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Joint Space Summer Camp Program

July 22 - August 18, 2013

The University of Alabama in Huntsville German Aerospace Center (DLR) The University of Rostock

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Table of Contents

Welcome……………………………………………………………………………..4

Schedules

Schedule in Huntsville………………………………………………………..5

Schedule in Neustrelitz……………………………………………………….7

Space Weather Summer Camp in Huntsville

Abstracts……………………………………………………………………..10

Project Work…………………………………………………………………23

Space Weather Summer Camp in Neustrelitz

Abstracts……………………………………………………………………..25

Project Work…………………………………………………………………37

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Welcome to the Joint Space Weather Summer Camp 2013

The Joint Space Weather Summer Camp is a partnership between UAHuntsville, the DLR and the University of Rostock. Because of the considerable historical ties between Huntsville and the state of Mecklenburg Vorpommern (Germany) in the development of , missiles, and eventually manned space flight, the Joint Space Weather Summer Camp was created to forge ties and develop communication between these two regions that have had such an impact on the 20th century.

During the 4 week series of lectures, hands-on projects, experiments, and excursions you will be given an understanding of both the theoretical underpinnings and practical appli- cations of Space Weather and solar and . During the first two weeks in Huntsville, we begin by focusing on the as the primary cause of space weather in the entire , and discuss fundamental processes in physics, the solar and the interaction processes between the and ’s upper atmosphere.There will also be the opportunity to participate in either data or practical-based project work, enabling you to gain a practical understanding of the top- ics that will be discussed in the lectures both in Huntsville and in Germany. During the last two weeks in Northern Germany we will focus on the upper atmosphere and .Besides the lectures there will also be practical project work and we will visit the University of Rostock and the Leibniz-Institute of e.V. at the University of Rostock (IAP) in Kühlungsborn.

The Joint Space Weather Summer Camp is much more than just lectures, projects and experiments. It also provides a wonderful opportunity for cultural exchanges between the US and Germany in an academic setting. The visit of the ‘Historical Technical Museum in Peenemünde’ in the Northeast of Germany or the visit of the US Space and Center in Huntsville, USA, are just two further examples of a program that goes beyond.

We hope that the Joint Space Weather Summer Camp will be an interesting introduction to the theoretical and practical aspects of Space Weather combined with a cultural ex- change between the US and Germany!

The Joint Space Weather Summer Camp 2013 Committee Joint Space Weather Space Joint Summer Camp

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Joint Space Weather Summer Camp

July 22 – August 3, 2013 in Huntsville

Monday, July 22 Modeling of Magnetic Non-Potentiality of an Active Region Using a Three-Dimensional, Data Driven Active ______Region Evolution Model

Universal Basic Processes S. T. Wu in Plasma Physics CSPAR The University of Alabama in Huntsville Jakobus LeRoux CSPAR, One of the major interesting problems for The University of Alabama in Huntsville space weather forecasting is to have the capa- bility of predicting solar eruptive events. To The basic description of a plasma system will achieve this goal, we must investigate the evo- be introduced, starting from a kinetic descrip- lution of an Active Region. In this presenta- tion and culminating in the magnetohydrody- tion, we will present an analysis of magnetic namic (MHD) description. On the basis of field structures of the productive AR10720 of both kinetic and MHD models, we will dis- January 15, 2005 AND AR11283 of Septem- cuss the following four universal plasma phys- ber 6, 2011 using a data-driven 3D MHD ical processes at an introductory level: model. The measured magnetic field from Big Bear (BBSO) digital 1) Small amplitude waves and fluctua- vector magnetogram (DGVM) for AR 10720 tions in a plasma; and the SDO/HMI measurements for AR 11283 are used to model the non-potential 2) Nonlinear behavior of fluctuations and magnetic field changes. The numerical results dissipation and MHD turbulence; include the change of magnetic flux, the net

electric current, the length of magnetic shear 3) Shock waves, considering both a basic MHD description and a more refined of the main neutral line, and the flux normal- kinetic description; ized measure of the field twist. From these results we found the above four non-potential 4) Reconnection, described by MHD and magnetic parameters increase and decrease the important role of kinetic processes. before and after solar eruption. In other words, these four parameters are necessary The important process of particle conditions for solar eruption. Then we reveal at shock waves is relegated to a separate a particular feature: “the fragmented strong presentation. shear along the neutral line”. This feature could be interpreted as the variability of the shear angle (angle between the observed and Weather Space Joint Summer Camp 10 potential horizontal field) along the neutral lation and an enhanced turbulence level at the line. It may be an additional condition for front of the second shock than the case of a eruption. This suggests that the active region single CME-driven shock. Therefore, a more probability of producing an eruption is not efficient particle acceleration will occur. In the only dependent on active region free energy context of the "twin-CME" scenario, I will but also on the variability of the shear angle discuss in detail, an examination of the single which appears to correspond to the fragment- GLE event in 24, the May 17 2012 ed strong shear along the neutral line. event. I will also discuss some statistical stud- ies of other large SEP events in solar cycle 23.

