrum with IceCube DTSTART:20130926T160000Z DTEND:20130926T162500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3223@events.icecube.wisc.edu DESCRIPTION:Speakers: Bakhtiyar Ruzybayev (o=udel\,ou=Institutions\,dc=ice cube\,dc=wisc\,dc=edu)\n\nWe report on the measurement of the all-particle cosmic ray energy spectrum with IceCube. Results of two different techniq ues will be presented. The first result is a measurement of the all-partic le cosmic ray energy spectrum in the energy range from 1.58 PeV to 1.26 Ee V using the IceTop air shower array\, which is the surface component of th e IceCube Neutrino Observatory at the South Pole. The second result is a measurement of cosmic ray energy spectrum using neural network techniques and the full IceCube as a 3-dimensional cosmic ray detector. The measured energy spectrum exhibits clear deviations from a single power law above th e knee around 4 PeV and below 1 EeV.\n\nhttps://events.icecube.wisc.edu/ev ent/48/contributions/3223/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3223/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Anisotropy: A Review DTSTART:20130926T140000Z DTEND:20130926T144000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3224@events.icecube.wisc.edu DESCRIPTION:Speakers: Gus Sinnis (Los Alamos National Laboratory)\n\nThe a nisotropy of the cosmic radiation has been studied for over half a century . For much of this time the results have been contradictory and difficult to understand. In the past decade there has been an increasing number of well measured anisotropies\, that exhibit interesting energy dependence. In this talk I will summarize the status of both large and small scale an isotropy measurements from a few TeV to above 10^19 eV. While some featur es of the observed anisotropies are firmly established others are not - fo r example the time dependence of the large scale anisotropy reported by Mi lagro and the chemical composition of the anisotropic component of the cos mic rays. I will discuss the observations that are on firm foundation and point to further measurements that must be made to confirm some of the mor e important but unconfirmed features of the anisotropies. Finally\, I will discuss a new interpretation of the small-scale anisotropy as a local clu mp of dark matter.\n\nhttps://events.icecube.wisc.edu/event/48/contributio ns/3224/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3224/ END:VEVENT BEGIN:VEVENT SUMMARY:Anisotropic diffusion of cosmic rays and the TeV-band cosmic ray a nisotropy DTSTART:20130926T204000Z DTEND:20130926T210500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3225@events.icecube.wisc.edu DESCRIPTION:Speakers: rahul kumar (ben-gurion university)\n\nWe calculate the time-dependent transport of cosmic rays from point like sources in the Galaxy\, assuming it can be described as diffusion. We show that the sur prisingly small anisotropy in the TeV band\, as recently reported by IceCu be and others\, can be reproduced assuming a small radial diffusion rate\, without assuming a uniform distribution of the sources in the Galaxy.\n\n https://events.icecube.wisc.edu/event/48/contributions/3225/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3225/ END:VEVENT BEGIN:VEVENT SUMMARY:What do the spectral breaks in CR spectrum tell us? DTSTART:20130927T205500Z DTEND:20130927T212000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3226@events.icecube.wisc.edu DESCRIPTION:Speakers: Serap Tilav (o=udel\,ou=Institutions\,dc=icecube\,dc =wisc\,dc=edu)\n\nRigidity dependent breaks and the hardening of the eleme ntal spectra observed above 200 GeV provided the most important hint on th e nature of the cosmic ray knee. Model independent analysis of the CR data (direct and indirect combined) shows at least 3 different source populati ons needed to describe the spectrum and composition from 200 GeV up to 200 EeV.\n\nhttps://events.icecube.wisc.edu/event/48/contributions/3226/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3226/ END:VEVENT BEGIN:VEVENT SUMMARY:Large-Scale Distribution of Arrival Directions of Cosmic Rays Dete cted at the Pierre Auger Observatory Above ~10 PeV DTSTART:20130926T165000Z DTEND:20130926T171000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3227@events.icecube.wisc.edu DESCRIPTION:Speakers: Olivier Deligny (CNRS/IN2P3 - IPN Orsay)\n\nHarmonic analyses dedicated to searches for large-scale anisotropies in both right ascension and declination distributions of cosmic rays detected above ~10 PeV at the Pierre Auger Observatory are presented. Though additional stat istics is still needed to characterize unambiguously the patterns as a fun ction of the energy due to their relatively low dipole and quadrupole ampl itudes\, the focus is given to the few current hints that may be indicativ e of the presence of a structure at large scale over a wide energy range. On the other hand\, the constraints on the production of cosmic rays provi ded by the upper limits obtained on the dipole and quadrupole amplitudes i n the EeV energy range are discussed.