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David Seckel (University of Delaware)09/06/2014, 09:00Mon AM I - Welcome
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Prof. Francis Halzen (University of Wisconsin-Madison)09/06/2014, 09:10Mon AM I - Welcome
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Prof. Kara Hoffman (o=umd,ou=Institutions,dc=icecube,dc=wisc,dc=edu)09/06/2014, 09:50Mon AM I - Welcome
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Prof. Nikolay Budnev (Irkutsk State University)09/06/2014, 10:50Mon AM II - Acoustic
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Dr Robert Lahmann (Erlangen Centre for Astroparticle Physics)09/06/2014, 11:15Mon AM II - AcousticThe technique of acoustic neutrino detection is a promising approach for future large-scale ultra-high-energy neutrino detectors in water. To investigate this technique in the deep sea, the AMADEUS system has been integrated into the ANTARES neutrino telescope in the Mediterranean Sea. Installed at a depth of more than 2000m, the 36 acoustic sensors of AMADEUS are based on piezo-ceramics...Go to contribution page
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Mr Dominik Kiessling (Erlangen Centre for Astroparticle Physics)09/06/2014, 11:40Mon AM II - AcousticAcoustic neutrino detection is a promising approach to extend the energy range of neutrino telescopes to energies beyond 10^{18} eV. Current water-Cherenkov-neutrino-telescopes, like e.g. KM3NeT, include acoustical sensors in addition to the optical ones. While the main purpose of these acoustic sensors is the position calibration of the detection units, they could be used as instruments for...Go to contribution page
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Prof. Sean Danaher (Northumbria University)09/06/2014, 12:00Mon AM II - AcousticRecent developments in the construction of a line array projector for the calibration of Acoustic Neutrino TelescopesGo to contribution page
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Dr Robert Lahmann (Erlangen Centre for Astroparticle Physics)09/06/2014, 12:20Mon AM II - AcousticTo survey large volumes of water for acoustic signals from neutrino interactions, optical fiber-based hydrophones could potentially have several advantages over conventional hydrophones based on piezo ceramics. Optical fibers form a natural way to create a distributed sensing system in which several sensors are attached to a single fiber. The detection system in this case will consist of...Go to contribution page
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Prof. Alvarez-Muniz Jaime (Dept, of Particle Physics, Univ. of Santiago de Compostela, Spain)09/06/2014, 14:10Mon PM I - Emission Theory & ModelingI will review the current understanding of radio emission from particle showers in both dense dielectric media and the atmosphere. A net charge is generated in those showers due to the Askaryan effect in dense media, and to Askaryan as well as geomagnetic effects in air. I will discuss macroscopic and microscopic approaches to model the emitted radiation. The prominent role of shock wave...Go to contribution page
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Katharine Mulrey (University of Delaware)09/06/2014, 14:50Mon PM I - Emission Theory & ModelingGeomagnetic radiation from air showers is an attractive technique for detecting ultra-high energy cosmic rays. Macroscopic and microscopic models have been developed which qualitatively agree with field observations. A controlled laboratory experiment at the Stanford Linear Accelerator Center (SLAC) was designed to test these models. The experiment measures the radio frequency emission from...Go to contribution page
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Anne Zilles (KIT)09/06/2014, 15:15Mon PM I - Emission Theory & ModelingThe SLAC T-510 experiment was designed to reproduce the physics of radio emission from air showers in a controlled lab experiment with the goal to test established formalisms for simulation of radio emission physics: the “end-point" formalism and the "ZHS" formalism. Simulation results derived with these formalisms can be explained by a superposition of magnetically induced transverse current...Go to contribution page
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Prof. Olaf Scholten (KVI-CART, Univ. of Groningen)09/06/2014, 15:35Mon PM I - Emission Theory & ModelingWith the LOFAR antenna array we have measured the the polarization footprint of the radio emission from extensive air showers for a large number of single events. The polarization direction is determined from the Stokes parameters integrated over the time duration of the radio pulse. It will be shown that for events for which no thunderstorm activity has been registered the polarization...Go to contribution page
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Prof. Jaime Alvarez-Muniz (Univ. Santiago de Compostela, Spain)09/06/2014, 16:30Monday PM II - Emission Modeling & ExperimentThe radiation emitted by atmospheric showers is currently interpreted in terms of the deviation of the charged particles in the magnetic field of the Earth and the emission due to the charge excess (Askary'an effect). Each of these mechanisms has a distinctive polarization. The complex signal patterns obtained both in dedicated experiments measuring average behaviors and in simulations, can be...Go to contribution page
