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Since the fall of 2003 the Louisiana Aerospace Catalyst Experiences for Students (LaACES) program has been providing university students a two semester project that culminates with the flight of a scientific balloon experiment. During the first semester students complete the Student Ballooning Course (SBC) which teaches basic skills necessary to develop a working scientific payload. The SBC consists of a series of lectures and activities providing instruction in electronics, programming, project management, balloon payload design, and introductory circuit assembly. The SBC introduces the BalloonSat, a sub-assembly designed at LSU for LaACES which contains a microcontroller, real-time clock and a four channel analog-to-digital converter. The second semester is spent on the design, development, testing and calibration of the payloads. Upon completion of the Flight Readiness Review, students travel to the NASA Columbia Scientific Balloon Facility (CSBF) in Palestine, Texas for integration, launch, recovery and science presentations. A flight capable Automatic Packet Reporting System (APRS) radio beacon armed with GPS and command capable cut down was developed to track the balloon during flight and to cut-down the payloads. Tracking vehicles are outfitted with radios tuned to APRS frequency and laptops displaying maps of the payload location. Here we describe LaACES; program development, tools and technologies, implementation, program, management issues and flight experiences.

The CALorimetric Electron Telescope (CALET) is a high-energy astroparticle physics space experiment installed on the International Space Station (ISS), developed and operated by Japan in collaboration with Italy and the United States. The CALET mission goals include the investigation of possible nearby sources of high-energy electrons, of the details of galactic particle acceleration and propagation, and of potential signatures of dark matter. CALET measures the cosmic-ray electron + positron flux up to 20 TeV, gamma-rays up to 10 TeV, and nuclei with Z=1 to 40 up to 1,000 TeV for the more abundant elements during a long-term observation aboard the ISS. Starting science operation in mid-October 2015, CALET performed continuous observation without major interruption with close to 20 million triggered events over 10 GeV per month. Based on the data taken during the first two-years, we present an overview of CALET observations: uses w/o major interruption 1) Electron + positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation including a characterization of on-orbit performance. Results of the electromagnetic counterpart search for LIGO/Virgo gravitational wave events are discussed as well., 10 pages, 10 figures, a contribution to the proceedings of 26th Extended European Cosmic Ray Symposium, 6-10 July 2018, Russia, which summarizes our recent publications such as arXiv:1712.01711, arXiv:1712.01757, arXiv:1803.05834, arXiv:1806.09728, and arXiv:1807.01435

Galactic cosmic rays consist of protons, electrons and ions, most of which are believed to be accelerated to relativistic speeds in supernova remnants. All components of the cosmic rays show an intensity that decreases as a power law with increasing energy (for example as E(-2.7)). Electrons in particular lose energy rapidly through synchrotron and inverse Compton processes, resulting in a relatively short lifetime (about 10(5) years) and a rapidly falling intensity, which raises the possibility of seeing the contribution from individual nearby sources (less than one kiloparsec away). Here we report an excess of galactic cosmic-ray electrons at energies of approximately 300-800 GeV, which indicates a nearby source of energetic electrons. Such a source could be an unseen astrophysical object (such as a pulsar or micro-quasar) that accelerates electrons to those energies, or the electrons could arise from the annihilation of dark matter particles (such as a Kaluza-Klein particle with a mass of about 620 GeV).

The High Altitude Student Platform (HASP) was originally conceived to provide student groups with access to the near-space environment for flight durations and experiment capabilities intermediate between what is possible with small sounding balloons and low Earth orbit rocket launches. HASP is designed to carry up to twelve student payloads to an altitude of about 36 km with flight durations of 15–20 h using a small zero-pressure polyethylene film balloon. This provides a flight capability that can be used to flight-test compact satellites, prototypes and other small payloads designed and built by students. HASP includes a standard mechanical, power and communication interface for the student payload to simplify integration and allows the payloads to be fully exercised. Over the last two years a partnership between the NASA Balloon Program Office (BPO), Columbia Scientific Balloon Facility (CSBF), Louisiana State University (LSU), the Louisiana Board of Regents (BoR), and the Louisiana Space Consortium (LaSPACE) has led to the development, construction and, finally, the first flight of HASP with a complement of eight student payloads on September 4, 2006. Here we discuss the primary as-built HASP systems and features, the student payload interface, HASP performance during the first flight and plans for continuing HASP flights. The HASP project maintains a website at http://laspace.lsu.edu/hasp/ where flight application, interface documentation and status information can be obtained.