\n\nhttps://events.icecube.wisc.edu/e vent/48/contributions/3227/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3227/ END:VEVENT BEGIN:VEVENT SUMMARY:Explanation for the Anisotropies at Small and Medium Angular Scale s DTSTART:20130927T170500Z DTEND:20130927T173000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3228@events.icecube.wisc.edu DESCRIPTION:Speakers: Gwenael Giacinti (University of Oxford)\n\nThe diffu sion approximation (DA) predicts a dipolar anisotropy\, but cannot explain the anisotropies at smaller scales. However\, the DA is not designed to p redict phenomena arising on spatial scales smaller than the cosmic ray mea n free path. We demonstrate here that energy-dependent smaller scale aniso tropies naturally appear on the sky and reflect the local concrete realiza tion of the turbulent magnetic field within the cosmic ray mean free path. \n\nhttps://events.icecube.wisc.edu/event/48/contributions/3228/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3228/ END:VEVENT BEGIN:VEVENT SUMMARY:Recovering the observed B/C ratio in a dynamic spiral-armed cosmic ray model DTSTART:20130927T164000Z DTEND:20130927T170500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3230@events.icecube.wisc.edu DESCRIPTION:Speakers: David Benyamin (The Hebrew University)\, Nir Shaviv (The Hebrew University)\, Piran Tsvi (The Hebrew University)\, Ehud Nakar (Tel-Aviv University)\n\nWe develop a fully three dimensional numerical c ode describing the diffusion of cosmic rays in the Milky Way. It includes the nuclear spallation chain up to Oxygen\, and allows the study of vario us cosmic ray properties\, such as the CR age\, grammage traversed\, and t he ratio between secondary and primary particles. This code enables us to explore a model in which a large fraction of the cosmic ray acceleratio n takes place in the vicinity of galactic spiral arms and that these spira l arms are dynamic.\nWe show that the effect of having dynamic spiral arms is to limit the age of cosmic rays at low energies. This is because at lo w energies the time since the last spiral arm passage governs the Cosmic R ay (CR) age\, and not diffusion. Using the model\, the observed spectral d ependence of the secondary to primary ratio is recovered without requiring any further assumptions such as a galactic wind\, re-acceleration or vari ous assumptions on the diffusivity. In particular\, we obtain a secondary to primary ratio which increases with energy below about 1 GeV.\n\nhttps: //events.icecube.wisc.edu/event/48/contributions/3230/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3230/ END:VEVENT BEGIN:VEVENT SUMMARY:Understanding the anisotropy of TeV cosmic rays DTSTART:20130928T161500Z DTEND:20130928T164000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3231@events.icecube.wisc.edu DESCRIPTION:Speakers: Ming Zhang (Florida Institute of Technology)\n\nRece nt IBEX observation of a ribbon structure in energetic neutral atom emissi ons indicates that the level of turbulence in the interstellar magnetic fi eld is quite low. The quasilinear theory of particle transport predicts a very large parallel diffusion and a very small perpendicular diffusion. A pplying this extremely anisotropic diffusion to cosmic ray transport from a past nearby point source\, we find that there will most likely be a larg e particle intensity gradient perpendicular to the magnetic field directio n. The gradient can change with particle energy rapidly because it is sen sitive to the magnitude of perpendicular diffusion coefficient. While cosm ic ray anisotropy from particle diffusion still points towards the point s ource\, drift anisotropy or b cross gradient anisotropy\, which is enhance d from the perpendicular diffusion anisotropy by the ratio of particle gyr oradius to perpendicular mean free path\, is always perpendicular to the m agnetic field. In the paper\, we will demonstrate how the combination the Compton-Getting effect\, diffusion and drift can result in various behavio rs of large-scale cosmic ray anisotropy. In the mean time\, the large-sca le anisotropy can be break into medium-scale anisotropy when the particles are slightly deflected by the heliospheric magnetic field.