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Dr Frank Schröder (Karlsruhe Institute of Technology (KIT))09/06/2014, 16:50Monday PM II - Emission Modeling & ExperimentWe investigated the radio wavefront of cosmic-ray air showers with LOPES measurements and CoREAS simulations: the wavefront is of hyperbolic shape and can be used to reconstruct the shower maximum. LOPES was a digital, interferometric antenna array at the Karlsruhe Institute of Technology (KIT) at an altitude of 110 m. LOPES consisted of up to 30 antennas on an area with approximately 200 m...Go to contribution page
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Prof. Enrique Zas (Univ. of Santiago de Compostela, Spain)09/06/2014, 17:10Monday PM II - Emission Modeling & ExperimentThe recent detection of radio pulses with the ANITA experiment has revealed characteristic signatures of geomagnetic emission and has been attributed to coherent radio flashes from air showers that get reflected on the ice cap. In spite of recent progress in simulating and understanding radio pulses from air showers, no detailed studies are available to date to address the impact of the...Go to contribution page
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Jessica Stockham (University of Kansas)09/06/2014, 17:30Monday PM II - Emission Modeling & ExperimentFor radio antenna neutrino and cosmic ray detectors located in or above the Antarctic ice sheet, the reconstruction of both ultra-high energy (UHE) neutrino and cosmic ray air shower events requires knowledge the transmission and reflection properties of the air-ice interface. To better understand these properties, in-lab and field data will be obtained and analyzed. The in-lab experiment will...Go to contribution page
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Dr Tim Huege (Karlsruhe Institute of Technology)10/06/2014, 08:30Tues AM I - Air Shower Main ExperimentOver the past decade, radio detection of cosmic rays has matured from small-scale prototype experiments to installations spanning several km^2 with more than a hundred antennas. The physics of the radio signal is well understood and simulations and measurements are in good agreement. We have learned how to extract important cosmic ray parameters such as the geometry of the air shower and...Go to contribution page
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Mr Lilian Martin (SUBATECH)10/06/2014, 09:10Tues AM I - Air Shower Main ExperimentCODALEMA is the last experiment currently running in Europe dedicated to the extensive air shower detection using the observation of its induced radio electric field and with the ambition to promote this radio detection technique to a mature technology suited to a next generation giant cosmic ray observatory. The latest experimental upgrade of CODALEMA consisting in a large array of autonomous...Go to contribution page
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Joerg Hoerandel (Radboud University Nijmegen)10/06/2014, 09:40Tues AM I - Air Shower Main ExperimentHigh-energy cosmic rays impinging onto the atmosphere of the Earth initiate cascades of secondary particles: extensive air showers. The electrons and positrons in air showers interact with the geomagnetic field and emit radiation, which we record in the tens-of-MHz regime. The LOFAR radio telescope measures the radio emission with high antenna density and two polarization directions. We used...Go to contribution page
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Mr Jens Neuser (University of Wuppertal)10/06/2014, 10:10Tues AM I - Air Shower Main ExperimentThe Auger Engineering Radio Array (AERA) at the Pierre Auger Observatory in Argentinia is constructed in multiple stages starting in 2010. The current stage consists of 124 dual-polarized radio detector stations covering an area of 6 km^2. One of the main goals is to study the radio emission process for energies beyond 10^{17} eV in the range from 30-80 MHz. Having the unique opportunity for...Go to contribution page
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Ms Yuliya Kazarina (Physical faculty, Irkutsk State University, Irkutsk, Russian Federation)10/06/2014, 11:10Tues AM II - Air Shower ExperimentThe Tunka-Rex experiment (Tunka Radio Extension) was created in 2012 at the Tunka Valley (Republic of Buryatia, Russia). Its purpose is to investigate methods for the energy spectrum and the mass composition of high energy cosmic rays based on the radio emission of air showers. Tunka-Rex is an array of 25 radio antennas distributed over an area of 3 km2. The most important feature of the...Go to contribution page
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Felix Werner (KIT)10/06/2014, 11:40Tues AM II - Air Shower ExperimentMicrowave radiation from high-energy air showers has been observed in the C band (3.4–4.2 GHz) with the Cosmic-Ray Observation via Microwave Emission (CROME) setup. The obtained dataset provides a unique opportunity to study the radio emission of air showers at microwave frequencies. The compatibility of the measured GHz signals with different hypotheses for the emission mechanism is...Go to contribution page