Particle Acceleration in Large SEP Events-modeling extreme SEP events Tuesday, July 23

Gang Li ______CSPAR, The University of Alabama in Huntsville

In extreme Solar Energetic Particle (SEP) Cosmic Rays thoughout the events, such as GLE events, protons are often Vladimir Florinski accelerated to GeV/nucleon. Understanding CSPAR, the underlying particle acceleration mecha- nism in these events is a major goal for space The University of Alabama in Huntsville weather/ studies. In Solar Cycle 23, a total of 16 GLEs have This year marks a one hundred and first anni- been identified. Most of them have preceding versary of the discovery of cosmic ionizing CMEs and in-situ energetic particle observa- . Initially though to be gamma-rays tions show some of them are enhanced in IC- (hence the name), cosmic rays turned out to be ME or flare-like material. Motivated by this energetic charged particles (atomic nuclei and observation, we proposed a "twin-CME" sce- electrons) that permeate the Galaxy. Because nario for GLE events. In this scenario, two of their large Larmor radius, cosmic rays are CMEs erupt in sequence during a short period capable of entering the heliosphere and are of time from the same Active Region (AR) routinely detected on Earth and in interplane- with a pseudo-streamer-like pre-eruption tary space. They are a valuable tool to learn

magnetic field configuration. about the properties of the plasma in those The first CME is narrower and slower and the parts of the solar system that are too distant to second CME is wider and faster. We show be directly explored by . This tutori- that the magnetic field configuration in our al is an introduction to the physics of low en- proposed scenario can lead to magnetic recon- ergy cosmic-ray transport within our solar nection between the open and closed field system, including the solar wind and the heli- lines that drape and enclose the first CME and osheath. I will introduce the famous Parker its driven shock. The combined effect of the equation that describes the process of cosmic- presence of the first shock and the existence of ray diffusion in turbulent space plasmas. Sim- the open close reconnection is that when the ple applications of Parker equation to cosmic second CME erupts and drives a second ray transport in the expanding solar wind will

Joint Space Weather Space Joint Summer Camp shock, one finds both an excess of seed popu- be discussed. I will also give an update on the

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latest results from the Voyager mission that physical and mathematical, for energetic par- may have recently crossed the boundary of the ticles propagating in a magnetically turbulent solar system. environment will be presented. The interaction of cosmic rays with expanding flows such as the solar wind will be discussed briefly. The main focus of the lecture will be on the appli- cation of the basic description of energetic The Origin of the Fast and particle scattering and transport at a shock Slow Solar Wind wave. We will show that particles can be ac- celerated at a via the process of

diffusive shock acceleration and that quite Gary P. Zank remarkably a power law distribution in mo- CSPAR mentum independent of the details of the dif- The University of Alabama in Huntsville fusive scattering emerges. We will discuss The basic description of expanding flows in a some applications of the theory of diffusive nozzle will be discussed as a basis for under- shock acceleration. standing the solar wind flow. The Parker model and early observations of the solar wind will be presented. From this, we will infer the structure of the interplanetary magnetic field and the “Parker spiral.” The basic properties of the slow solar wind and fast wind will be Space Weather Instrumentation discussed, and from this the difficulties of the Parker model will be identified. Subsequent James Spann refinements of the fast solar wind model will NASA Marshall Space Flight Center be described, and the need for a hot corona and the segregation of the wind by coronal The value of space weather operations and holes will be addressed. We will conclude products are only as good as their accuracy. with a brief introduction to two modern mod- Our understanding of the dynamic space envi- els for heating the solar corona and driving a ronment and knowledge of its impacts on sys- fast wind. tems enables accuracy. Therefore, it is impera- tive that accurate models and sound theories associated with the physics of space weather

are developed. Observations of key space en- |

Particle Acceleration and Transport Theory vironment parameters motivate and guide the- ories and models. In turn, theories and models point to key observations that should be meas- ured. This is an iterative process. Gary P. Zank This talk will (1) develop the interactive na- CSPAR ture of theory/models with observations/ in- The University of Alabama in Huntsville struments, (2) provide an overview of the types of observations associated with space A fundamental plasma process in space and weather including remote and in situ sensing, astrophysical plasmas is that of energetic par- and (3) show and example of what is involved ticle transport and particle energization at in developing space instrumentation. shock waves. The basic description, both Weather Space Joint Summer Camp

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______

Grazing Incidence X-Ray Spectrometry

Radiation Hazards Mark Sterrett CSPAR, Jim Adams CSPAR, The University of Alabama in Huntsville The University of Alabama in Huntsville MaGIXS is comprised of a Wolter I telescope, The environment in space a slit, a pair of parabolic mirrors, a plano vari- poses a hazard for space crews and also af- able line-spaced grating and a CCD detector. fects space systems, especially electronics. This design and layout have been optimized to This lecture will cover the health hazards produce an optical system with peak effective posed by space radiation and how these haz- area of 5 mm^2, a wavelength range of 0.6-2.4 ards are managed. The effects of space radia- nm, spectral resolution of 2.0 pm, and spatial tion on spacecraft will also be discussed. The pixels of 2.5 arcsec along a 5 arcminute slit. focus will be mainly on radiation effects on The resulting instrument will resolve the solar electronics. The various effects will be de- spectrum for features in the solar corona with scribed and the techniques for estimating the a two orders of magnitude increase over pre- vulnerability of electronic parts will be dis- vious soft x-ray spectrographs in spatial and cussed. Also techniques or radiation hardening spectral resolution. spacecraft will be reviewed.

Techniques for Measuring the Magnetic Perspectives on Building Laboratory and Field in the Solar Corona Flight Instrumentation for Plasma meas- urements Ken Kobayashi CSPAR,

The University of Alabama in Huntsville

Kenneth. H. Wright CSPAR The University of Alabama in Huntsville Magnetic fields play a key role in the dynam- ics and energy transfer of the solar atmos- Development of a laboratory instrument to phere, from the to the corona diagnose plasma wakes and the evolution of and beyond. Energetic events such as flares its design through different flight versions will and coronal ejections (CMEs) are be- be discussed. Data from laboratory experi- lieved to be powered by energy stored in, and ments and from space flight missions will also transported by, magnetic fields. Yet our be presented. The author will review guiding understanding of the magnetic field in the principles for space instrument/mission devel- chromosphere and corona are based on indi-

Joint Space Weather Space Joint Summer Camp opment and, lastly, discuss his recent experi- rect measurements, such as extrapolation from