\n\nhttps://eve nts.icecube.wisc.edu/event/48/contributions/3231/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3231/ END:VEVENT BEGIN:VEVENT SUMMARY:A New Analysis Method for High-Energy CR Hadron Arrival Directions DTSTART:20130926T192000Z DTEND:20130926T195000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3232@events.icecube.wisc.edu DESCRIPTION:Speakers: Philipp Kronberg (University of Toronto)\n\nA new ap proach to understanding the VHECR / UHECR sky is presented. I describe a multi-parameter analysis that is based on the observed CR arrival directio n distribution. The sky plot origin can be any chosen reference source of cosmic rays. This source-centered sky (unlike [l\,b] etc.) displays simu lated energy-species-direction data. I discuss a preliminary UHECR-determ ined estimate of the intergalactic magnetic field out to ~4Mpc on the assu mption that Cen A is the principal UHECR source. Other assumptions and mo dels can be applied within this general conceptual framework.\n\nThe analy sis method (Yüksel\, Stanev\, Kistler & Kronberg ApJ 2012) can be applied to data from AUGER\, HiRes\, TA\, and their successors. A specific examp le shows\, within our reference assumptions\, how the strength and structu re of B(sub{IGM}) is approximately constrained at >~ 20 nG out to D~4Mpc\, based on recent AUGER data. This is new "territory" for IGM magnetic fie ld probes\, and also the first VHECR sky-based probe of B(sub{IGM}) on nea rby-Universe supra-galactic scales. It is a potentially powerful template for the understanding\, and future modeling\, of VHECR / UHECR propagatio n at greater distances. I also discuss the dependence of CR energy and sp ecies on the observed distribution of arrival directions.\n\nhttps://event s.icecube.wisc.edu/event/48/contributions/3232/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3232/ END:VEVENT BEGIN:VEVENT SUMMARY:Aperiodic magnetic field fluctuations and their effect on cosmic r ays DTSTART:20130927T145500Z DTEND:20130927T152500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3234@events.icecube.wisc.edu DESCRIPTION:Speakers: Reinhard Schlickeiser (Ruhr-University Bochum\, Germ any)\n\nUnderstanding cosmic $(\\delta B\,\\delta E)$-fluctuations in magn etized (interstellar medium) and nonmagnetized (IGM: intergalactic medium) plasmas is of crucial importance for cosmic ray transport\, including the role of collective and noncollective modes and wave-like\, weakly-propaga ting and aperiodic fluctuations. The ordering $B_0\\gg \\delta B\\gg \\del ta E$ in magnetized systems\, necessary for explaining the observed nearly isotropic CR momentum distribution function\, is the basis for a perturba tion scheme leading to the modified diffusion-convection CR transport equa tion and expressions for the CR anisotropy. \n\nThe nonmagnetized IGM med ium containes aperiodic magnetic fluctuations which are spontaneously emit ted by the fully-ionized thermal electron-proton IGM plasma at a level of $\\vert \\delta B\\vert =1.5\\cdot 10^{-16}n_{-7}T_4^{-3/2}$ G. These spon taneously emitted fluctuations affect the propagation of CR protons and el ectrons in the IGM at energies below $10^{15}$ eV.\n\nhttps://events.icecu be.wisc.edu/event/48/contributions/3234/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3234/ END:VEVENT BEGIN:VEVENT SUMMARY:Some remarks on heliospheric observations DTSTART:20130928T145500Z DTEND:20130928T152500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3235@events.icecube.wisc.edu DESCRIPTION:Speakers: Klaus Scherer (Institut für Theoretische Physik Leh rstuhl IV: Weltraum- und Astrophysik Ruhr-Universität Bochum D-44780 Bo chum Germany)\, Horst Fichtner (Institut für Theoretische Physik Lehrstu hl IV: Weltraum- und Astrophysik Ruhr-Universität Bochum D-44780 Bochum Germany)\n\na\n\nhttps://events.icecube.wisc.edu/event/48/contributions/ 3235/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3235/ END:VEVENT BEGIN:VEVENT SUMMARY:Newborn Pulsars as sources of Ultrahigh Energy Cosmic Rays DTSTART:20130926T210500Z DTEND:20130926T213000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3236@events.icecube.wisc.edu DESCRIPTION:Speakers: Ke Fang (University of Chicago)\n\nThe workings of t he most energetic astrophysical accelerators in the Universe are encoded i n the origin of ultrahigh energy cosmic rays (UHECRs). Current observation s by the Auger Observatory\, the largest UHECR observatory\, show a spect rum that agrees with an extragalactic origin\, as well as an interesting  transition in chemical composition from light element to heavier element a s energy increases. Candidate sources range from young neutron stars to ga mma-ray bursts and events in active galaxies. In this talk\, we will dis cuss newborn pulsars as the sources of ultrahigh energy cosmic rays.  