The purpose of the ATIC balloon experiment is to measure the energy spectra of primary cosmic rays with individual charge resolution from protons to iron over the energy range from ∼50 GeV to 200 TeV. The particle energy is measured by a bismuth germanate (BGO) scintillation calorimeter. The procedure of calorimeter calibration is described, in particular, calibration of the temperature dependence of the calorimeter sensitivity using the data of in-flight measurements. A technique for determining the energy deposited in the calorimeter in view of the temperature dependence of its sensitivity is presented. The maximum systematic error in determining the deposited energy by the calorimeter is 10% or less, and the probable error is estimated at 6%.

The Advanced Thin Ionization Calorimeter (ATIC) experiment is designed to investigate the charge composition and energy spectra of primary cosmic rays over the energy range from about 10(11) to 10(14) eV during Long Duration Balloon (LDB) flights from McMurdo, Antarctica. Currently, analysis from the ATIC-1 test flight and ATIC-2 science flight is underway and preparation for a second science flight is in progress. Charge identification of the incident cosmic ray is accomplished, primarily, by a pixilated Silicon Matrix detector located at the very top of the instrument. While it has been shown that the Silicon Matrix detector provides good charge identification even in the presence of electromagnetic shower backscatter from tile calorimeter, the detector only measures the charge once. In this paper, we examine use of the top scintillator hodoscope detector to provide a second measure of the cosmic ray charge and, thus, improve the ATIC charge identification. (c) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.

An outstanding issue with aerospace workforce development is what should be done at the university level to attract and prepare undergraduates for an aerospace career. One approach adopted by many institutions is to lead students through the design and development of small payloads (less than about 500 grams) that can be carried up to high altitude (around 30 km) by a latex sounding balloon. This approach has been very successful in helping students to integrate their content knowledge with practical skills and to understand the end-to-end process of aerospace project development. Sounding balloons, however, are usually constrained in flight duration (∼30 min above 24 km) and payload weight, limiting the kinds investigations that are possible. Student built picosatellites, such as CubeSats, can be placed in low Earth orbit removing the flight duration constraint, but the delays between satellite development and launch can be years. Here, we present the inexpensive high altitude student platform (HASP) that is designed to carry at least eight student payloads at a time to an altitude of about 36 km with flight durations of 15–20 h using a small zero-pressure polyethylene film balloon. This platform provides a flight capability greater than sounding balloons and can be used to flight-test compact satellites, prototypes and other small payloads designed and built by students. The HASP includes a standard mechanical, power and communication interface for the student payload to simplify integration and allows the payloads to be fully exercised. HASP is lightweight, has simple mission requirements providing flexibility in the launch schedule, will provide a flight test opportunity at the end of each academic year.

The preliminary energy spectra of heavy nuclei C, O, Ne, Mg, Si, and Fe in the primary cosmic rays measured by the ATIC-2 experiment are presented and compared to previous data and to propagation models. Using previous data to extend the ATIC-2 results for all heavy nuclei to higher energy, the combined spectra can be best fit with diffusion model with weak reacceleration and scattering on random magnetic field with a Kolmogorov spectrum fluctuations becoming dominant at high energy. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved.

A major concern of many aerospace industries and space agencies worldwide is the continuing decrease in undergraduate student enrollment and graduation from aerospace and closely related degree programs. With a decreasing number of new aerospace workforce candidates, expanding or sustaining our exploration of the universe over the coming decades could be at risk. In Louisiana, we have developed the Aerospace Catalyst Experiences for Students (ACES) program to address this issue by attracting new students to aerospace-related programs and providing interdisciplinary training on how to design, build, and manage aerospace payloads. Based upon the National Space Grant Student Satellite Program “Crawl, Walk, Run, Fly!” methodology, ACES closely ties cross-discipline content knowledge with extensive hands-on experiences to instill skills that are then applied by the students to design, document, build, test, and operate a small balloon-borne scientific payload. The ACES concept was initially piloted during 2002–2003 and now includes a semi-formal “Student Ballooning Course”, five Louisiana institutions and serves ∼45 students.

The Advanced Thin Ionization Calorimeter (ATIC) balloon-borne experiment is designed to perform cosmic-ray elemental spectra measurement from 50 GeV to 100 TeV for nuclei from hydrogen to iron. These measurements are expected to provide crucial hints about some of the most fundamental questions in astroparticle physics today. ATTIC'S design centers on an 18 radiation length (X(sub Omnicron)) deep bismuth germanate (BGO) calorimeter, preceded by a 0.75 lambda(sub int) graphite target. In September 1999 the ATIC detector was exposed to high-energy beams at CERN's SPS accelerator, within the framework of the development program for the Advanced Cosmic-ray Composition Experiment for the Space Station (ACCESS). In December 2000 - January 2001, ATIC flew on the first of a series of long duration balloon (LDB) flights from McMurdo Station, Antarctica. We present here results from the 1999 beam-tests, including energy resolutions for electrons and protons at several beam energies from 100 GeV to 375 GeV, as well as signal linearity and collection efficiency estimates. We show how these results compare with expectations based on simulations, and their expected impacts on mission performance.