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the sun's and field lines inferred Space Weather and Mission Operations from imaging observations. Direct measure- ments are still very much experimental. Joseph I. Minow The talk will review the primary means of NASA, Marshall Space Flight Center measuring magnetic magneticfields remotely, i.e. Zeeman effect and Hanle effect. The solar Space weather can impact all phases of space physics group at NASA MSFC / UAHunts- mission operations starting with launch deci- ville have developed two ex- sions, through the on- operations period, periments that attempt to measure these ef- and during the final phase of decom- fects in the sun's chromosphere. The instru- missioning. Mission operations teams use ment principles and designs will be discussed. space weather data from a variety of sources to characterize the environment for space situ- ational awareness, to determine if current con- ditions are within operational constraints, for scheduling science and engineering operations to minimize impact of the , Thursday, July 25 and for specifying the operational environ- ment during anomaly investigations. The data requirements are variable and typically

______unique to a specific mission. This presenta- tion will highlight examples of space weather impacts on space missions, real time sources Spacecraft Charging of data for monitoring the space environment, Joseph I. Minow and practical strategies for incorporating space weather data into mitigation schemes used to NASA, Marshall Space Flight Center minimize the detrimental effects of space weather. Spacecraft charging is the accumulation of a net charge density on spacecraft surfaces (sur- face charging) or in spacecraft materials (in-

ternal or deep dielectric charging). Charging In-Situ Charged Particle Instrumentation is a fundamental physical process for materi- used for Space Weather Measurements als exposed to the space plasma and radiation

environment resulting in a net electric poten- | tial relative to the space plasma environment. Victoria N. Coffey Charging can also be a potential threat to NASA, Space Science Department space systems requiring evaluation of charg- Experimentally, the measurements taken for ing effects both at the design and operational Space Weather are largely pursued through phase of space programs. This presentation different types of instrumentation to study the provides an overview of the physical process- properties and physical processes in our space es involved in the spacecraft charging process, environments that are permeated by waves, techniques used to model spacecraft charging, particles, photons, electric and magnetic and provides examples of the impact of charg- fields. This science is largely pursued through ing on satellite operations and charged particle in-situ charged particle instrumentation that measurements in the space environment. can be utilized in either earth, planetary, or Joint Space Weather Space Joint Summer Camp

14 heliospheric missions (e.g., ionospheric or energy and mass from the Sun and heliosphere magnetospheric environments). We will dis- as it traverses down to the Earth. This session cuss the main types of charged particle in- will provide an overview of what Geospace is struments, how their measurements are made, and what its role is in the solar-terrestrial sys- and how these measurements broaden our tem. This includes how Geospace screens the understanding. Examples of specific instru- solar wind, responds to external drivers, and ments and their components will be presented. generates its own space weather that impact Advantages and disadvantages of each will be space assets and ground-based systems. We further discussed along with a tour of the Low will explore the fact that Geospace is not a Energy Electron and Ion Facility (LEEIF) that passive recipient of solar variability, but an has been used to develop, test, and calibrate active participant in space weather. these instruments for sounding rocket and satellite missions.

Inner Processes and Coupling

Dennis L. Gallagher Monday, July 29 NASA, Space Plasma Physics Group Marshall Space Flight Center ______

The inner magnetosphere is loosely defined to be the region of space threaded by terrestrial magnetic field lines from geosynchronous Geospace Overview orbit inward. The dominant sources of energy in this region are the radiation belts and the James Spann, Dennis L. Gallagher . The dominant mass in the region NASA Marshall Space Flight Center is the , which is an extension of the ionosphere. The region is characterized by Space weather has its origins beyond the the transport of plasma and energy both in- Earth, almost entirely at the Sun. However, ward driven by the solar wind magnetosphere the impacts of space weather on our society interaction and outward driven by ionization

occur within the near-Earth space environment of the upper atmosphere and by plasma heat- called Geospace. Geospace is the region ing. The physical processes involved depend around the Earth that begins at ~80 km alti- on particle-particle and wave-particle process- tude where the neutral atmosphere and ionized es and on electric currents driven by energetic ionosphere/ begin to interact, plasma through the resistive ionosphere. and extends out to the far limits of where its Plasma dynamics throughout the inner magne- magnetic field impacts the impinging solar tosphere are highly coupled with that in the wind. With few exceptions, all the space as- ionosphere and thermosphere as a conse- sets that exist are in Geospace. Therefore to quence of these processes. An overview of understand space weather and its impact on these interactions and their consequences society it is required that we comprehend how will be discussed.

Joint Space Weather Space Joint Summer Camp Geospace filters, converts and dissipates the

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Ionospheric Radio Science Solar Flares as a Source of Energy in the Earth’s Magnetotail Linda Krause NASA, Marshall Space Flight Center Sabrina Savage NASA, Research Astrophysicist

, we have a problem!” The iconic Flares on the solar surface propagate energy declaration heralds a well-known story of into the solar system which in turn affect the technical heroism that would make any geek Earth’s magnetosphere. Coronal mass ejec- proud, one in which scientists and engineers tions (CMEs) are a notable consequence of worked around the clock to save the of solar eruptive events and are the result of the three aboard the crippled Apol- magnetic field reconfiguration. Interesting lo 13 until it could safely hobble home. But sunward-flowing voids are now an expected what if those communication signals never consequence resulting from the passage of reached Mission Control back on Earth be- CMEs from solar flaring regions. Recent ob- cause of a space weather storm? This talk will servations made using the extreme-ultraviolet provide a survey of topics related to iono- (EUV) imagers aboard SDO/AIA have high- spheric radio science, including communica- lighted their association to magnetic reconnec- tion and GPS navigation outages resulting tion, which is in turn associated with continual from solar and geomagnetic storms. General- energy release following flare initiation. I will ly, the Earth's magnetic field protects us from discuss how these flows propagate, their con- the harmful solar particles streaming toward nection to flare energy release, and tie them us at supersonic . However, sometimes back to potentially analogous events in the there are vast explosions of solar material magnetotail. sending large blobs of plasma hurling through space toward Earth. These blobs slam into the