We will show that a newborn pulsar model naturally injects heavier elements and can fit the observed spectrum once propagation in the supernova remnan t is taken into account. With the proper injection abundances\, integrate d cosmic rays from the extragalactic pulsar population can match observati on in all aspects - energy spectrum\, chemical composition\, and anisotro py. We will also examine the fingerprints of their Galactic counterparts o n cosmic ray spectrum. Lastly\, we will discuss the multi-messenger smoki ng gun of this scenario - the detectability of high energy neutrinos from pulsars and magnetars.\n\nhttps://events.icecube.wisc.edu/event/48/contrib utions/3236/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3236/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurements of the cosmic rays spectrum and large scale anisotrop ies with the KASCADE-Grande experiment DTSTART:20130926T162500Z DTEND:20130926T165000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3237@events.icecube.wisc.edu DESCRIPTION:Speakers: Andrea Chiavassa (Universita` di Torino)\, Collabora tion for the KASCADE-Grande (-)\n\nThe KASCADE-Grande experiment measured with high precision EAS generated by cosmic rays in the 10^16-10^18 eV ene rgy range\, for each event the total number of charged particles and the n umber of muons were determined.\nBased on these two observables we estimat e the primary energy of each event and we separate the events into two sam ples generated by light and heavy primaries respectively.\nThe measurement of the all particle and of the light and heavy mass groups energy spectra will be presented. Our results show that:\na) the all particle spectrum c annot be described by a single index power law\; \nb) the heavy primaries mass group one show a steepening at ~8x10^16 eV\;\nc) the light primaries mass group one show a hardening at ~10^17 eV.\nA search for large scale an isotropies\, based on the east-west method\, will also be presented. No si gnificant anisotropies were detected. The obtained upper limits will be di scussed and compared with the results of other experiments.\n\nhttps://eve nts.icecube.wisc.edu/event/48/contributions/3237/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3237/ END:VEVENT BEGIN:VEVENT SUMMARY:Super-TIGER and the search for Galactic Cosmic-Ray Origins DTSTART:20130927T193500Z DTEND:20130927T200500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3238@events.icecube.wisc.edu DESCRIPTION:Speakers: John Ennis Ward (Washington University in St. Louis) \n\nSuper-TIGER is a large area (5.4 m^2) balloon-borne instrument designe d to measure cosmic-ray nuclei in the charge interval 30 <= Z <= 42 with i ndividual-element resolution and high statistical precision\, and make exp loratory measurements through Z = 56. These measurements will provide sens itive tests of the emerging model of cosmic-ray origins in OB associations and models of the mechanism for selection of nuclei for acceleration. Fur thermore\, Super-TIGER will measure with high statistical accuracy the ene rgy spectra of the more abundant elements in the interval 10 <= Z <= 28 at energies 0.8 < E < 10 GeV/nucleon to test the hypothesis that nearby micr o-quasars could superpose features on the energy spectra.\nSuper-TIGER\, w hich builds on the heritage of the smaller TIGER\, was constructed by a co llaboration involving WUSTL\, NASA/GSFC\, Caltech\, JPL and U Minn. It was successfully launched from Antarctica in December 2012\, collecting high- quality data for over one month. Particle charge and energy were measured with a combination of plastic scintillators\, acrylic and silica-aerogel C herenkov detectors\, and a scintillating fiber hodoscope. Details of the f light\, instrument performance\, data analysis and preliminary results of the Super-TIGER measurement will be presented.\n\nhttps://events.icecube.w isc.edu/event/48/contributions/3238/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3238/ END:VEVENT BEGIN:VEVENT SUMMARY:Large scale anisotropy of cosmic rays and directional neutrino sig nals from Galactic sources DTSTART:20130927T223500Z DTEND:20130927T230000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3239@events.icecube.wisc.edu DESCRIPTION:Speakers: Luis Anchordoqui (University of Wisconsin Milwaukee) \n\nQuite recently the IceCube Collaboration has reported an observation o f 26 neutrino candidates above ~ 50 TeV. Including the two ~ 1 PeV neutrin os reported earlier in 2013\, these 28 events constitute a 4.3\\sigma exce ss compared to the atmospheric background. In this talk\, I will explore t he compatibility between the data and an unbroken power-law neutrino spect rum\, for various values of spectral index \\Gamma >= 2. I will show that \\Gamma ~ 2.3 is consistent at the ~ 1.5\\sigma level with the observed ev ents up to 1 PeV and to the null observation of events at higher energies. I will then assume that the sources of this unbroken spectrum are Galact ic\, and deduce (i) an energy-transfer fraction from parent protons to pio ns\, and (ii) a discriminating test between the two most popular models (" dip" and "ankle") for the Galactic to extragalactic cosmic-ray transition. Future IceCube data will test the unbroken power law hypothesis\, and\, i f the neutrino sources are Galactic\, discriminate between the "dip" and " ankle" models of Galactic to extragalactic transition.