We analyze the characteristics of the albedo, or the backscatter current, which constitutes a background for charge measurements in calorimetric experiments in high-energy cosmic rays. We compare the experimental data obtained in the flights of the ATIC spectrometer with the simulations performed using the GEANT 3.21 code. We discuss the influence of the backscatter on the charge resolution in the ATIC experiment.

The galactic cosmic radiation spans over 14 decades in energy and follows a power law spectrum in energy which shows two features, a steepening in the power law at a few times 1015 eV—the 'knee'—and a subsequent flattening in the power law at a few times 1018 eV—the 'ankle'. The 'knee' was discovered over 40 years ago through the measurement of cosmic ray initiated air showers, yet its origin and the underlying physics remain largely unknown. Experiments over the past four decades, from both balloon and space platforms, have pressed measurements to ever higher energy and to greater precision. This progression is briefly reviewed with emphasis on the current generation of experiments studying the high-energy regime up to the knee using direct particle-by-particle measurements. Prospects for understanding the 'knee' in terms of the acceleration of the cosmic rays and possible future experiments are included.

During the 1990–1991 solar maximum, the CRRES satellite measured helium from 38 to 110 MeV n−1, with isotopic resolution, during both solar quiet periods and a number of large solar flares, the largest of which were seen during March and June 1991. Helium differential energy spectra and isotopic ratios are analyzed and indicate that (1) the series of large solar energetic particle (SEP) events of 2–22 June display characteristics consistent with CME-driven interplanetary shock acceleration; (2) the SEP events of 23–28 March exhibit signatures of both CME-driven shock acceleration and impulsive SEP acceleration; (3) below about 60 MeV n−1, the helium flux measured by CRRES is dominated by solar helium even during periods of least solar activity; (4) the solar helium below 60 MeV n−1 is enriched in 3He, with a mean 3He/4He ratio of about 0.18 throughout most of the CRRES mission `quiet' periods; and (5) an association of this solar component with small CMEs occurring during the periods selected as solar `quiet' times.

Terrestrial Gamma ray Flashes (TGFs) -- very short, intense bursts of electrons, positrons, and energetic photons originating from terrestrial thunderstorms -- have been detected with satellite instruments. TETRA, an array of NaI(Tl) scintillators at Louisiana State University, has now been used to detect similar bursts of 50 keV to over 2 MeV gamma rays at ground level. After 2.6 years of observation, twenty-four events with durations 0.02- 4.2 msec have been detected associated with nearby lightning, three of them coincident events observed by detectors separated by ~1000 m. Nine of the events occurred within 6 msec and 3 miles of negative polarity cloud-to-ground lightning strokes with measured currents in excess of 20 kA. The events reported here constitute the first catalog of TGFs observed at ground level in close proximity to the acceleration site., To be published in Journal of Geophysical Research: Space Phys. 118, 1

[1] Terrestrial gamma-ray flashes (TGFs)—very short, intense bursts of electrons, positrons, and energetic photons originating from terrestrial thunderstorms—have been detected with satellite instruments. TGF and Energetic Thunderstorm Rooftop Array (TETRA), an array of NaI(Tl) scintillators at Louisiana State University, has now been used to detect similar bursts of 50 keV to over 2 MeV gamma-rays at ground level. After 2.6 years of observation, 24 events with durations 0.02–4.2 ms have been detected associated with nearby lightning, three of them coincident events observed by detectors separated by ∼1000 m. Nine of the events occurred within 6 ms and 5 km of negative polarity cloud-to-ground lightning strokes with measured currents in excess of 20 kA. The events reported here constitute the first catalog of TGFs observed at ground level in close proximity to the acceleration site.