Earth's magnetic field, compressing it on the day side and causing many complex reactions

on the nightside, some of which result in auro- ra. The problems arise when this reorganiza- tion of magnetic field energies our Earth's Tuesday, July 30 plasma environment in a complex way, often

resulting in plasma “bubbles” that scramble ______radio transmissions similar to the distortion of | an underwater in front of Jacuzzi bub- bles. With this talk, we will discuss iono- spheric structures, plasma instabilities, solar Gamma-ray Signatures of Solar Flares drivers, diagnostics, and forecasting systems. We'll take a look at one case study, and con- clude with some thoughts about opportunities Michael Briggs for student research in this field. CSPAR, The University of Alabama in Huntsville

Energetic processes that occur in solar flares can create gamma-ray signatures. Accelerated Joint Space Weather Space Joint Summer Camp

16 ions can create radioactive isotopes, some of An Introduction to which emit gamma-ray lines from approxi- mately 1 to 6 MeV. David H. Hathaway Hundred-MeV protons can create pions. Neu- NASA, MSFC tral pions decay into gamma-rays. Positrons are produced from charged pions and by some The key scientific questions for Solar Physics radioisotopes; from positron annihilation we – the scientific study of the Sun – have observe a signature 511 keV line. evolved over the last century from questions Neutrons combine with protons, emitting a concerning the source of the Sun’s energy characteristic 2.2 MeV line. The nuclear (nuclear fusion) to three space weather related gamma-ray lines are especially useful as diag- questions: 1) How is the cycle pro- nostic of the energy of the particles that creat- duced? 2) How is the corona heated/solar ed the radioisotopes. wind driven? And 3) How are solar flares and I shall use Fermi observations of the M2 solar coronal mass ejections produced? This intro- flare of 2010 June 12 as an example. duction to Solar Physics will describe the na- ture of these problems and current avenues for exploring solutions.

Photospheric Magnetic Field Evolution Terrestrial Gamma-ray Flashes: Gamma The Inner Boundary Condition for rays Electrons, Radio Discharges and the Heliosphere Antimatter Signals from Thunderstorms

David H. Hathaway Valerie Connaughton NASA, MSFC CSPAR The University of Alabama in Huntsville Intense magnetic fields loop outward from the solar interior in the sunspot zones through the Terrestrial Gamma-ray Flashes (TGFs) have themselves. The turbulent motions at become an unexpectedly rich area of scientific the surface of the Sun shred these fields and discovery for the Fermi Gamma-ray Space Tel- spread them out across the surface where they escope, an astrophysical space mission get caught up in the global flows – differential launched in June 2008. TGFs seen by GBM rotation (faster than average rotation at the

are detected through their gamma-ray or elec- equator and slower than average near the tron-positron signals depending on the position poles) and meridional flow (flow along merid- of Fermi relative to the initiation point. I will ian lines from the equator to the poles). In this discuss the population of TGFs observed by talk the evolution of the magnetic field at the GBM, focusing on their temporal properties surface of the Sun will be described along and their very close relationship to the associ- with its use as the inner boundary condition ated radio signals detected by the World Wide for the structure and evolution of the helio- Lightning Location Network (WWLLN). sphere.

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Wednesday, July 31 closed bipolar fields that range in size from as large as the solar radius to as little as a thou- sand times smaller. Typical observed explo- ______sions are shown in solar images and explained with cartoons of the form and action of the Unlocking the Secrets of the Sun magnetic field. The take-home points are:

Amy R. Winebarger • All space weather is made or modulat- NASA, Marshall Space Flight Center ed by the Sun’s magnetic activity. • All magnetic fields on the Sun are The recent launch of the High-Resolution made from Ω-loop bipoles that are 10 Coronal Imager (Hi-C) as a sounding rocket to 1000 times smaller than the Sun has offered a new, different view of the when they emerge. Sun. With ~ 0.2" resolution and 5 second ca- • The field in an emerged bipole often dence, Hi-C reveals dynamic, small-scale has free energy that it releases by ex- structure within a complicated active region, ploding. including coronal braiding, reconnection re- • The greatest explosions of the big bi- gions, cool, evolving structures, and flows poles are gigantic CME/flare eruptions along active region fans. By combining the that blast out into the solar wind and Hi-C data with other available data, we have make the most violent space weather. compiled a rich data set which can be used to • Explosions of the smallest bipoles pos- address many outstanding questions in solar sibly power the quiet corona and physics. Though the Hi-C rocket flight was steady solar wind of normal space short (only 5 minutes), the added insight of the weather. small-scale structure gained from the Hi-C • Each explosion, large or small, is an data allows us to look at this active region (+- explosion of stressed magnetic field 1 day of flight) and other active regions with unleashed by reconnection. new understanding. The results from the Hi-C sounding rocket were recently published in Nature and have inspired more than 150 media reports. In this talk, I will show some the first Reconstruction of Magnetic Clouds from results from the Hi-C sounding rocket and In-Situ Spacecraft Measurements

explain how they help us advance problems that have stymied the astrophysical communi- | ty for almost 100 years. Qiang Hu CSPAR, The University of Alabama in Huntsville