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Dr Imen Al Samarai (IPNO)10/06/2014, 12:10Tues AM II - Air Shower ExperimentObservations of microwave radiation emitted by low energy electrons left after the passage of a high energy electron beam in accelerator experiments offered new possibilities of Ultra High Energy Cosmic Rays (UHECR) detection techniques based on microwave radiation. This would bring a tenfold increase in detector duty cycle compared to the standard fluorescence technique. The emission...Go to contribution page
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Mr Benoît REVENU (Subatech)10/06/2014, 12:40Tues AM II - Air Shower ExperimentThe code SELFAS computes the electric field emitted by the secondary electrons and positrons in air showers initiated by high-energy cosmic rays. SELFAS is based on the shower universality. We will focus on the main successes of the code to explain observations in the range MHz-GHz, and we will insist on the signal emitted by the sudden death of air showers when the front disappear in the...Go to contribution page
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10/06/2014, 13:00Pick up at Loews is between 1:15 and 1:30 PM. Guide will meet those who want the group tour at Smithsonian Castle on the Mall side. This tour will end at 5:00 PM. Bus will pick up passengers there and take them to the boat dock - the Dandy Zero on Prince Street in Alexandria, VA. The cruise will run from 6:30 PM to 9:30 PM, and includes dinner. The bus will pick up at the pier around 9:40...Go to contribution page
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Ms Anna Nelles (Radboud University Nijmegen)11/06/2014, 09:00Weds AM I - Air Shower DetailThe detection of radio emission of air showers has rapidly advanced in the past years. New experiments have shed light on the details of the emission and air shower simulations provide rather accurate models of the measured emission. To exploit radio emission in large-scale experiments, a simple and analytic parametrization of the distribution of the radio signal at ground level is needed....Go to contribution page
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Dr Stijn Buitink (Radboud University Nijmegen, Netherlands)11/06/2014, 09:20Weds AM I - Air Shower DetailLOFAR is a multipurpose radio telescope which can be used for radio detection of cosmic rays while running astronomical observations at the same time. In the dense core individual air showers are detected by hundreds of dipole antennas. The raw electromagnetic waveform as detected by each antenna is stored in a five-second ring buffer, which is read out when a trigger is issued by the LORA...Go to contribution page
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Dr Qader Dorosti Hasankiadeh (Karlsruher Institut für Technologie (KIT);)11/06/2014, 09:40Weds AM I - Air Shower DetailThe Auger Engineering Radio Array (AERA) aims to detect extensive air showers caused by the interactions of ultra-high energy cosmic rays with the Earth atmosphere, providing complementary information to the Auger surface, fluorescence and muon detectors. The second stage of AERA, currently consisting of 124 radio stations, has been completed at the Pierre Auger Observatory in early 2013, ...Go to contribution page
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Mrs Olga Kambeitz (IEKP, KIT)11/06/2014, 10:00Weds AM I - Air Shower DetailAERA, the Auger Engineering Radio Array, located at the Pierre Auger Observatory in Malargüe, Argentina measures the radio emission of extensive air showers in the 30-80 MHz frequency range. It consists of 124 antenna stations of which 24 are log periodic dipole antennas (LPDAs) and 100 are so-called butterfly antennas. Both antenna types measure two electric field components (North-South and...Go to contribution page
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Mrs Jennifer Maller (Subatech)11/06/2014, 10:50Weds AM II - Air Shower DetailThe Auger Engineering Radio Array consists of 124 radio stations covering 6 km² installed within the low energy extension of the Pierre Auger Observatory in Argentina; this location allows a multi-hybrid measurement of air-showers with the fluorescence telescopes, the water-Cherenkov and the muon detectors close to the radio array. AERA detects the radio emission from cosmic-ray induced air...Go to contribution page
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Dr Alain Lecacheux (CNRS - Observatoire de Paris), Dr Lilian MARTIN (SUBATECH-UMR6457)11/06/2014, 11:10Weds AM II - Air Shower DetailRadio pulses associated with Extended Air Showers (EAS) produced in terrestrial atmosphere by High Energy Cosmic Rays (UHECR) of energy 10^17 eV and above, are now routinely observed by dedicated radio instruments on ground. This may offer a new and appealing way for elucidating the nature and origin of involved primary particles, an open question still unsolved. Unfortunately, the high...Go to contribution page
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Mr Didier CHARRIER (SUBATECH-UMR6457)11/06/2014, 11:30Weds AM II - Air Shower DetailThe Butterfly antenna is a compact, active and dual polarization antenna specifically developed for the radio detection of extensive air showers in the 20-200MHz frequency range. Butterfly antennas are in operations at Nançay for the CODALEMA experiment since october 2008, and at Auger for the AERA experiment since may 2013. The overall characteristics of an active antenna are given by the...Go to contribution page