Helium nuclei have been measured within the magnetosphere (L ≤ 6) during the 1990/1991 CRRES mission over an energy range of ∼40–100 MeV nucleonl−1. The Office of Naval Research 604 instrument resolves helium isotopes with a mass resolution of ∼0.1 amu. Each helium isotope can be represented by a power law energy spectrum, and the energy spectrum of the 3He is different from that of 4He; that is, the 3He/4He ratio is energy dependent. In the energy range 51–86 MeV/nucleon the 3He/4He ratio is 7.4 ± 2.6 for L = 1.15–1.3 and 2.2±0.6 for L = 1.8–2.15. All observed helium events at L < 2.65 show pitch angle distributions consistent with equatorially trapped ions, whereas the distributions at larger L values are more uniform, within a factor of 2. For 2.15 < L < 6, as L decreases, the 3He/4He ratio increases and the helium energy spectrum softens. A possible origin of the geomagnetically trapped helium isotopes at L

High energy (approximately 40-100 MeV/nucleon) geomagnetically trapped helium nuclei have been measured, for the first time, by the ONR-604 instrument during the 1990/1991 Combined Release and Radiation Effects Satellite (CRRES) mission. The helium events observed at L less than 2.3 have a pitch angle distribution peaking perpendicular to the local magnetic field and are contained in peaks located at L = 1.2 and 1.9. The events in each peak can be characterized by power law energy spectra with indices of 10.0 +/- 0.7 for L = 1.9-2.3 and 6.8 +/- 1.0 for L = 1.15-1.3, before the large storm of 24 March 1991. CRRES was active during solar maximum when the anomalous component is excluded from the inner heliosphere, making it unlikely that the observed events derived from the anomalous component. The trapped helium counting rates decrease gradually with time indicating that these high energy ions were not injected by flares during the 1990/91 mission. Flare injection prior to mid-1990 may account for the highest energy particles, while solar wind injection during magnetic storms and subsequent acceleration could account for the helium at lower energies.

A strong excess in a form of a wide peak in the energy range of 300-800 GeV was discovered in the first measurements of the electron spectrum in the energy range from 20 GeV to 3 TeV by the balloon-borne experiment ATIC (J. Chang et al. Nature, 2008). The experimental data processing and analysis of the electron spectrum with different criteria for selection of electrons, completely independent of the results reported in (J. Chang et al. Nature, 2008) is employed in the present paper. The new independent analysis generally confirms the results of (J. Chang et al. Nature, 2008), but shows that the spectrum in the region of the excess is represented by a number of narrow peaks. The measured spectrum is compared to the spectrum of (J. Chang et al. Nature, 2008) and to the spectrum of the Fermi/LAT experiment., Comment: LaTeX2e, 10 pages, 4 figures, a paper for ECRS 2010 (Turku, Finland); http://www.astrophys-space-sci-trans.net/7/119/2011/

The energy spectrum of galactic cosmic ray Helium was measured in two different balloon experiments launched four days apart from Canada: SMILI-I on 1-Sept-1989 and MASS on 5-Sept-1989. A slow Forbush decrease began on 4-Sept-1989 and had not reached its maximum at the time of the MASS flight. Comparison of the balloon measurements shows a fractional decrease of 0.37 to 0.15 in the Helium flux between 200 and 450 MeV/nucleon (1.2–2.0 GV). The rigidity dependence is analyzed in two models and found to be steeper than previous observations. Interplanetary particle data and ground-based Neutron Monitor results are consistent with the balloon observations. Probable sources for this Forbush decrease are discussed.

Titanium is a rare, secondary nucleus among Galactic cosmic rays. Using the Silicon matrix in the ATIC experiment, Titanium has been separated. The energy dependence of the Ti to Fe flux ratio in the energy region from 5 GeV per nucleon to about 500 GeV per nucleon is presented., Comment: 8 pages, 4 figures, accepted for publication in Astronomy Letters

The primary scientific mission of the Black Hole Finder Probe (BHFP), part of the NASA Beyond Einstein program, is to survey the local Universe for black holes over a wide range of mass and accretion rate. One approach to such a survey is a hard X-ray coded-aperture imaging mission operating in the 10--600 keV energy band, a spectral range that is considered to be especially useful in the detection of black hole sources. The development of new inorganic scintillator materials provides improved performance (for example, with regards to energy resolution and timing) that is well suited to the BHFP science requirements. Detection planes formed with these materials coupled with a new generation of readout devices represent a major advancement in the performance capabilities of scintillator-based gamma cameras. Here, we discuss the Coded Aperture Survey Telescope for Energetic Radiation (CASTER), a concept that represents a BHFP based on the use of the latest scintillator technology., Comment: 12 pages; conference paper presented at the SPIE conference "UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XIV." To be published in SPIE Conference Proceedings, vol. 5898