Explosive Solar Magnetic Fields and Coronal Mass Ejections (CMEs) are explosive Space Weather events that originate, propagate away from the Sun, and carry along solar material with em- bedded solar magnetic field. Some are accom- Ron Moore panied by prominence eruptions. The entire NASA, Marshall Space Flight Center process can be observed by multiple instru- mentations on-board several on-going space- An overview is given of the explosions of

craft missions. The interplanetary counterparts Weather Space Joint Summer Camp magnetic arcades on the Sun, explosions of 18 of CMEs (ICMEs) are often detected in-situ event rates. This work is presently being by spacecraft ACE and Wind, which provide done here at UAH and MSFC and will be re- both magnetic field and plasma measurements viewed in this talk. In addition, we will pre- sampled along the spacecraft path across the sent other forecasting methods and their effi- ICME structure. All these remote-sensing and cacy, as well as the process of research to op- in-situ measurements make it possible to per- eration (R2O). form the intercomparison between the (I)CMEs and their source regions at the Sun. In particular, a subset of ICMEs, so-called Magnetic Clouds (MCs) can be characterized by magnetic flux-rope structures. We will ap- ply the Grad-Shafranov reconstruction tech- nique to examine the configuration of MCs Thursday, August 1 and to derive relevant physical quantities. We will select recent events during the rising phase of enhanced solar activity, and utilize ______additional observations from the most recent spacecraft missions, such as the STEREO and SDO spacecraft. Both observational analyses of solar source region characteristics including Electron Kinetic Scale Simulations flaring and dimming, and the corresponding MC structures will be presented. Ross Burrow CSPAR, The University of Alabama in Huntsville

Flare and CME Driven Space Weather Particle in cell (PIC) code is a numerical Effects and Forecasting method for implicitly solving the Vlasov equation for collisionless plasmas. Theoreti- cally and conceptually the PIC method is sim- David Falconer CSPAR, ple and works by brute force, solving particle The University of Alabama in Huntsville motion via the Lorentz force equation and the electromagnetic fields directly through Max- Solar flares and Coronal Mass Ejections well's equations. If computer resources were (CMEs) are the drivers of the most severe not an issue PIC code would, in principle, able

forms of space weather. Space weather can to resolve the relevant physics for large (AU create benign effects such as the Northern scale) as well as small (Debye) scale astro- Lights, but it can also interfere with GPS, ap- physical simulations, but in reality PIC is lim- ply unexpected voltages to power transmission ited by the fact that it is a very computer- lines, and harm and astronauts. NO- resource expensive, plasma simulation meth- AA is in charge of monitoring and forecasting od. Thus PIC simulations are typically em- space weather for the nation. While forecast- ployed for electron kinetic (fine) scale plasma ing when the next flare or CME will occur is simulations. beyond current capabilities, forecasting the We discuss the construction of a 1D PIC code probability of an event in the future is possi- and present some simulation results including ble. One method that is being developed uses the evolution of a two-stream instability due to

Joint Space Weather Space Joint Summer Camp a free-energy proxy and empirically-derived counter-streaming electrons, as well as the

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evolution of an ion ring-beam in the presence small angles to 90 degrees, separated from the of electrostatic fluctuations. We also discuss fast wind that originates at coronal holes sub- the development of a new type of hybrid code, stantially affects plasma at the heliospheric which promises gains in computational effi- interface, in the compressed plasma layers ciency by using PIC methods to couple ener- ahead of and behind the heliopause. The solar getic ion populations with the hydromagnetic, cycle may be the reason of the complicated multifluid equations, with coupling via the flow structure being observed in the inner he- pressure tensor. liosheath by Voyager 1. We present the results of the solar cycle simulations based on differ- ent numerical models, including the model with the SW boundary conditions derived Numerical Simulations from Ulysses measurements, and demonstrate how they can explain the observations of Sergey Borovikov small to negative SW radial compo- CSPAR, nents at Voyager 1, as well as an abrupt de- The University of Alabama in Huntsville crease in the ACR flux. The possibility of us- ing observational data as boundary conditions Numerical simulations may produce gigabytes for the SW simulations is discussed. of data, which are values of some physical quantities. Although these data are self- sufficient, it is nearly impossible to analyze them by looking at the numbers. In this talk, we will look how visualization techniques Looking to the interstellar boundary with help researches to understand physical phe- IBEX nomena. We will examine different types of plots, discuss best practices in the visualiza- tion, and speak about software/hardware as- J. Heerikhuisen, E. Zirnstein pects of the visualization. CSPAR, The University of Alabama in Huntsville

The IBEX spacecraft has two neutral atom detectors (IBEX-Hi and -Lo) that sample each Large-Scale Simulations of the time direction of the sky at least once every six Dependent Heliosphere months, allowing it to produce all-sky maps of (ENA) flux at a range |

N. Pogorelov CSPAR, of energies. Since neutrals are not affected by The University of Alabama in Huntsville magnetic fields, and since collisions are very infrequent, IBEX is able to detect ENAs that Solar cycle has a profound influence on the traveled from the boundary region between solar wind (SW) interaction with the local the heliosphere and the local interstellar medi- (LISM) on more than one um (LISM). In this talk we introduce the time scale. Also, there are substantial differ- IBEX spacecraft and some of its capabilities. ences in individual solar cycle lengths and SW We will then show results of simulating Hy- behavior within them. The presence of a slow drogen (H) ENA and interstellar H flux meas- SW belt, with a variable latitudinal extent urements at the IBEX spacecraft position, changing within each solar cycle from rather while including the Compton-Getting (CG) effect. The CG effect arises when measure- Weather Space Joint Summer Camp 20 ments of particle flux are made in a frame - who accepted their country’s call to service moving with respect to the frame of the emis- and would become known as the Mercury 7. sion source. In this case, measurements made These men who had jockeyed for the best fly- in the IBEX spacecraft frame, which moves ing jobs in the military, began competing for ~30 km/s circularly along the ecliptic plane, rides on rockets. Most would eventually vie produce different results than those measured for the ultimate ride to the moon. This was the in the solar inertial frame. We will first show dream—a chance to ascend to the top of the results from simulating high energy H atom pyramid—a lion-hearted pilot’s deepest de- fluxes relevant to IBEX-Hi measurements, sire. Ed Buckbee, who has enjoyed a 50 + particularly that of the IBEX ribbon. Then we year association with the U.S. space program, will show results from simulating low energy follows these brave pioneers. From Alan H atom fluxes relevant to IBEX-Lo measure- Shepard’s sub-orbital flight to the last man to ments. The CG effect becomes increasingly walk on the moon, Gene Cernan, Buckbee important at lower particle energies, particu- covers all the manned missions of that era. larly when including radiation pressure and Through time and personal friendships, he gravitational effects. captures their dreams of flying higher, faster and farther than anyone in the known uni- verse. You are taken behind the scenes to wit- ness the competition between chimpanzees and astronauts and the conflict between NASA engineers designing capsules and those Friday, August 2 who would pilot them. They were our first astronauts. The path they blazed now shines for others; on a voyage that is a measure of the ______best in us all. The Mercury 7 astronauts were the first, the bold, the brave. They had the right stuff. They were The REAL Space Cow- Remembering the Real Space Cowboys boys. The Soul Of An Explorer Lives In Us All!