\n\nhttps://events.i cecube.wisc.edu/event/48/contributions/3239/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3239/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic magnetic deflections of UHECRs including realistic random fields DTSTART:20130926T213000Z DTEND:20130926T215500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3240@events.icecube.wisc.edu DESCRIPTION:Speakers: Azadeh Keivani (Louisiana State University)\, Glenny s Farrar (Center for Cosmology and Particle Physics\, New York University) \, Michael Sutherland (Louisiana State University)\, James Matthews (Louis iana State University)\n\nA\n\nhttps://events.icecube.wisc.edu/event/48/co ntributions/3240/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3240/ END:VEVENT BEGIN:VEVENT SUMMARY:Sensitivity of the orbiting JEM-EUSO mission to large-scale anisot ropies DTSTART:20130926T222000Z DTEND:20130926T224500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3241@events.icecube.wisc.edu DESCRIPTION:Speakers: Peter Denton (Vanderbilt University)\, thomas weiler (vanderbilt university)\, Luis Anchordoqui (University of Wisconsin Milwa ukee)\, Andreas Berlind (Vanderbilt University)\, Matthew Richardson (Vand erbilt University)\n\nThe two main advantages of space-based observation o f extreme-energy (>~10^19 eV) cosmic-rays (EECRs) over ground-based observ atories are the increased field of view and the all-sky coverage with near ly uniform systematics. The former guarantees increased statistics whereas the latter enables a partitioning of the sky into spherical harmonics. We have begun an investigation\, using the spherical harmonic technique\, of the reach of JEM-EUSO into potential anisotropies in the extreme-energy c osmic-ray sky-map for several different source models. The technique is ex plained here\, and first results are presented. The discovery of anisotrop ies would help to identify the long-sought origin of EECRs.\n\nhttps://eve nts.icecube.wisc.edu/event/48/contributions/3241/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3241/ END:VEVENT BEGIN:VEVENT SUMMARY:Modeling the Lyman-alpha backscatter observed by Voyager 1 and 2 i n the outer heliosphere and the structure of the heliospheric bow shock DTSTART:20130928T154500Z DTEND:20130928T161500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3242@events.icecube.wisc.edu DESCRIPTION:Speakers: Gary Zank (University of Alabama in Huntsville)\n\n1 ) Observations made by ultraviolet (UV) detectors on board Pioneer 10 \, V oyager 1 \, and Voyager 2 can be used to analyze the distribution of neut ral hydrogen throughout the heliosphere\, including the interaction region s of the solar wind and local interstellar medium. We use state-of-the art three-dimensional (3D) magnetohydrodynamic (MHD) – kinetic neutral H mo dels to simulate Lyman-alpha backscatter as would be seen by the three spa cecraft\, exploiting a new 3D Monte Carlo radiative transfer code under so lar minimum conditions (Fayock et al.\, 2013) . Both observations and simu lations of the UV backscatter intensity are normalized for each spacecraft flight path at 15 AU\, and we compare simulations with Voyager 1 and 2 an d Pioneer 10 Lyman-alpha data results\, finding a very close match with th e Voyager data. Our results predict a large increase in the Lyman-alpha in tensity as the hydrogen wall is approached.\n\n2) Recent IBEX observations indicate that the local interstellar medium (LISM) flow speed is less tha n previously thought (23.2 km/s rather than 26 km/s)\, indicating that the LISM flow may be either marginally super-fast magnetosonic or sub-fast ma gnetosonic. This raises two questions: (A) Can a LISM model that is barely super-fast or sub-fast magnetosonic account for Ly-alpha observations tha t rely critically on the additional absorption provided by the hydrogen wa ll (H-wall)? and (B) If the LISM flow is weakly super-fast magnetosonic\, does the transition assume the form of a traditional shock or does neutral hydrogen (H) mediate shock dissipation and hence structure through charge exchange? Both questions are addressed using three-dimensional self-consi stently coupled magnetohydrodynamic plasma – kinetic neutral H models wi th different LISM magnetic field strengths (2\, 3\, and 4mG) as well as pl asma and neutral H number densities. The 2 and 3mG models are fast magneto sonic far upwind of the heliopause whereas the 4μ G model is fully subson ic. The 2mG model admits a broad (~50–75 AU) bow-shock-like