Dedication.- Preface.- Part I: Contemporary Challenges in Astrophysics and Cosmology.- Outstanding Problems in Particle Astrophysics T.K. Gaisser.- Constructing the cosmos, from sunboats to superchisters V. Trimble.- Recent Results from the Spitzer Space Telescope: A new View of the Infrared Universe G.G. Fazio.- Beyond the Standard Model in Particle Physics and Cosmology: Convergence or Divergence? M.Yu. Khlopov.- B-L Genesis: Generalities and Impact on Neutrino Physics M. Yoshimura.- Part II: Explosive Events and their Aftermath.- Stellar explosion: from supernovae to gamma-ray bursts K. Postnov.- Close by Compact Objects and Recent Supernovae in the Solar Vicinity S. Popov.- Supernova Remnants as Cosmic Accelerators V. Ptuskin.- Radial distribution of GRBs in host galaxies D.I. Kosenko et al.- Black holes: physics and astrophysics J.D. Bekenstein.- The Efficiency of Using Accretion Power of Kerr Black Holes I. Dutan, P.L. Biermann.- Dark Matter: Past, Present and future V. Trimble.- On Dynamics of Relativistic Shock Waves with Losses in Gamma-ray Burst Sources E.V. Derishev et al.- The dynamics of the Carina spiral arm S. Naoz, N.J. Shaviv.- Magnetic Field Generation and electron acceleration in Collisionless Shocks C.B. Hededal et al.- Part III: High Energy Gamma Ray and Neutrino Astronomy.- High energy neutrino astronomy and underwater detectors E. Migneco, G. Riccobene.- Recent Results from the Milagro Gamma Ray Observatory J.A. Goodman, for the Milagro Collaboration.- Physics potential and first results of the MAGIC telescope E. Aliu et al.- First Results from the H.E.S.S. Cherenkov Telescope System in Namibia M. Raue for the H.E.S.S. Collaboration.- The AMANDA Neutrino Telescope A. Silvestri for the AMANDA Collaboration.- Observation of Very High Energy Gamma Rays from the Remnant of SN 1006 with HEGRA CT1 V. Vitale for HEGRA CT1-Munich group.- Optical Astronomy with Cherenkov telescopes E. de Ona-Wilhelmi et al.- Status of ANITA andANITA-lite A. Silvestri for the ANITA Collaboration.-Optical SETI with MAGIC A. Armada et al.- Part IV: Energetic Particles:from the Heliosphere to the Galaxy and Beyond.- Elemental Composition and Propagation of Cosmic Rays at High Energies D. Mueller.- TeV-scale Gravity: Detecting black holes with cosmic ray air showers Eun-Joo Ahn, M. Cavaglia.- Ultra High Energy Cosmic Rays: Analysis of Directional Correlations with Astrophysical Sources I.C. Maris, P.L. Biermann.- Are Clusters Indicators of Cosmic Ray Anisotropy? A.A. Mikhailov, N.N. Efremov.- Using Cosmic Rays for Monitoring and Forecasting Dangerous Solar Flare Events L.E. Dorman.- The Knee in the Energy Spectrum of Cosmic Rays J.R. Horandel.- The KASCADE-Grande experiment M. Brueggemann et al.- Calibration of the KASCADE-Grande Hadron Calorimeter at an Accelerator S. Plewnia et al.- The AMS experiment A.S. TorrentoCoello.- Solar Neutron Observation at Ground Level and from Space M.R. Moser et al.- Monte Carlo simulations and semianalytical parameterisations of the atmospheric muon flux B. Mitrica et al.- Measurement of the Fluorescence Yield in Air with the AirLight Experiment T. Waldenmaier et al.- Participants.- Index.

The primary scientific mission of the black hole finder probe (BHFP), part of the NASA Beyond Einstein program, is to survey the local Universe for black holes over a wide range of mass and accretion rate. One approach to such a survey is a hard X-ray coded-aperture imaging mission operating in the 10-600 keV energy hand, a spectral range that is considered to be especially useful in the detection of black hole sources. The development of new inorganic scintillator materials provides improved performance (for example, with regards to energy resolution and timing) that is well suited to the BHFP science requirements. Detection planes formed with these materials coupled with a new generation of readout devices represent a major advancement in the performance capabilities of scintillator-based gamma cameras. Here, we discuss the coded aperture survey telescope for energetic radiation (CASTER), a concept that represents a BHFP based on the use of the latest scintillator technology.