Ed Buckbee U.S. Space & Rocket Center Space Weather “As far as returning to normal , I don’t think any of us ever returned to normal life. I

don’t think any us were normal people to be- U.S. Space & Rocket Center gan with.” Mercury Alan B. Shepard, Jr. Forecast: Lot's of sun (except at "night"). Cloud free (above the horizon). Fifty-two years ago, Alan Shepard climbed No precipitation (except in case of propellant aboard a Huntsville-developed Mercury Red- leak!) stone rocket and blasted off from Cape Ca- Be sure to prepare for extensive UV, EUV and naveral to became the first American to ride even Xray exposure if you expect to take a a rocket. That was the beginning for U.S. stroll outside. manned space flight. He had been selected to (As an extraordinary requirement when train with America’s first astronauts—John strolling, bring along your own breathing at- Glenn, Wally Schirra, Gordon Cooper, Gus mosphere as well!) Joint Space Weather Space Joint Summer Camp Grissom, Scott Carpenter and Deke Slayton-

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For the rest of the week (and even longer) expect no major changes for a long time.

Our observation post? , the US first space station, orbited precisely 40 years ago in 1973. Skylab was flown in 3 missions of about 1, 2 and 3 months duration, all world records at the time. Although there were many experiments in multiple fields conducted, we will talk mostly about research done on the Sun at wavelengths which cannot penetrate the earth's atmosphere. Secondly we discuss the many life science experiments conducted to better understand how the human body adapts to and then readapts when one comes back to a normal gravitational environment

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Weather Space Joint Summer Camp

22 Project work in Huntsville Project 2 Grad-Shafranov Reconstruction of Mag- ______netic Flux Ropes

Qiang Hu11, Christian Möstl2, Chales J. Farrugia3 1 CSPAR, The University of Alabama in Project 1 Huntsville 2 Institute, Graz, Austria 3 SOFIE – Solar Flares Detected by University of New Hampshire, Durham

Ionospheric Effects The Grad-Shafranov (GS) reconstruction Daniela Wenzel method has recently become widely used in German Aerospace Center (DLR), Neustrelitz the space physics community in different contexts. It has been often used on struc- SOFIE is an educational project developed by tures in space plasmas which can be de- the DLR_Project_Lab in Neustrelitz / Germa- scribed by the approximation of magneto- ny. It aims to develop a network of stations hydrostatics such as the , flux and is intended for long-term studies. The transfer events, flux ropes in the Earth's project is concerned with the observation of magnetotail, as well as magnetic flux radio bursts emitted by the sun (so-called solar ropes/magnetic clouds in the solar wind. flares). The method is capable of deriving a cross These flares may be detected via measure- section of a cylindrical structure (non- ments of the resulting amplitude of signals axisymmetric) from single-spacecraft data emitted by VLF transmitters (3-30 kHz). along a line across the structure. Whenever a flare hits earth’s atmosphere, X- In this project, a program package written in rays cause an increase of electron density in MATLAB (courtesy of Christian Möstl) the lower ionosphere. By this, conditions for will be utilized for learning the method and propagation of terrestrial radio signals are analyzing real in-situ spacecraft measure- altered, enabling a detection of the causes. ments of magnetic flux ropes/magnetic During the camp a receiver will be set up. clouds. These programs are based on those This requires building an antenna. Afterwards developed by Qiang Hu in his 2002 JGR data analysis and signal processing are dis-

paper. They were extended by Christian cussed. Implementations are going to be done Möstl (Space Research Institute, Graz, Aus- in Python; a short introduction into that lan- tria) during his PhD thesis (finished in guage will be given. The ground-based data is 2009) to include a graphical user interface compared to satellite data (GOES). We will (GUI), which makes it easy to apply the experience a couple of filters and first compar- reconstruction method for a single event isons in strength and time delay of solar after the satellite data have been put into a flares’ maxima. proper format. Knowledge of and experi- ence with MATLAB is not required, but would be helpful. The goal of this project is to go through the process of data acquisi- tion, interval selection, pre-processing, final Joint Space Weather Space Joint Summer Camp

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reconstruction and visualization of the re- Project 4 sult. The evaluation of the project will be based on the execution of the program, the Scientific Visualization of Space Envi- correct and coherent analysis of the data, ronment Data and the interpretation of the final results. Bonus points will be awarded if the team Linda Krause could succeed in 3D visualization of the NASA, Marshall Space Flight Center result and deriving additional physical quantities associated with a magnetic flux rope. This project will teach students how to devel- op 3D surface model of space environment

structures from 3D gridded vector data sets. For example, it is one thing to have magnetic field vector data on a 3D grid, and quite an- Project 3 other to construct magnetic field lines from those data. The students will learn an open Numerical Simulation of Ring-Current source tool called VisIt. They will use VisIt particles to visualize magnetic field lines, isosurfaces, and particles using space environment data Jacob Heerikhuisen that will be provided to them. Time permit- CSPAR ting, the student may learn how to animate the The University of Alabama in Huntsville 3D surface models. The Earth’s magnetic field is approximately a dipole. Particles in a dipole field are initially confined to field lines and so move up or down toward a pole. Near the pole, however, field lines converge and particles are reflected by the conservation of magnetic moment. This results in particles "bouncing" on field lines between the north and south poles. Additional- ly particle drift around the earth, thereby cre- ating the rind-current, due to the curvature of

the field-lines. We will simulate the ring cur- rent by assuming a simple form the the Earth’s | magnetic field, and numerically computing the of charged particles.