structure. T he 3mG model has a smooth super-fast–sub-fast magnetosonic transition th at resembles a very broad\, ~200 AU thick\, bow wave. A theoretical analys is shows that the transition from a super-fast to a sub-fast magnetosonic downstream state is due to the charge exchange of fast neutral H and hot n eutral H created in the supersonic solar wind and hot inner heliosheath\, respectively. For both the 2mG and the 3mG models\, the super-fast magneto sonic LISM flow passes through a critical point. Because the Mach number i s only barely super-fast magnetosonic in the 3mG case\, the hot and fast n eutral H can completely mediate the transition and impose a charge exchang e length scale on the structure\, making the solar-wind–LISM interaction effectively bow-shock-free. The charge exchange of fast and hot heliosphe ric neutral H therefore provides a primary dissipation mechanism at the we ak heliospheric bow shock. Both super-fast magnetosonic models produce a s izeable H-wall. We find that (1) a sub-fast magnetosonic LISM flow cannot model the observed Ly-alpha absorption profiles along four sightlines corr esponding to upwind\, sidewind\, and downwind\; and (2) both the super-fas t magnetosonic models can account for the Ly-alpha observations\, with pos sibly the bow-shock-free 3μ G model being slightly favored.\n\nhttps://ev ents.icecube.wisc.edu/event/48/contributions/3242/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3242/ END:VEVENT BEGIN:VEVENT SUMMARY:Three-dimensional Structure of the Time-dependent Heliosphere Inte racting with the Local Interstellar Medium DTSTART:20130928T134500Z DTEND:20130928T142500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3243@events.icecube.wisc.edu DESCRIPTION:Speakers: Nikolai Pogorelov (University of Alabama in Huntsvil le)\, Sergey Borovikov (University of Alabama in Huntsville)\, Jacob Heeri khuisen (University of Alabama in Huntsville)\, Gary Zank (University of A labama in Huntsville)\n\nIn this brief overview\, we describe observationa l and modeling aspects of the solar wind (SW) interaction with the local i nterstellar medium (LISM) paying particular attention to three-dimensional and time-dependent effects. We demonstrate that time-dependent phenomena may substantially affect the global streamline and magnetic field topology in the inner heliosheath (IHS) - a plasma layer between the heliospheric termination shock and the heliopause. It is shown that Voyager spacecraft observations cannot be easily interpreted without invoking solar cycle\, m agnetic reconnection\, and MHD instability effects. In particular\, the so lar wind flow backward toward the Sun can be explained by the evolution of magnetic barriers developing in the IHS over the solar cycle. In view of the recent announcement of the Voyager1 penetration into the LISM\, we dis cuss some issues related to numerical modeling of the heliopause instabili ty. The behavior of the heliospheric current sheet in the inner heliosheat h is discussed\, which is sometimes accompanied by transition to a turbule nt flow regime.\nWe also show the results of our numerical modeling of the SW-LISM interaction using observational boundary conditions.\n\nhttps://e vents.icecube.wisc.edu/event/48/contributions/3243/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3243/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray measurements with the Fermi Large Area Telescope DTSTART:20130927T212000Z DTEND:20130927T214500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3244@events.icecube.wisc.edu DESCRIPTION:Speakers: Justin Vandenbroucke (UW Madison)\n\nTBD\n\nhttps:// events.icecube.wisc.edu/event/48/contributions/3244/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3244/ END:VEVENT BEGIN:VEVENT SUMMARY:A hadronic explanation of the lepton anomaly DTSTART:20130927T221000Z DTEND:20130927T223500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3245@events.icecube.wisc.edu DESCRIPTION:Speakers: Philipp Mertsch (KIPAC\, Stanford)\, Markus Ahlers ( o=uwmad\,ou=Institutions\,dc=icecube\,dc=wisc\,dc=edu)\, Subir Sarkar Sark ar (University of Oxford)\n\nThe anomaly in the cosmic ray positron fracti on\, first observed by the PAMELA experiment and later confirmed by Fermi- LAT and AMS-02\, has generated a lot of interest and theoretical efforts\, mostly due to the suggested interpretation as an indirect signature of da rk matter annihilation in the Galaxy. I will argue that this interpretatio n is now strongly disfavoured by searches for gamma-rays from the galactic halo and turn to possible astrophysical explanations. A hadronic model of production and acceleration of secondaries in mature supernova remnants p rovides a compelling explanation of hard secondary positrons and links to signatures in other hadronic channels\, like neutrinos.