BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Implication of the sidereal anisotropy of ~10 TeV cosmic ray inten sity observed with the Tibet III air shower array DTSTART;VALUE=DATE-TIME:20070710T133000Z DTEND;VALUE=DATE-TIME:20070710T134200Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-256@cern.ch DESCRIPTION:Speakers: Prof. TAKITA\, M. (University of Tokyo)\nThis paper presents the sidereal anisotropy of ~10 TeV galactic cosmic ray \n(GCR) in tensity observed by the Tibet Air Shower experiment. The observed sky-\nma p of the directional anisotropy clearly shows the large-scale feature \nco nsisting of excess and deficit of the relative intensity. We note that the \nobserved angular separation between the excess and the deficit is ~120 deg\, \nwhich is much smaller than 180 deg expected from the uni-direction al flow but \nsignificantly larger than 90 deg expected from the bi-direct ional counter \nstreaming. According to our preliminary least-square analy sis\, the large-scale \nfeature can be reproduced by a combination of the uni-directional and bi-\ndirectional flows with reference axes perpendicul ar to each other. We suggest \nthat such two streams can be expected if th e GCR population is lower at the \nlocation of the heliosphere in the loca l interstellar cloud (LIC) than that outside \nLIC. If this is the case\, the orientation of the local interstellar magnetic field can \nbe inferred from the reference axis of the bi-directional streaming.\n\nhttps://indic o.nucleares.unam.mx/event/4/session/87/contribution/256 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/256 END:VEVENT BEGIN:VEVENT SUMMARY:Direction of the anisotropy vector of cosmic rays of TeV energies DTSTART;VALUE=DATE-TIME:20070710T134200Z DTEND;VALUE=DATE-TIME:20070710T135400Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-492@cern.ch DESCRIPTION:Speakers: Dr. LIDVANSKY\, Alexander (Institute for Nuclear Res earch\, Russian Academy of Sciences)\nWe present preliminary results of me asuring the direction of the anisotropy \nvector of cosmic ray intensity. The measurements were made with the Carpet \nair shower array of the Baksa n Neutrino Observatory. The anisotropy vector \ndirection is determined by analyzing the distribution of time delays of the \nshower signal detected by distant detectors of the array relative to the array’s \ncentral par t. It is demonstrated that the anisotropy vector has the direction RA \n ≈ 1.5 h and DEC ≈ 62º in the equatorial coordinate system\, which c orresponds \nto the position in the galactic plane. The implications of th is result and its \nconsistency with some recent measurements are discusse d.\n\nhttps://indico.nucleares.unam.mx/event/4/session/87/contribution/492 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/492 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of the Anisotropy of 10 TeV Primary Cosmic Ray Nuclei Flux with the Super-Kamiokande-I Detector DTSTART;VALUE=DATE-TIME:20070710T135400Z DTEND;VALUE=DATE-TIME:20070710T140600Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-394@cern.ch DESCRIPTION:Speakers: Dr. OYAMA\, Yuichi (KEK)\nThe relative sidereal vari ation in the arrival direction of primary\ncosmic ray nuclei of median ene rgy 10 TeV was measured using downward\,\nthrough-going muons detected wit h the Super-Kamiokande-I detector.\nThe projection of the anisotropy map o nto the right ascension axis has\na first harmonic amplitude of\n(6.64 +/- 0.98 (stat.) +/- 0.55 (syst.)) x 10^-4 and a phase at maximum at\n(33.2^o +/- 8.2^o (stat.) +/- 5.1^o (syst.)) right ascension.\nA sky map in equat orial coordinates indicates an\nexcess region in the constellation of Taur us and a deficit region toward Virgo.\nThe excess region is centered at\n( alpha_T\,delta_T) = (75^o +/- 7^o\, -5^o +/- 9^o)\nwith a half opening ang le chi_T = (39 +/- 7)^o\;\nthe excess flux is (0.104 +/- 0.020)% above the isotropic expectation.\nThe corresponding parameters for the deficit regi on are\n(alpha_V\, delta_V) = (205^o +/- 7^o\, 5^o +/- 10^o)\,\nchi_V = (5 4 +/- 7)^o\, and (-0.094 +/- 0.014)%.\nThe data do not allow us to rule ou t a pure dipole form for the anisotropy\n(allowed at 13% confidence level) \; they are better described\nby the excess and deficit cones described ab ove.\nWe explored the implications under the assumption that the true anis otropy\nis not distorted too much by the analysis filter so that\nit is we ll-described by the observed excess and deficit cones.\n\nhttps://indico.n ucleares.unam.mx/event/4/session/87/contribution/394 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/394 END:VEVENT BEGIN:VEVENT SUMMARY:Vortex electric field in interplanetary medium and the 11-year mod ulation of galactic cosmic ray anisotropy DTSTART;VALUE=DATE-TIME:20070710T140600Z DTEND;VALUE=DATE-TIME:20070710T141800Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-131@cern.ch DESCRIPTION:Speakers: Dr. GERASIMOVA\, Sardaana (Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy SB RAS)\nOn the basis of world networ k data of neutron monitors and muon telescopes \nat the Yakutsk and Nagoya stations the galactic cosmic ray anisotropy directed \ntransverse to the mean field line (in the direction of 15.00 LT) has been \nrevealed. This c omponent undergoes the 11-year variation. Its value rises as \nthe IMF int ensity\, solar activity level and neutral sheet deformation increase. \nSu ch a property of this component is explained by the action of vortex elect ric \nfield in the heliosphere.