BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Cosmic Ray Energetics And Mass (CREAM) Overview DTSTART;VALUE=DATE-TIME:20070705T133000Z DTEND;VALUE=DATE-TIME:20070705T134200Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-677@cern.ch DESCRIPTION:Speakers: Prof. SEO\, Eun-Suk (University of Maryland)\nThe Co smic Ray Energetics And Mass balloon-borne experiment has \naccumulated 70 days of exposure during two successful flights in Antarctica. \nThe inst rument is configured with complementary and redundant particle \ndetectors . Energy measurements are made with a transition radiation detector \nand an ionization calorimeter. Charge measurements are made with timing\, \np ixelated Si\, and Cherenkov detectors to provide powerful rejection of \nb ackscatter particles. High energy cosmic-ray data from the first two fligh ts \nwere collected over a wide energy range from ~ 10 GeV to ~ 1 PeV at a n \naverage altitude of ~38.5 km (~3.9 g/cm^2 atmospheric overburden). \nP reliminary analysis indicates the data extend above 100 TeV and follow \nr easonable power laws. All elements from protons to Fe nuclei are separate d \nwith excellent charge resolution. The payload recovered from the first flight has \nbeen refurbished and is being integrated in preparation for the third launch\, \nscheduled for December 2007. Simultaneously\, the pa yload recovered from the \nsecond flight is being refurbished for a subseq uent fourth flight. Results from \nthe ongoing analysis and future plans will be presented in this paper.\n\nhttps://indico.nucleares.unam.mx/event /4/session/89/contribution/677 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/677 END:VEVENT BEGIN:VEVENT SUMMARY:The Physics of Pamela Space Mission DTSTART;VALUE=DATE-TIME:20070705T134200Z DTEND;VALUE=DATE-TIME:20070705T135400Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-289@cern.ch DESCRIPTION:Speakers: Prof. PICOZZA\, Piergiorgio (University and INFN of Roma Tor Vergata)\nThe Space Mission Pamela\, launched in orbit on 15 June 2006\, represents the \nstate-of-the-art of the investigation of the cos mic radiation to addressing the \nmost compelling issues facing astrophys ics and cosmology: the nature of the \ndark matter that pervades the unive rse\, the apparent absence of cosmological \nantimatter\, the origin and e volution of matter in the galaxy. \nThe primary scientific goal of the Pam ela investigation is the search for \nevidence of non baryonic particle s falling outside Standard Model particles \nphysics and of heavy antinu clei.. Concomitant\, but not secondary\, goals are \nthe study of the ene rgy dependence of cosmic ray lifetimes in the Galaxy\, the \nvalidation o f models of acceleration\, transport and secondary production of \ncosmic radiation in the Galaxy\, the monitoring of the solar activity and the \n knowledge of the role of solar and terrestrial relationships in the energe tic \nparticle propagation in the heliosphere. The observational objective s are the \nmeasurements of the fluxes and the energy spectra of antiprot ons\, protons. \npositrons\, electrons and light nuclei in a very large en ergy range and the \nsearch for antinuclei with a sensitivity of the orde r of 10^{-7} in antiHe/He .\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/89/contribution/289 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/289 END:VEVENT BEGIN:VEVENT SUMMARY:Isotopic composition of cosmic ray sources DTSTART;VALUE=DATE-TIME:20070705T140600Z DTEND;VALUE=DATE-TIME:20070705T141800Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-738@cern.ch DESCRIPTION:Speakers: Dr. MOSKALENKO\, Igor (Stanford University)\nWe use the GALPROP code and the ACE data to derive the cosmic ray isotopic\ncompo sition at the sources. The composition is derived for two propagation mode ls\,\ndiffusive reacceleration and plain diffusion. We show that the compo sitions derived\nassuming different propagation models are different. We a lso compare the isotopic\ncomposition at the sources with the latest solar composition. This may provide a clue\nto the origin of low energy cosmic rays and their acceleration time scale.