Joint Space Weather Space Joint Summer Camp

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Joint Space Weather Summer Camp

August 4 – August 18, 2013 in Neustrelitz and Rostock

Tuesday, August 6 sensing and scientific satellites. Thus, DLR Neustrelitz, as one of the four stations belong- ing to the Real Time Solar Wind (RTSW) ______network of NOAA, contributes essentially to the permanent availability of solar wind data measured onboard NASA’s ACE satellite. Huge remote sensing data volume is success- Welcome and Visit DLR Neustrelitz fully managed in the EOC by using the Data Information Management System (DIMS). Holger Maass, Hans-Joachim Stottke Research activities in the Institute for Remote German Aerospace Center (DLR), Neustrelitz sensing Methods focus on studying scattering and radiative transfer in the Earth’s atmos- phere for improving atmospheric corrections The Neustrelitz site of the German Aerospace of remote sensing data. Center (DLR) is located in Mecklenburg- Vorpommern, approximately 100 km north of In the field of , the research Berlin. More than 60 employees are working is focused on developing algorithms for pre- in three institutes the cise and safe navigation in particular in the • Earth Observation Centre maritime application sector. Thus, technologi- • Institute for Communications and Nav- cal developments have been carried out for the igation Rostock Research Harbour. • Institute for Remote-sensing Methods To correct and the impact of space weather

and the Technology Marketing section. In effects on GNSS applications, the ionosphere addition a school-lab is just established for is permanently monitored and modelled in educating students in space sciences and relat- near real time. Research activities focus on ed innovative technologies. DLR Neustrelitz developing methods to detect, forecast and site has access to modern technological sys- mitigate ionospheric perturbations having the tems suitable for the demands of a real-time capability to degrade GNSS systems. Derived data centre for GMES and Galileo related re- Data products are disseminated via the Space search tasks. Weather Application Center Ionosphere (SWACI), a project which is essentially sup- The national is a department ported by the state government of Mecklen- of the Earth observation center (EOC) and burg Vorpommern.

Joint Space Weather Space Joint Summer Camp takes care for reception of numerous remote

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Introduction and History of Introduction to Satellite Orbital Ionospheric Research at DLR Mechanics for Space Weather Applications Norbert Jakowski German Aerospace Center (DLR), Neustrelitz Ben Opperman SANSA Space Science The Neustrelitz site of the German Aerospace Center (DLR) has a nearly 100 years old his- Satellite-borne measurements of space weath- tory of space weather related observations and er phenomena significantly enhance our un- research. Activities were always focussed on derstanding of, and modelling capability for observations of the propagation characteristics predicting space weather processes and of radio waves and studies of the ionospheric events. Specific space mis- impact. After the launch of the first satellite, sions however require specialised to Sputnik 1, in 1957 the focus shifted rapidly achieve its mission objects and orbits may from terrestrial HF to transionospheric radio differ from one mission to another. wave propagation. Knowledge and understanding of satellite or- Nowadays, when considering modern space bit characteristics and dynamics is subsequent- based radio systems of telecommunication, ly required in the design of relevant orbits for navigation and remote sensing, our modern specific space weather satellite missions. The society depends strongly on reliability of used objective of the lecture is to supply necessary transionospheric signals. This is a strong mo- background on orbit dynamics and design tivation to study the ionosphere and associated with emphasis on space weather missions. The space weather phenomena. Fortunately, dual content will cover basic dynamics derived frequency signals of Global Navigation Satel- from Kepler and Newton’s laws; various orbit lite Systems (GNSS) such as GPS or Glonass types; the application of perturbations to orbit can effectively be used for monitoring and design and the importance and characteristics modelling the ionosphere for research and of Lagrangian points. The orbit characteristics establishing ionospheric services which pro- of ACE, GOES, SOHO, STEREO and other vide crucial information and data to customers satellites will be discussed. Basic software for to warn them or to enable ionospheric correc- demonstrating orbit propagation and design tions/mitigation of erroneous radio signals. will be introduced.

DLR Neustrelitz has a long-term experience in monitoring, studying and modelling the iono- | sphere. The strong relationship of ionospheric behav- iour with space weather phenomena is the basis for our interest in organizing the Space Weather Summer Camp in close cooperation with the University of Alabama Huntsville. A short overview on the summer school pro- gramme in Germany will be given.

