BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Estimation of the Energy Spectra of Primary Cosmic Ray Nuclei DTSTART;VALUE=DATE-TIME:20070704T170500Z DTEND;VALUE=DATE-TIME:20070704T171700Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-965@cern.ch DESCRIPTION:Speakers: Prof. KEMPA\, Janusz (Warsaw University of Technolog y\, Off-Campus Plock)\nEnergy spectra and chemical composition of the prim ary cosmic ray nuclei for energies\nhigher than 1 PeV are obtained mainly from measurements of intensities and various\nproperties of extensive air showers. Additional and importent data from the study of\ngamma ray famili es are available in addition. In bouth cases we have informations \nfrom t he range of very high fluctuations. An importent fact that we are working with\nthe very steep primary energy spectra has to be taking into account. In this research\ndifferent probability distributions have been used as w ell as their convolutions with\npower primary spectrum.The role of the inf luence of different parameters on the\nmeasurements of primary spectra wil l be discussed in the paper.\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/4/contribution/965 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/965 END:VEVENT BEGIN:VEVENT SUMMARY:Constraints on the lepton content of PWN from the local CR positro n spectrum DTSTART;VALUE=DATE-TIME:20070704T171700Z DTEND;VALUE=DATE-TIME:20070704T172900Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-945@cern.ch DESCRIPTION:Speakers: Dr. BUESCHING\, Ingo (Unit for Space Physics\, North -West University\, Potchefstroom)\nGeminga is a nearby pulsar with an age of 3.42e+05 yr and a spin down power of\n3.2e+34 erg/s at present. The win d of this pulsar most probably had powered a PWN\nthat broke up about le ss than 1.e+05 yr after the birth of the pulsar. Assuming that\nleptonic p articles accelerated by the pulsar were confined in the PWN and got\nrele ased into the interstellar medium on breakup of the PWN\, we calculate the \ncontribution of these particles to the locally observed cosmic ray elect ron and\npositron spectra. Our calculations show that within the framework of our model\, the\nlocal CR positron spectrum imposes constraints on pul sar parameters for Geminga\, e.g.\nthe pulsar period at birth\, and also t he local interstellar diffusion coefficient for\nCR leptons.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/4/contribution/945 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/945 END:VEVENT BEGIN:VEVENT SUMMARY:Chemical composition of cosmic rays at the knee measured by the Ti bet air-shower-core detector. DTSTART;VALUE=DATE-TIME:20070704T172900Z DTEND;VALUE=DATE-TIME:20070704T174100Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-356@cern.ch DESCRIPTION:Speakers: Prof. SHIBATA\, Makio (Faculty of Engineering\, Yoko hama National University)\nFurther analysis is made on the Tibet hybrid ex periment to measure the energy \nspectrum of light component (proton and h elium) of the cosmic rays at the knee.\nThe result from three years observ ation by the burst detectors operated\nwith Tibet III air-shower array is presented and compared with the\nresult of the first phase experiment.\n\n https://indico.nucleares.unam.mx/event/4/session/4/contribution/356 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/356 END:VEVENT BEGIN:VEVENT SUMMARY:Measuring Cosmic Ray Composition at the Knee with SPASE-2/AMANDA- II DTSTART;VALUE=DATE-TIME:20070704T174100Z DTEND;VALUE=DATE-TIME:20070704T175300Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-1285@cern.ch DESCRIPTION:Speakers: Dr. SONG\, Chihwa (University of Winsconsin)\nImport ant information pertaining to the origin of high-energy cosmic rays can be gained by studying their mass \ncomposition in the region of the knee (~3 PeV). Thus\, air showers have been observed at the South Pole using the \nSPASE-2 surface array\, which measures the electron-component\, and the AMANDA-2 neutrino telescope\, which \nmeasures the coincident muon-compone nt. These two components\, together with a neural network and a well-\nun derstood Monte Carlo simulation\, yield the cosmic ray energy spectrum as well as the relative cosmic ray \ncomposition in the knee region. We repor t on the results of the analysis.