Preface M.M. Shapiro. I: High Energy Processes. Theory of Cosmic Ray and High-Energy Gamma-Ray Production in Supernova Remnants E.G. Berezhko. Hadronic Collisions at Very High Energies I. Kurp. Electron Acceleration by Quasi-Parallel Shock Waves Y. Uvarov. Magnetohydrodynamic wind Driven by Cosmic Rays in a Rotating Galaxy V.N. Zirakashvili, et al. II: Sources in our Galaxy. Supernovae, Superbubbles, Nonthermal Emission & Light Element Nucleosynthesis in the Galaxy A.M. Bykov. Cosmic Ray Interactions in the Galactic Center Region P.L. Biermann, et al. Dark Matter Halo of our Galaxy R. Cowsik. A New Model for the Thermal X-Ray Composites and the Proton Origin gamma-Rays from Supernova Remnants O. Petruk. Evolution of Isolated Neutron Stars S. Popov. High Energy Outburst of Recurrent Transient Pulsar A0535+26 T.N. Dorokhova, N.I. Dorokhov. Section III: Extra-Galactic Sources and Cosmological Connections. High Energy Particles in Active Galactic Nuclei P.L. Biermann. Galactic Clues About the High-Energy Processes in BL Lac (AGN) Jets S. Markoff, et al. Nonthermal Phenomena in Clusters of Galaxies Y. Rephaeli. Correlation and Clustering: Statistical Properties of Galaxy Large Scale Structures F.S. Labini, A. Gabrielli. The Sunyaev-Zeldovich Effect and its Cosmological Significance Y. Rephaeli. IV: Cosmic Photons: X-Rays and gamma-Rays. An Overview on GEV-TEV Gamma Ray Astronomy: Past-Present Future V. Fonseca. A Brief Introduction to the Study of Afterglows of Gamma Ray Bursts R. Cowsik. Searches for TEV gamma-Ray Emission with the Hegra Cherenkov Telescopes N. Gotting, et al. Variables Gamma Ray Sources, 1: Interactionsof Flare Energetic Particles with Solar and Stellar Winds L.I. Dorman. Variables Gamma Ray Sources, 2: Interactions of Galactic Cosmis Rays with Solar and Stellar Winds L.I. Dorman. Comets As X-Ray Objects S. Ibadov. V: Cosmic Ray Particles. Cosmic Ray Origin: General Overview V.S. Ptuskin. Galactic Cosmic Ray Composition: From the Anomalous Component to the Knee M.I. Panasyuk. Low Energy Cosmic Ray Nuclei and Their Propagation in the Galaxy M. Giller. Reacceleration of Galactic Cosmic Rays: Secondary Electron Capture Isotopes Measured by the Cosmic Ray Isotope Spectrometer S.M. Niebur. The Astrophysics of Ultra-Heavy Galactic Cosmic Rays (And How We Can Detect Them) J.T. Link. EAS:N -- Ne Measurements with the EAS-Top Array S. Valchierotti. L3+Cosmics: An Atmospheric Muon Experiment at Cern T. Chiarusi. VI: Future Prospects. Nuclear Paleoastrophysics: Prospects and Perspectives G. Kocharov, et al. H.E.S.S. -- The High Energy Stereoscopic System I. Jung. Development of Atmospheric Cherenkov Detectors at Milagro R. Atkins. Nemo: Neutrino Mediterranean Observatory G. Riccobene. Subject Index. Participants.

ACCESS—Advanced Cosmic-ray Composition Experiment for Space Station—was selected as a new Mission Concept under NRA 96-OSS-03, with the goal of combining calorimeter and transition radiation techniques to provide measurements of cosmic rays from Hydrogen through Nickel up to energies approaching the “knee” in the cosmic ray all particle spectrum, plus providing measurements of the Z>28 (Ultra-Heavy) nuclei at all energies. An instrument to perform such an investigation is undergoing an ISS/STS Accommodation Study at JSC. The instrument concept, the mission plan, and the accommodation issues for an ISS attached payload which include, in part, the carrier, ISS Site, thermal control, power, data and operations are described and the current status of these issues, for an ACCESS Mission, is summarized.

The observed spectrum of ultra-high energy cosmic rays virtually guarantees the presence of ultra-high energy neutrinos due to their interaction with the cosmic microwave background. Every one of these neutrinos will point back to its source and, unlike cosmic rays, will arrive at the Earth unattenuated, from sources perhaps as distant as z =20. The neutrino telescopes currently under construction, should discover a handful of these events, probably too few for detailed study. In this talk I will describe how an array of VHF and UHF antennas embedded in a large salt dome, SalSA (Saltdome Shower Array) promises to yield a teraton detector (> 500 km3-sr) for contained neutrino events with energies above 1017 eV. Our simulations show that such a detector may observe several hundreds of these neutrinos over its lifetime. Our simulations also show how such interactions will provide high energy physicists with an energy frontier for weak interactions an order-of-magnitude larger than that of the LHC. The flavor ID capalities of SALSA, combined with the extreme L/E of these neutrinos, will provide a window on neutrino oscillations and decay times eight orders of magnitude higher than laboratory experiments. In addition to the latest simulation results, we describe progress on detectors and site selection.