\n\nhttps://events. icecube.wisc.edu/event/48/contributions/3245/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3245/ END:VEVENT BEGIN:VEVENT SUMMARY:Elemental and Isotopic Abundances and Their Implications for Cosmi c Ray Origins DTSTART:20130927T200500Z DTEND:20130927T203000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3246@events.icecube.wisc.edu DESCRIPTION:Speakers: M.E. Wiedenbeck (Jet Propulsion Laboratory\, Califor nia Institute of Technology\, Pasadena CA 91109)\, T.T. Von Rosenvinge (NA SA/Goddard Space Flight Center\, Greenbelt MD 20771)\, E.C. Stone (Califor nia Institute of Technology\, Pasadena CA 91125)\, R.A. mewaldt (Californi a Institute of Technology\, Pasadena CA 91125)\, R.A. Leske (California In stitute of Technology\, Pasadena CA 91109)\, M.H. Israel (Washington Unive rsity\, St. Louis MO 63130)\, A.C. Cummings (California Institute of Techn ology\, Pasadena\, CA 91109)\, E.R. Christian (NASA/Goddard Space Flight C enter\, Greenbelt MD 20771 USA)\, W.R. Binns (Washington University\, St. Louis\, MO 63130)\, Georgia de Nolfo (NASA/GSFC)\n\nThe answer to the ques tion of the origin of galactic cosmic rays lies not only with directional anisotropies for the highest energies where direction is preserved but als o with in the signatures found in their energy spectra and composition.   Elemental and isotopic measurements carry the imprint of nucleosynthesis\, acceleration time scales\, and residence times within the Galaxy.  Recen t isotopic measurements with the Cosmic Ray Isotope Spectrometer (CRIS) f rom ~80-600 MeV/nucleon aboard the Advanced Composition Explorer (ACE) sat ellite as well as elemental data from Mg through Sr from the Trans-Iron Ga lactic Element Recorder (TIGER)\, suggest an origin linked to OB associati ons.  GCR ratio measurements of 22Ne/20Ne\, 58Fe/56Fe\, and 31Ga/32Ge in particular\, are consistent with a source material that is a mixture of the interstellar material (with solar system abundances) and outflow/ejec ta from massive stars. (The following is a complicated concept and may nee d to be longer to get the points across. I don’t understand it.) Furth ermore\, the ordering of refractory and volatile elements with atomic mas s is improved if the source material includes massive star outflow/ejecta\ , resulting in power-law trend with atomic mass with similar slopes for bo th but with refractory elements preferentially accelerated by a factor of ~4.  Together with recent observations of high-energy gamma-rays from SNR s and extended sources\, we conclude that the likely source of GCRs is con sistent with an origin in OB associations and their associated superbubble s.\n\nhttps://events.icecube.wisc.edu/event/48/contributions/3246/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3246/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-Ray Anisotropy with the HAWC Observatory DTSTART:20130926T144000Z DTEND:20130926T151000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3247@events.icecube.wisc.edu DESCRIPTION:Speakers: Daniel Fiorino (UW-Madison)\, The HAWC Collaboration (The HAWC Collaboration)\n\nThe High-Altitude Water Cherenkov (HAWC) Obse rvatory is a TeV gamma-ray and cosmic-ray detector operating at an altitud e of 4100 meters in Mexico. HAWC is an extensive air-shower array comprisi ng 300 optically-isolated water Cherenkov detectors. While the observator y is only partially deployed\, with 100 Cherenkov detectors in data acquis ition since summer 2013\, statistics are already sufficient to perform stu dies of cosmic-ray anisotropy. We discuss the status and performance of t he detector\, including the pointing accuracy and angular resolution as in ferred from the observation of the moon shadow and simulations\, and prese nt first results on small-scale cosmic-ray anisotropy.\n\nhttps://events.i cecube.wisc.edu/event/48/contributions/3247/ LOCATION:Northwoods\, 3rd floor Center URL:https://events.icecube.wisc.edu/event/48/contributions/3247/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-ray anisotropy studies at TeV and PeV energies with AMANDA\ , IceCube\, and IceTop DTSTART:20130926T151000Z DTEND:20130926T154000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3248@events.icecube.wisc.edu DESCRIPTION:Speakers: Marcos Santander (University of Wisconsin-Madison)\n \nThe study of the cosmic ray anisotropy in the TeV-PeV energy range could provide clues about the origin and propagation of cosmic rays in our gala xy. The measurement of this per-mille-anisotropy requires data sets with s everal billion cosmic-ray events. A sample of this size has been collected over the last six years by the IceCube neutrino telescope at the south po le\, which detects cosmic ray muons at a rate of about 2 kHz. In the IceCu be data\, we observe a significant anisotropy in the southern sky for prim ary energies between 20 and 400 TeV.