\n\nhttps://indico.nucleares.unam.mx/even t/4/session/4/contribution/1285 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/1285 END:VEVENT BEGIN:VEVENT SUMMARY:A Possible Mechanism to Form the Source Composition of Galactic Co smic Rays as Viewed from the Fractionation of Heavy Elements in Carbonaceo us Chondrites DTSTART;VALUE=DATE-TIME:20070704T175300Z DTEND;VALUE=DATE-TIME:20070704T180500Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-821@cern.ch DESCRIPTION:Speakers: Dr. SAKURAI\, Kunitomo (Advanced Research Institute for Science and Engineering\, Waseda University)\nReferring to the observe d data in the depletions of elements in the interstellar\nclouds\, the che mical composition of dust grains has been deduced\, though it is highly\nv ariable among these clouds. This variability seems to reflect upon the pla ce where\nsuch dust grains are formed inside these clouds. Deep inside the clouds\, the chemical\ncomposition of dust grains is well coincident with that of carbonaceous chondrites as\nclassified as CI. Since the source co mposition of galactic cosmic rays in much more\nabundant in refractory and siderophile elements\, being classified as heavy and\nultra-heavy ones\, as compared with those as contained in carbonaceous CI chondrites\,\nthe m ost of volatile elements must have been lost during the process which took place\nin forming the matter as identified to be “seed mass” which is to be later\naccelerated to cosmic ray every this process seems necessari ly to be associated with\nthe heating and ionization of dust grains formed within interstellar clouds. Volatile\nelements must have effectively been lost from chondrites though that process\, which\nbecome process\, and th en form the seed mass\, which becomes the source matter from\nwhich cosmic rays are generated afterward.\n\nhttps://indico.nucleares.unam.mx/event/4 /session/4/contribution/821 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/821 END:VEVENT BEGIN:VEVENT SUMMARY:Primary and Secondary Contributions to Arriving Abundances of Cosm ic Ray Nuclides DTSTART;VALUE=DATE-TIME:20070704T180500Z DTEND;VALUE=DATE-TIME:20070704T181700Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-1117@cern.ch DESCRIPTION:Speakers: Dr. WIEDENBECK\, Mark (Jet Propulsion Laboratory\, C alifornia Institute of Technology)\nThe arriving abundances of a variety o f cosmic-ray nuclides consist of\ncomparable amounts of primary material p roduced by stellar\nnucleosynthesis and secondary matter resulting from fr agmentation of\nheavier nuclei by collisions during interstellar propagati on. In\norder to utilize such species in studies of cosmic-ray source\nco mposition it is necessary to determine the secondary fraction\npresent in the arriving material and to assess the uncertainty in this\ndetermination . We have extracted the primary and secondary\ncontributions to the arriv ing abundances for isotopes of elements\nbetween B and Ni by using 1) meas urements of cosmic-ray elemental and\nisotopic composition obtained from t he Cosmic Ray Isotope Spectrometer\n(CRIS) instrument on the Advanced Comp osition Explorer (ACE)\nspacecraft\, 2) a data base of measured and calcul ated fragmentation\ncross sections\, and 3) a leaky box model of interstel lar propagation.\nWe present derived decompositions and discuss their impl ications for\nstudies of the composition of cosmic-ray source material.\n\ nThis work was supported by NASA at Caltech (under grant NAG5-12929)\,\nJP L\, Washington University\, and GSFC.\n\nhttps://indico.nucleares.unam.mx/ event/4/session/4/contribution/1117 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/1117 END:VEVENT BEGIN:VEVENT SUMMARY:Evidence that a cluster of UHECRs was produced by a burst or flare DTSTART;VALUE=DATE-TIME:20070704T181700Z DTEND;VALUE=DATE-TIME:20070704T182900Z DTSTAMP;VALUE=DATE-TIME:20260611T141331Z UID:indico-contribution-4-0-1269@cern.ch DESCRIPTION:Speakers: Prof. FARRAR\, Glennys (New York University)\nThe Ur sa Major (UM) cluster of UHECRs consists of 5 events in the combined\nHiRe s-AGASA sample above 10 EeV which are consistent with coming from a single point\nsource\, with little magnetic deflection. The probability of find ing the cluster of 4\nhighest energy events by chance is about 2 10^-3\; t he probability that the 5th low\nenergy event is a chance correlation\, gi ven the size of the low energy dataset\, is\none in 6. The spectrum of th e UM UHECR cluster is in good agreement from that\nexpected from a burstin g or flaring source\, and in poor agreement with that of a\ncontinuous sou rce\, with a factor 500 relative probability. The energy released in\nthe burst or flare and the time-delay of the UHECRs compared to photons from the\nburst are determined\, as a function of the unknown source distance. Compatibility of\nthese constraints with various models of bursting sourc es is discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/4/con tribution/1269 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/4/contribution/1269 END:VEVENT END:VCALENDAR