\nThe 22-year variation of anisotropy compo nent directed along the magnetic field \nis of a drift origin.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/87/contribution/131 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/131 END:VEVENT BEGIN:VEVENT SUMMARY:ACE/Wind multispacecraft analysis of anisotropic solar wind fluctu ations DTSTART;VALUE=DATE-TIME:20070710T141800Z DTEND;VALUE=DATE-TIME:20070710T143000Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-937@cern.ch DESCRIPTION:Speakers: Dr. DASSO\, Sergio (Instituto de Astronomía y Físi ca del Espacio (IAFE))\nThe propagation of galactic and solar cosmic rays in the\nsolar wind (SW) can be strongly influenced by the SW\nfluctuations properties. Magnetohydrodynamic (MHD) scale\nfluctuations in the solar wi nd are usually highly\nanisotropic\, and have also been found to exhibit d ifferent\nproperties in regions of high and low solar wind speed.\nWe anal yze here the anisotropy properties of the solar\nwind fluctuations from si ngle (assuming Taylor\nfrozen-in hypothesis) and multispacecraft analysis\ n(observing the pure spatial structures).\nFrom the single spacecraft anal ysis (5 years of\nobservations from ACE) we found that the\nfast solar win d contains fluctuations (magnetic\, velocity\nand cross helicity fluctuati ons) with\nwave numbers mostly parallel to the\nmean magnetic field\, whil e in the slow wind the\nfluctuations are mostly perpendicular.\nIn this wo rk we compare these previous results\nwith a multispacecraft\nanalysis usi ng combined observations of ACE-Wind.\n\nhttps://indico.nucleares.unam.mx/ event/4/session/87/contribution/937 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/937 END:VEVENT BEGIN:VEVENT SUMMARY:Solar and heliospherc cosmic ray observations with PAMELA experim ent DTSTART;VALUE=DATE-TIME:20070710T143000Z DTEND;VALUE=DATE-TIME:20070710T144200Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-501@cern.ch DESCRIPTION:Speakers: Dr. CASOLINO\, Marco (INFN ROma2)\nPAMELA was launc hed on June $15^{th}$ 2006 in a pressurized container on board the\nRuss ian Resurs-DK1 satellite. The satellite is flying in high inclination ($ 70^o$)\,\nlow Earth Orbit (350-600 km)\, allowing measurements in variou s points and\nconditions of the geomagnetosphere. It is a multi-purpose apparatus composed of a\npermanent\nmagnet spectrometer to provide partic le charge\, rigidity and incoming angle. A \nseries of six \nscintillato r counters arranged at its extremities provide redundant Time-of-Flight\ nand charge data. Lepton/hadron identification is performed by a\nSili con-Tungsten calorimeter and a Neutron detector placed at the\nbottom of t he device. An Anticounter system is used offline to\nreject false triggers coming from the satellite. \nThe device is capable of detecting protons (80 MeV- 700 GeV)\, antiprotons (80\nMeV-190 GeV)\, electrons (50 MeV - 4 00 GeV)\, positrons (50 MeV - 270 Gev) and light\nnuclei ($\\simeq 100 Me V/n 200GeV/nuc). For its characteristics PAMELA is capable of\naddressing various items of heliospheric physics. For instance it is capable of\np erforming for the first time a very precise measurement of the high energ y\ncomponent in solar events and to detect directly positrons and neut rons produced\nin these events. Also long term solar modulation\, charg e dependent effects\, trapped\n particles and Jupiter electrons will b e studied in the three years of expected\nmission. We will describe the ch aracteristics of the detector and the scientific\nobjectives in light of i ts first months of data taking in space.\n\nhttps://indico.nucleares.unam. mx/event/4/session/87/contribution/501 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/501 END:VEVENT BEGIN:VEVENT SUMMARY:Charge and Mass Composition of heavy ions in the Earth’s Radiati on Belt DTSTART;VALUE=DATE-TIME:20070710T144200Z DTEND;VALUE=DATE-TIME:20070710T145400Z DTSTAMP;VALUE=DATE-TIME:20261017T114750Z UID:indico-contribution-87-0-811@cern.ch DESCRIPTION:Speakers: Dr. HAREYAMA\, Makoto (Advanced Research Institute f or Science and Engineering\, Waseda University)\nEnergetic heavy ions with 20 – 200 MeV/n in the radiation belts have been observed by\nHeavy Ion Telescope (HIT) onboard TSUBASA satellite which stayed in the geostationar y\ntransfer orbit with the inclination of 28.5 deg. The observed data duri ng quiet\nperiod in the outer region of radiation belt found out that the relative abundance\nfor major elements\, C\, O\, Ne\, Mg\, Si and Fe\, wer e similar to that of galactic cosmic\nrays (GCRs) obtained by ACE/CRIS at Lagrangian points as L1\, in particularly for the\nratio of 22Ne/20Ne\, wh ile the absolute intensities in the radiation belt were less\nthan that ob tained by ACE/CRIS beyond the radiation belt. On the other hand\, in the\n inner region of radiation belt near the earth\, the major elements except for helium\nnuclei could not observed and the ratio of 3He/4He was enhance d as compared with that\nof solar abundance or GCR abundance. Thus charge and mass composition of heavy ions\nobtained from these data available wil l give us the considerations of possible origin\nand behavior of energetic heavy ions in the radiation belt.\n\nhttps://indico.nucleares.unam.mx/eve nt/4/session/87/contribution/811 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/87/contribution/811 END:VEVENT END:VCALENDAR