\n\nThe anisotropy has a large-scale c omponent of per-mille strength\, accompanied by localized excess and defic it regions with smaller amplitudes and typical angular sizes between $10^{ \\circ}$ and $20^{\\circ}$.\nA study of the time variability of the anisot ropy is performed by combining data from IceCube and its predecessor exper iment\, AMANDA\, which operated between 2000 and 2007. Finally\, A change in the shape and an increase in the amplitude of this anisotropy is observ ed at PeV energies by including events of IceTop\, the air shower array ab ove IceCube.\n\nhttps://events.icecube.wisc.edu/event/48/contributions/324 8/ LOCATION:Northwoods\, 3rd floor Center URL:https://events.icecube.wisc.edu/event/48/contributions/3248/ END:VEVENT BEGIN:VEVENT SUMMARY:Telescope Array: Results & Plans DTSTART:20130926T215500Z DTEND:20130926T221500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3249@events.icecube.wisc.edu DESCRIPTION:Speakers: Douglas Bergman (University of Utah)\n\nI will prese nt recent Telescope Array measurements of the spectrum\, composition and a nisotropy of ultra-high energy cosmic rays. I will then present our curren t work and plans for the future.\n\nhttps://events.icecube.wisc.edu/event/ 48/contributions/3249/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3249/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct Measurements of Cosmic Rays DTSTART:20130927T185500Z DTEND:20130927T193500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3250@events.icecube.wisc.edu DESCRIPTION:Speakers: Eun-Suk Seo (University of Maryland)\n\nDirect measu rements of cosmic rays with balloon-borne and space based instruments are used for understanding cosmic ray origin\, acceleration and propagation\, as well as exploring the supernova acceleration limit and searching for ex otic sources such as dark matter. The energy reach of direct measurements is limited by the detector size and exposure time\, but incident particle s are identified element-by-element with excellent charge resolution. Rece nt results and their implications will be reviewed. The outlook of future experiments will also be discussed.\n\nhttps://events.icecube.wisc.edu/eve nt/48/contributions/3250/ LOCATION:Union South\, UW-Madison URL:https://events.icecube.wisc.edu/event/48/contributions/3250/ END:VEVENT BEGIN:VEVENT SUMMARY:First Results of the AMS-02 Experiment on the ISS DTSTART:20130927T214500Z DTEND:20130927T221000Z DTSTAMP:20260915T175600Z UID:indico-contribution-3252@events.icecube.wisc.edu DESCRIPTION:Speakers: Jorge Casaus (CIEMAT - Spain)\n\nAMS-02 is a general purpose cosmic ray detector operating on the International Space Station since 19 May 2011. The results based on the data collected during the firs t 2 years of the mission include high precision measurements of the proton \, helium\, electron and positron fluxes\, and the boron to carbon ratio i n the energy range from ~1GeV/n to ~1TeV/n. Proton and helium spectra are consistent with single power laws with no fine structures or breaks. The b oron to carbon ratio shows no evidence for a structure within the studied energy range. The positron fraction is determined in the energy range from 0.5 to 350GeV and its energy spectrum shows an steadily increasing fracti on from 10 to ~250GeV with no fine structure. The positron to electron and positron to proton ratios are consistent with isotropy within this energy range.\n\nhttps://events.icecube.wisc.edu/event/48/contributions/3252/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3252/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray acceleration in the presence of super diffusion DTSTART:20130927T154500Z DTEND:20130927T161500Z DTSTAMP:20260915T175600Z UID:indico-contribution-3254@events.icecube.wisc.edu DESCRIPTION:Alfvenic turbulence that determines the magnetic field wanderi ng exhibit the process of superdiffusion which results in the perpendicula r\ndisplacement to change as y~x^3/2\, where x is the distance measured al ong magnetic field is the distance perpendicular to the magnetic field\,\n provided that y is less than the injection scale of the turbulence. This p rocess changes substantially the acceleration of cosmic rays in perpendicu lar\nshocks\, which were considered as the accelerating agent of anomalous cosmic rays. I shall discuss how the process of superdiffusion changes\nt he acceleration in parallel and perpendicular shocks and show the analogie s between the shock and reconnection acceleration.\n\nhttps://events.icecu be.wisc.edu/event/48/contributions/3254/ LOCATION:Northwoods (Union South\, UW-Madison) URL:https://events.icecube.wisc.edu/event/48/contributions/3254/ END:VEVENT END:VCALENDAR