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Mr Daniel Huber (KIT), Dr Tim Huege (Karlsruhe Institute of Technology)11/06/2014, 11:50Weds AM II - Air Shower DetailThe LOPES experiment was a radio interferometer built at the existing air shower array KASCADE-Grande in Karlsruhe, Germany. The last configuration of LOPES was called LOPES-3D and consisted of ten tripole antennas. Each of these antennas consisted of three crossed dipoles east-west, north-south and vertically aligned. With this, LOPES-3D had the unique possibility to study the benefits of...Go to contribution page
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Timo Karg (DESY)11/06/2014, 12:10Weds AM II - Air Shower DetailA challenge that is common to many experiments in high-energy astroparticle physics is the need for sparse instrumentation in areas of 100 km2 and above, often in remote and harsh environments. All these arrays have similar requirements for read-out and communication, power generation and distribution, and synchronization. Within the TAXI project we are developing a transportable, modular...Go to contribution page
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Dr Valerio Verzi (Istituto Nazionale Fisica Nucleare)11/06/2014, 14:00Weds PM I - GHZ / MBRThe Air Microwave Yield (AMY) experiment investigate the molecular bremsstrahlung radiation emitted in the GHz regime from an electron beam induced air-shower . The measurements have been performed with 510 MeV electron beam in a wide frequency range between 1 and 20 GHz. We present the apparatus and the results of the tests performed at the Beam Test Facility (BTF) of Frascati INFN...Go to contribution page
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Dr Imen Al Samarai (IPNO)11/06/2014, 14:25Weds PM I - GHZ / MBRA detection technique of Ultra High Energy Cosmic Rays (UHECR) complementary to fluorescence and Radio techniques would be the use of the Molecular Bremsstrahlung Radiation (MBR) emitted by low energy electrons left after the passage of the showers in the atmosphere. The emission mechanism is expected from quasi-elastic collisions of electrons produced in the shower by the ionization of...Go to contribution page
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Mr Philipp Papenbreer (Bergische Universität Wuppertal)11/06/2014, 14:45Weds PM I - GHZ / MBRThe Cosmic-Ray Observation via Microwave Emission (CROME) experiment is designed to study GHz radio emissions from extensive air showers. Multiple radio antennas measure externally triggered by the KASCADE-Grande air-shower array. The experiment is designed to detect a potentially isotropic, unpolarized component as expected by molecular bremsstrahlung emission in the low-energy electron...Go to contribution page
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Mr Lars Petzold (KIT)11/06/2014, 15:05Weds PM I - GHZ / MBRAt the Karlsruhe Institute of Technology (KIT) the microwave detector experiment CROME (Cosmic Ray Observation via Microwave Emission) has been built up. It was aimed to investigate radio emissions from cosmic ray air showers in L-Band (1.0 to 1.6 GHz) and the extended C-Band (3.4 to 4.2 GHz). The final setup used high-gain parabolic reflector-type antennas which are illuminated either with...Go to contribution page
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Prof. Olaf Scholten (KVI-CART, Univ. of Groningen)11/06/2014, 15:55Weds PM II - Lunar
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Dr Clancy James (University of Erlangen-Nuernberg)11/06/2014, 16:35Weds PM II - LunarThe effects of lunar surface roughness, on both small and large scales, on Askaryan radio pulses generated by particle cascades beneath the lunar surface has never been fully estimated. Surface roughness affects the chances of a pulse escaping the lunar surface, its coherency, and the characteristic detection geometry. It will affect the expected signal shape, the relative utility of different...Go to contribution page
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Dr Timothy Miller (Johns Hopkins University Applied Physics Lab)11/06/2014, 16:55Weds PM II - LunarWe describe a potential confluence between EeV neutrino detection and planetary science: a concept for an instrument to measure the thickness of the ice shell on a planetary body, such as Jupiter’s moon Europa or Saturn’s moon Enceladus, by making use of the Askaryan Effect RF signal from EHE neutrinos observed from an orbiting spacecraft. Unlike a large high powered active device, i.e., an...Go to contribution page
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Krijn de Vries (VUB)11/06/2014, 17:15Weds PM II - LunarWe discuss the radar detection technique for the detection of high-energy neutrino-induced particle cascades in ice. A high-energy neutrino interacting in ice will induce a particle cascade. When propagating through the ice, this cascade will ionize the medium producing a plasma. The different properties of this ionization plasma, such as its size and lifetime, will be discussed to determine...Go to contribution page