The ratios of fluxes of heavy nuclei from sulfur (Z=16) to chromium (Z=24) to the flux of iron were measured by the ATIC-2 experiment. The ratios are decreasing functions of energy from 5 GeV/n to approximately 80 GeV/n, as expected. However, an unexpected sharp upturn in the ratios are observed for energies above 100 GeV/n for all elements from Z=16 to Z=24. Similar upturn but with lower amplitude was also discovered in the ATIC-2 data for the ratio of fluxes of abundant even nuclei (C, O, Ne, Mg, Si) to the flux of iron. Therefore the spectrum of iron is significantly different from the spectra of other abundant even nuclei., Comment: 4 pages, LaTeX2e, a paper for 23rd European Cosmic Ray Symposium (2012)

A new balloon instrument, the advanced thin ionization calorimeter (ATIC), is currently under development by an international collaboration involving researchers in the U.S., Germany, Korea, Russia and the Ukraine. The instrument will be used, in a series of long duration balloon flights, to investigate the charge composition and energy spectra of primary cosmic rays over the energy range from about 1010 to 1014 eV. The ATIC instrument is designed around a new technology, fully active Bismuth Germanate (BGO) ionization calorimeter that is used to measure the energy deposited by the cascades formed by particles interacting in an approximately 1 proton interaction length thick carbon target. The charge module comprises a highly segmented, triply redundant set of detectors (scintillator, silicon matrix and Cherenkov) that together give good incident charge resolution plus rejection of the 'backscattered' particles from the interaction. Trajectory information is obtained both from scintillator layers and from the cascade profile throughout the BGO calorimeter. This instrument is specifically designed to take advantage of the existing NASA long duration balloon flight capability in Antarctica and/or the Northern Hemisphere. The ATIC instrumentation is presented here, while a companion paper at this conference discusses the expected performance.© (1996) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Geomagnetically trapped helium nuclei, at high energy (∼40–100 MeV/nucleon), have been measured by the ONR‐604 instrument during the 1990/1991 CRRES mission. The ONR‐604 instrument resolved the isotopes of helium with a mass resolution of 0.1 amu. The energetic helium observed at L

I Cosmic Gamma Rays, X-Rays, and Neutrinos: The Sky as Viewed from the Compton Gamma-Ray Observatory, G. Kanbach Cosmic Gamma-Ray Bursts, M. Baring Gamma-Ray Production in the Winds of Wolf-Rayet Stars, P.J. Meintjes, G. Kanbach Origin of High-Energy X-Ray Emission from NGC 253, O. Goldshmidt Spectral and Temporal Variability in Low-Mass X-Ray Binaries, N.D. Kylafis Solar and Supernova Neutrinos, T. Stanev Neutrino Masses in Astrophysics, R. Gandhi. II Cosmic Rays: Source Composition of Cosmic Rays and Models of Origin, R. Silberberg, C.H. Tsao, M.M. Shapiro Some Highlights of the 1993 International Cosmic Ray Conference, R. Silberberg, C.H. Tsao Recent Results from the Fly's Eye Experiment, D.J. Bird, et al The High Resolution (Hi-Res) Fly's Eye Detector, D.J. Bird The Hegra Experiment at La Palma, V. Fonseca The Extensive Air-Shower Experiment in Tibet, M. Nishizawa Production and Acceleration of Ultra-High-Energy Particles by Black Holes and Strings, C. Sivaram Cosmic-Ray Nonlinear Effects in Space Plasma: General Characteristics and Dynamic Galactic Halo Dynamic Heliosphere, L.I. Dorman Pulsars and Supernova Remnants Pulsars - Recent Results on their Physics and their Dynamics, F.G. Smith Synchrotron and Inverse Compton Processes in Supernova Remnants, O.C. de Jager Cosmology - The Big Bang and the Infrared Sky as Seen by COBE, J.C. Mather Inflation, the Top, and All That, Y. Ne'eman Formation of Galaxies in a Dark-Matter Dominated Universe - a New Approach, P.G. Macedo, J.P.M. de Carvalho New Ways in Cosmology - Friedmann-Lemaitre Model Derived from the Lyman-Alpha Forest in Quasar Spectra Alternative Models for the Very Early Universe, H.J. Blome, W. Priester, J. Hoell.

