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Jackie Davies (RAL Space)Since the launch of the STEREO spacecraft, a plethora of techniques have been developed to investigate the three-dimensional kinematics of solar transients, such as Coronal Mass Ejections (CMEs), from their signatures in imaging observations. These techniques, which range from the highly complex and computationally intensive forward modelling method to methods based on simple curve fitting,...Go to contribution page
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Mr julio Cesar Mejia-Ambriz (MEXART, UNAM)The Mexican Array Radio Telescope (MEXART) is a transit station to perform IPS observations at 140 MHz. The antenna is a matricial array of dipoles covering a collecting area of about 10,000 square meters. Previously, we reported the first MEXART IPS observations (Mejia, et al. 2010) employing a quarter of the total array. At this moment we are performing observations with an half of the total...Go to contribution page
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Noe Lugaz (Institute for Astronomy)In this talk, I will review different methods to determine a CME direction and velocity from single and multiple spacecraft remote-sensing observations. I will discuss why the assumptions of constant speed and directions and very narrow CMEs have been successful so far and why this may change in the near future as the STEREO spacecraft move farther apart. I will finally discuss the case of...Go to contribution page
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Sergei Tyul'bashev (Pushchino Radio Astronomy Observatory)Since 2006 IPS observations are carried out using 16-beams Big Scanning Array of Lebedev Physical Institute in monitoring regime. All the sources with scintillating flux greater than 0.2 Jy are recorded daily at the frequency 111MHz during 24 hours in the sky strip of 8o width in declination. Methods of observations and data processing are briefly discussed. Results are presented showing the...Go to contribution page
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Dr Timothy Howard (SWRI, Boulder, CO, USA)Heliospheric imaging has evolved considerably since the early days of SMEI in 2003. Progress has been made from two directions: improving the quality of the data themselves; and developing techniques to exploit the geometry and Thomson scattering physics. Through the former we have improved noise reduction and enabled the detection of smaller and fainter transients and through the latter we...Go to contribution page
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Ms Justyna M. Sokół (Space Research Centre PAS), Dr Maciej Bzowski (Space Research Centre PAS)In the first portion of the talk, given on behalf of the IBEX Science Team, we will present observations of Energetic Neutral Atoms from the heliospheric interface region and beyond performed by the Interstellar Boundary Explorer (IBEX) spacecraft. In addition to the expected signal from the heliospheric interface, IBEX discovered an arc-like, persistent Ribbon of enhanced ENA emissiona in all...Go to contribution page
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Dr Richard Fallows (Aberystwyth University)The LOw Frequency ARray (LOFAR) is a new array of radio telescopes centred on the Netherlands with additional stations across Europe. Designed to operate at frequencies from 10 to 250MHz, it is one of a new generation of "software telescopes". Currently, it is in the latter stages of the commissioning phase and a wide variety of scientific experiments are in testing mode. Measurement of...Go to contribution page
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Dr Mario M. Bisi (Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive #0424, La Jolla, CA 92093-0424 USA / Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus, Aberystwyth, Ceredigion, SY23 3BZ, Wales, UK)General contributions throughout the workshop as and when necessary including brief updates on the UCSD tomography routines, use of EISCAT/ESR/MERLIN/LOFAR for observations of IPS, future aspirations for obersations of IPS, and other relevant topics of discussion.Go to contribution page
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Prof. Mike Hapgood (RAL Space)Interplanetary scintillation (IPS) is one of several techniques that can track density structures propagating out from the Sun. Thus it is potentially an important space weather activity that can help to predict the onset of geomagnetic storms. That potential was recognized over twenty years ago, when a joint UK-US project sought to use the Cambridge IPS array to develop an operational system...Go to contribution page
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Dr Americo Gonzalez-Esparza (MEXART, UNAM)The Mexican Array Radio Telescope (MEXART) consists of a 64x64 (4096) full-wavelength dipole antenna array, operating at 140 MHz, with a bandwidth of 2 MHz, occupying about 9,660 square meters (69m x 140m) (http://www.mexart.unam.mx). This is a dedicated radio array for Interplanetary Scintillation (IPS) observations located at: latitude 19 degrees 48' N, longitude 101 degrees 41' W. We...Go to contribution page
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Dr Elizabeth Jensen (Planetary Science Institute)A complex solar eruption occurred at the beginning of August 2010 releasing a disappearing filament and a halo CME on an Earthward trajectory from Region 1092. The first ICME arrived on August 3rd followed by a second stronger ICME on the 4th; both were traveling at approximately a factor of 2 greater than the surrounding solar wind. The CMEs triggered a G2-class geomagnetic storm. We...Go to contribution page