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Mr Samridha Kunwar (The University of Kansas)11/06/2014, 17:35Weds PM II - LunarThe detection of high – energy cosmic rays is currently limited by the rarity of the most interesting rays striking Earth. We describe the development of an observatory based on a remote sensing technique known as bi-static radar, that aims to achieve remote coverage over large portions of the Earth's surface. The radar project's receiver and transmitter stations have already been functional...Go to contribution page
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Dr Carl Pfendner (Ohio State University)12/06/2014, 08:30Thurs AM I - In-Ice Neutrino MainThe Askaryan Radio Array (ARA) is an ultra-high energy (UHE) cosmic neutrino detector located at the South Pole. The cosmic ray flux cut off above primary energies of 10^19.5 eV leads us to expect a UHE neutrino flux due to the GZK effect. The detection of these UHE cosmic neutrinos will add to the understanding of the sources and physics of UHE cosmic rays. ARA uses the radio Cherenkov...Go to contribution page
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Keith Bechtol (KICP, University of Chicago)12/06/2014, 09:00Thurs AM I - In-Ice Neutrino MainThe goal of the proposed Greenland Neutrino Observatory (GNO) is to discover and study ultra-high energy neutrinos by looking for radio emission from particle cascades induced by these neutrinos in the Greenland ice sheet. GNO will consist of an array of radio antenna stations deployed near Summit Station in central Greenland, sitting atop a 3 km deep ice sheet. Preliminary analysis of field...Go to contribution page
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Dr Corey Reed (UC Irvine)12/06/2014, 09:30Thurs AM I - In-Ice Neutrino MainThe ARIANNA experiment uses low noise, low power and inexpensive technology to search for radio pulses emitted by extremely high energy cosmic neutrino interactions. Three detector stations have been deployed in the Ross Ice Shelf of Antarctica, taking both environmental as well as radio pulse data. The stations are powered by solar and wind generators and transfer data north via...Go to contribution page
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David Seckel (University of Delaware)12/06/2014, 10:00Thurs AM I - In-Ice Neutrino MainA review of the instrument and science program is given, including the status of reanalysis of the cosmic ray events detected by the ANITA-I payload, and plans for ANITA-III.Go to contribution page
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Dr Andrew Romero-Wolf (Jet Propulsion Laboratory)12/06/2014, 10:50Thurs AM II - In-Ice Neutrino DetailInterferometric techniques are widely applied for a variety of radio detectors ranging from cosmology (redshifted 21 cm line and cosmic microwave background), radio astronomy (astrometry, imaging, and transient detection), and lightning. We present an interferometric technique for the reconstruction of ultra-wide band impulsive signals from ultra-high energy particles. This highly sensitive...Go to contribution page
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Thomas Meures (o=ulb,ou=Institutions,dc=icecube,dc=wisc,dc=edu)12/06/2014, 11:30Thurs AM II - In-Ice Neutrino DetailThe Askaryan Radio Array (ARA) is one of the future neutrino observatories focusing on the detection of GZK-neutrinos with energies beyond 1017eV through secondary radio waves. Observing GZK-neutrinos is especially interesting because it is one of the few ways to investigate the CR-spectrum beyond the observed GZK-cutoff. These neutrinos, when reaching the earth, produce particle cascades in...Go to contribution page
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Prof. Keiichi Mase (Chiba University)12/06/2014, 11:50Thurs AM II - In-Ice Neutrino DetailCoherent Cherenkov radio emissions from particle cascades were predicted by Askaryan, and the emissions were firstly detected at SLAC from the electro-magnetic cascades. Askaryan Radio Array (ARA) is being built at the South Pole to observe cosmogenic neutrinos by detecting the coherent radio emissions with the large instrumental area of about 100 km^2. We are planning an end to end...Go to contribution page
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Mr Mark Stockham (University of Kansas)12/06/2014, 12:10Thurs AM II - In-Ice Neutrino DetailAntarctic ice represents the interaction volume for multiple UHE neutrino experiments. When neutrinos collide with ice particles they produce radio waves that propagate to in-ice, surface, or balloon-borne detectors. The radio frequency signal strength observed at the detector, however, depends on the radio frequency attenuation length of the ice through which the neutrino-generated signal...Go to contribution page
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Rolf Nahnhauer (DESY)12/06/2014, 12:30Thurs AM II - In-Ice Neutrino DetailInformation about thermal probes and how to use them for autonomous deep drilling in ice will be given. The method presented may be useful for drilling holes at large distances and/or large numbers, necessary for building big (hybrid) arrays for cosmogenic neutrino detection.Go to contribution page
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