\n\nhttps://indico.nucleares.unam.m x/event/4/session/89/contribution/738 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/738 END:VEVENT BEGIN:VEVENT SUMMARY:Can solar 6Li abundance really be explained by Galactic cosmic-ray s? DTSTART;VALUE=DATE-TIME:20070705T141800Z DTEND;VALUE=DATE-TIME:20070705T143000Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-258@cern.ch DESCRIPTION:Speakers: Dr. PRODANOVIC\, Tijana (University of Novi Sad\, Se rbia)\nCosmic-ray interactions are the only known source of the rare isoto pe 6Li. The\nstandard picture is that the observed solar 6Li is produced by galactic cosmic-rays\naccelerated in supernova remnants. Thus lithium-6 is a unique probe of the local\nGalactic (hadronic) cosmic-ray history. O n the other hand\, extragalactic gamma-ray\nbackground is a measure of cos mic-ray fluence but for the average star-forming\ngalaxy. Using the connec tion between production of lithium and hadronic gamma-rays in\ncosmic-ray interactions we tested this assumption and came to a surprising and\nalarm ing result: extragalactic gamma-ray background allows for only ~50% of sol ar\nlithium-6 abundance to be produced by Galactic Cosmic Rays. Although e xtreme\nassumptions yield a consistent picture\, more realistic ones indic ate that solar 6Li\ncannot be produced by standard GCRs alone without over producing the hadronic gamma rays.\n\nhttps://indico.nucleares.unam.mx/eve nt/4/session/89/contribution/258 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/258 END:VEVENT BEGIN:VEVENT SUMMARY:CAN 59Ni SYNTHESIZED IN OB ASSOCIATIONS DECAY TO 59CO BEFORE BEING ACCELERATED TO COSMIC-RAY ENERGIES? DTSTART;VALUE=DATE-TIME:20070705T143000Z DTEND;VALUE=DATE-TIME:20070705T144200Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-359@cern.ch DESCRIPTION:Speakers: BINNS\, W. R. (Washington University in St. Louis)\n Observations from the Cosmic Ray Isotope Spectrometer (CRIS) aboard NASA ’s Advanced\nComposition Explorer (ACE) have shown that all relevant gal actic cosmic ray isotopic\nratios measured are consistent with an OB-Assoc iation origin of galactic cosmic rays\n(GCRs). Additionally CRIS measureme nts of the isotopic abundances of 59Ni and 59Co\nhave shown that the 59Ni has completely decayed into 59Co\, indicating a delay of\n>10^5 years betw een nucleosynthesis and acceleration. However\, it has been suggested\ntha t shocks generated from high-velocity Wolf-Rayet winds in the OB-Associati on\nenvironment must accelerate nuclei synthesized in nearby core-collapse SNe on a time\nscale short compared to the 59Ni lifetime of 7.6x10^4 year s. If this were the case\,\nit would imply that OB Associations could not be the source of most galactic cosmic\nrays. In this paper\, we describe t he OB-Association history and environment and show\nthat the time scales f or acceleration are such that most 59Ni should be expected to\ndecay natur ally in that setting\, strengthening the argument that OB associations are \nthe likely source of a substantial fraction of galactic cosmic rays.\n\n https://indico.nucleares.unam.mx/event/4/session/89/contribution/359 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/359 END:VEVENT BEGIN:VEVENT SUMMARY:Spectrum of Cosmic Rays\, produced in Supernova Remnants DTSTART;VALUE=DATE-TIME:20070705T144200Z DTEND;VALUE=DATE-TIME:20070705T145400Z DTSTAMP;VALUE=DATE-TIME:20260417T063515Z UID:indico-contribution-89-0-111@cern.ch DESCRIPTION:Speakers: Prof. BEREZHKO\, Evgeny (Yu.G. Shafer Institute of C osmophysical Research and Aeronomy\, Yakutsk\, Russia)\nA nonlinear kineti c theory of cosmic ray (CR) acceleration in\nsupernova remnants is employe d to calculate CR spectra. The magnetic field\nin SNRs is assumed to be si gnificantly amplified by the effectively accelerating \nnuclear CR compone nt. It is shown that the calculated CR spectra agree in a \nsatisfactory way with the existing measurements of the observed Galactic CR \n(GCR) spe ctrum up to an energy of 100 PeV. The power-law spectrum of \nprotons exte nds up to 3 PeV with a subsequent exponential cutoff that gives a\nnatural explanation for the observed knee in GCR spectrum.\nThe maximum energy of accelerated nuclei is proportional to their charge\nnumber Z. Therefore t he break in the GCR spectrum is the result of the\ncontribution of progres sively heavier species to the overall CR spectrum\,\nso that at 100 PeV th e CR spectrum is dominated by iron group nuclei.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/89/contribution/111 LOCATION:Merida\, Mexico Uxmal + Tulum (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/89/contribution/111 END:VEVENT END:VCALENDAR