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Ernesto Aguilar-Rodriguez (Instituto de Geofisica, UNAM)Interplanetary Type II radio burst radiation results from the excitation of plasma waves in the ambient medium by a coronal mass ejection (CME) driven shock, propagating outward from the Sun. Hence, these radio emissions provide a means of remotely tracking CME/shocks. The aim of this work is to present an analysis on the Type II radio bursts observed by Wind/WAVES and STEREO/SWAVES radio...Go to contribution page
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Igor Chashey (Pushchino Radio Astronomy Observatory)Big Scanning Array of Lebedev Physical Institute (BSA LPI) Radiotelescope has operating frequency 111 MHz and two independent 16 beams systems, each of them covering strip of the sky of about 8o width in declination. Since 2006 one of the beams systems is used for IPS observations in monitoring regime. In the present state several hundred of scintillating radio sources is observed during 24...Go to contribution page
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Dr Xing Li (IMAPS, Aberystwyth University)The solar wind electric and magnetic field data from Cluster spacecraft is analysed to investigate the behaviour of the turbulence dissipation range. The dependence of both electric and magnetic field power spectra on wave number k can be categorised as several power laws: at relatively low wave number, the power index is about -5/3 indicating a turbulence inertial range. Beyond an inertial...Go to contribution page
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Dr Elizabeth Jensen (Planetary Science Institute)On November 9, 2009, during the longest solar minimum in a century, the MESSENGER spacecraft en route to Mercury was in superior conjunction allowing the acquisition of Faraday rotation measurements. At 1.66 solar radii (456 Mm from the surface) on November 8th, MESSENGER's 8GHz radio frequency signal was absorbed. The observations taken on November 8th, 10th, and 11th show a 5 minute...Go to contribution page
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Dr Mario M. Bisi (CASS, UCSD / IMAPS, Aberystwyth University)Observations and modelling of the solar wind in the inner heliosphere via remote-sensing methods and data are of a critical importance to improving our understanding of the physics behind the origin and development of the solar wind, transients, and the various interactions which take place throughout the inner heliosphere. They are also essential to further our understanding of space weather...Go to contribution page
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Prof. Richard Harrison (RAL)August 2010 saw the first major activity of the new cycle. SDO observations of a complex series of events over an extended region of the solar atmosphere heralded the onset of a uniquely complete dataset of observations from many spacecraft, tracing multiple CME events from Sun to Earth and recording the impacts at the Earth. Central to this were the STEREO observations from out of the...Go to contribution page
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Dr Ian McCrea (RAL Space)This talk will cover the progress of EISCAT_3D development, its implementation, and also its capabilities for use in space weather and as a future remote-sensing instrument.Go to contribution page
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Prof. Mike Hapgood (RAL Space)This paper will explore at a conceptual level how the tracking of heliospheric transients (coronal mass ejections and co-rotating interaction regions) can lead to novel space weather services that can mitigate impacts on power grids, satellite navigation and timing systems, HF radio communications and spacecraft. The aim is to go beyond the usual bland statements about space weather impacts...Go to contribution page
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John Clover (CASS/UCSD)The University of California, San Diego (UCSD) time-dependent tomography program has been used successfully since the beginning of the year 2000 to remotely sense and forecast interplanetary scintillation (IPS) observations of coronal mass ejections. More recently this program has been adapted to provide forecasts of heliospheric density using Thomson-scattered data from the Solar Mass...Go to contribution page
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Dr Kenichi Fujiki (STELab., Nagoya Univ.)Interplanetary scintillation (IPS) is a phenomenon that is unique and allows one to measure solar wind velocities over a wide spatial range of interplanetary space where in-situ measurements are impossible or difficult. We have been observing the solar wind velocity structure using a multi-station IPS facility (327 MHz) at Solar-Terrestrial Environment Laboratory in Japan (STELab-IPS) since...Go to contribution page
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Dr Mario M. Bisi (Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive #0424, La Jolla, CA 92093-0424 USA / Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus, Aberystwyth, Ceredigion, SY23 3BZ, Wales, UK)A brief introduction to Aberystwyth and to the workshop.Go to contribution page
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Dr Mario Bisi (Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus)We present “PERSEUS”, a Pegasus Explorer for Remote SEnsing and in-sitU Space science. PERSEUS instruments work together to provide all sky coverage that enables mapping and 3D reconstruction of the global heliosphere. A coronagraph (CRG) observes rapidly-changing material flow and events (CME’s) near the solar surface while all-sky visible-light imagers (ASIs) observe light from these same...Go to contribution page
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