A new program is being considered by the U.S. National Aeronautics and Space Administration to investigate the galactic origin and the acceleration limit of cosmic rays by supernova remnants. This program would provide a direct test of the proposal that the bulk of galactic cosmic rays are accelerated by the blast waves of supernovae, through the same shock acceleration processes that operate in the heliosphere. NASA’s new long duration balloon capability will be used to carry out a series of flights, using proven detector technology, to measure the composition of cosmic rays from 1013 to 1015 eV, beyond the maximum energy to which supernova remnants should be capable of accelerating cosmic ray protons. In addition to providing a test of the standard model for cosmic ray origin and acceleration, this study would achieve and important overlap with ground‐based air‐shower measurements from 1014 to 1016 eV, allowing the air shower studies to extend the composition beyond the so‐called ‘‘knee’’ in the cosmic ...

Part I: Cosmic Rays. Composition, Propagation and Reacceleration of Cosmic Rays R. Silberberg, C.H. Tsao, J.R. Letaw. Continuous Reacceleration of Cosmic Rays in Galaxies M. Pohl. Cosmic Ray Composition at and above the Knee T. Stanev. Cosmic Rays of the Highest Energies X Chi, J. Wdowczyk, A.W Wolfendale. High Energy Cosmic Rays from Cores of Active Galactic Nuclei R.J. Protheroe, A.P Szabo. Part II: Neutrinos, Gamma Rays, X-Rays and Muons. Neutrino and Gamma-Ray Astrophysics R. Silberberg, M.M. Shapiro, C.H. Starr. Point Sources of TEV and PEV Cosmic Gamma Rays E.J. Fenyves. A Search for Radiative Neutrino Decay from Supernovae R.S. Miller, R.C. Svoboda. Recent Progress in Understanding of X-Ray Pulsars D.A. Leahy. Simultaneous Air Shower and Deep Muon Observations at Soudan W.W.M. Allison, et al. Part III: Cosmology. Nucleosynthesis in the Early Universe W.A. Fowler. The Age of the Observable Universe W.A. Fowler. An Inflationary Primer J.W Burton. Fluctuations in the Cosmic Background Radiation M. Giller, A.W Wolfendale.

This program was established for the purpose of studying projectile fragmentation; (1) as a function of energy, focusing first on the intermediate energy region, < 1 GeV/nucleon, where there have been few previous measurements and no systematic studies, and (2) as a function of projectile mass, starting with light beams and proceeding to species as heavy as nickel (and possibly beyond). The intermediate energy region is important as the transition between the lower energy data, where the interaction appears to be dominated by collective effects and the decay of excited nuclei, and the highest energy results, where nucleon-nucleon interactions are fundamental, limiting fragmentation'' applies, and the nucleus may well break-up before any de-excitation. The mass dependence of projectile fragmentation is largely unknown since most detailed work has involved light ion beams. Nuclear structure effects, for example, may well be quite prominent for heavier beams. Furthermore, the nuclear excitation functions for the production of different fragment isotopes have immediate application to the astrophysical interpretation of existing isotopic datasets obtained from balloon and satellite measurements of galactic cosmic rays.

We have proposed CALET (CALorimetric Electron Telescope) mission to make observations of high energy cosmic rays, electrons, gamma-rays, and nuclei, on the International Space Station (ISS). CALET mission has been approved as one of candidates for the next mission utilizing the Japanese Experiment Module (JEM). The detector of CALET consists of an imaging calorimeter (IMC) and a total absorption calorimeter (TASC). Main objective of cosmic-ray observation with CALET is to determine precise energy spectrum of electrons up to 20 TeV. As the super nova remnants (SNR) are taken to be sources of electrons, some structure caused by nearby electron sources is expected to appear in the energy spectrum over 1 TeV. Gamma-rays from 20 MeV to a few TeV can be also observed by CALET. Because a thick TASC of CALET gives high energy resolution, annihilation line of SUSY particle, which is a candidate of the dark matter, can be detected. Observation of nuclei is also possible up to 1000 TeV owing to the thick TASC. We have been going on conceptual design of CALET to clear a next judgment in one or two years to proceed to practical development for launching in 2013.

The relative abundances of elements and/or isotopes in the cosmic radiation are the source of information on both the sites of cosmic ray origin and acceleration and the conditions in the interstellar medium through which the particles travel. Recent (1988–90) measurements and interpretations have provided new information on cosmic ray composition and source abundances. These new results are described and compared to previous work.