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Wednesday, August 7 systems such as H2O for a wide range of den- sities and temperatures. Most interestingly, the equation of state data for hydrogen predict a ______first-order liquid-liquid phase transition with a critical point at 1400 K, 1.32 Mbar and 0.79 g/cm3 which is connected with a nonmetal-

to-metal transition [1,2]. The behavior of the Progress in Warm Dense Matter and electrical and thermal conductivity and of Planetary Physics their ratio (Lorenz number) is analyzed along this transition, especially the deviations from Andreas Becker, Winfried Lorenzen, the well-known Wiedemann-Franz relation [3] Robert Püstow, Ronald Redmer which might be important for the operation of University of Rostock planetary dynamos. Furthermore, we have identified the parameters for demixing of heli- The behavior of matter under extreme condi- um from hydrogen [4,5] which match the con- tions (megabar pressures, temperatures of sev- ditions in the interior of Saturn as long has eral 1000 K up to about 100.000 K) is im- been predicted. Finally, we have calculated portant for interior models of giant planets. the interior structure and composition of solar Surprisingly, the high-pressure phase diagram [6] and some extrasolar planets (GJ 436b [7], of even the simplest and most abundant ele- GJ 1214b [8]) within three-layer models. We ments hydrogen and helium is not well known will give exemplary results for the density and (Jupiter, Saturn). Interesting phenomena such temperature profile, the metallicity and size of as proton conduction and demixing are ex- the planetary cores, and for the slope of the pected when studying the behaviour of oxy- material properties along planetary isentropes gen, carbon, nitrogen, their hydrides and mix- [9,10]. tures at high pressures (, ). A large number of planets has been found [1] W. Lorenzen, B. Holst, R. Redmer, Phys. Rev. around other stars since 1995 which show a B 82, 195107 (2010). strong variation in mass, chemical composi- [2] M.A. Morales et al., PNAS 107, 12799 (2010). tion, and distance to their parent star so that [3] B. Holst, M. French, R. Redmer, Phys. Rev. B 83, 235120 (2011). solar and extrasolar giant planets are perfect [4] W. Lorenzen, B. Holst, R. Redmer, Phys. Rev. laboratories for the study of matter under ex- Lett. 102, 115701 (2009). treme conditions. In the first part we will re- [5] M.A. Morales et al., PNAS 106, 1324 (2009). view the main properties of the solar planets [6] J.J. Fortney, N. Nettelmann, Space Sci. Rev.

and introduce detection methods for extrasolar 152, 423 (2010).

planets and their properties. [7] N. Nettelmann et al., Astron. &Astrophys.523, In the second part we will give an introduction A26 (2010). into the physics of matter under extreme con- [8] N. Nettelmann et al., Astrophys. J. 733, 2 ditions. Because simple plasma models based (2011). on perturbation theory fail to describe strongly [9] N. Nettelmann, A. Becker, B. Holst, R. Redmer, correlated systems, ab initio methods have Astrophys. J. 750, 52 (2012). [10] M. French et al., Astrophys. J. Suppl. Ser. been applied to derive physical properties. For 202, 5 (2012). instance, molecular dynamics simulations based on finite-temperature density functional theory were used to calculate the equation of state, the electrical and thermal conductivity Joint Space Weather Space Joint Summer Camp of H, He, their mixtures, and of molecular

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Thursday, August 8 theoretical expertise has been developed at IAP to fill this gap. The activities of IAP con- centrate on the headquarter in Kühlungsborn ______(54°N) and on the ALOMAR observatory (Arctic Lidar Observatory for Middle Atmos- phere Research) being located at 69°N in Northern Norway. Furthermore, IAP runs a Welcome/Introduction to Atmospheric mobile lidar which is currently located in Da- Science at IAP vis, Antarctica. The IAP is member of the Leibniz-Society and has 80-90 employees. Franz-Josef Lübken The institute is funded by the local govern- Leibniz-Institute of Atmospheric Physics ment of Mecklenburg-Vorpommern, by the (IAP), Kühlungsborn, Germany federal government in Berlin, and by research grants from various organizations. The major task of the IAP is the experimental and theoretical exploration of the atmosphere from the ground to the lower thermosphere (≈10 – 120 km). The focus of the activities is on the thermal and dynamical state of the (50-100 km) at middle and Mesospheric Dynamics as latitudes, the coupling between various at- Observed by Radars mospheric layers, and long-term changes in the upper atmosphere. Experimental studies at Gunter Stober, Ralph Latteck, ManjaPlacke, IAP concentrate on highly sophisticated ob- Vivien Matthias, Peter Hoffmann and servations of temperatures and winds by Marius Zecha ground based lidars and radars, and on meas- Leibniz-Institute of Atmospheric Physics urements of turbulence and meteoric smoke (IAP), Kühlungsborn particles on sounding rockets. More recently, turbulence detection on balloons in the strato- sphere and ground based measurements of Radar remote sensing is a key element inves- water vapor by microwave technique have tigating atmospheric dynamics in the tropo- been developed. Theoretical investigations sphere/lower and in the meso- include the role of dynamical processes sphere. In particular, the mesosphere is char-

( waves, turbulence etc.) for the energy |

acterized by its high dynamic variability due and momentum budget of the atmosphere, as to tides, planetary waves, gravity waves and well as the role of ice layers (noctilucent turbulence. In this lecture we present an over- clouds, NLC) at≈83 km for the detection of view of different radars and techniques to in- climate change. Our understanding of the vestigate the dynamic situation at various spa- middle atmosphere is still rudimentary which tial and temporal scales. Further, the lecture is partly caused by the fact that this region is provides a short overview of the physics of the experimentally difficult to access and that the related scattering processes to obtain the at- theoretical description of the most relevant mospheric information. This includes also an physical processes changes fundamentally in introduction to special mesospheric phenome- the upper mesosphere/lower thermosphere. na like e.g. polar mesospheric summer echoes, Some worldwide unique experimental and

mesospheric echoes and meteors. As highlight Weather Space Joint Summer Camp

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a short introduction in the IAP student paper In north America some radars based on this rocket program is given. technology (AMISR) are now operating in the auroral zone and polar cap. In northern Europe a more advanced, more powerful radar with Friday, August 9 remote stations will be built. The new radar, with thousands of small antennas and trans- mitters, called EISCAT_3D is a three- ______dimensional imaging radar. It will make con- tinuous measurements of the geospace envi- ronment and its coupling to the Earth's atmos- phere from its location in the auroral zone at Incoherent Scatter Radars to Study the the southern edge of the northern polar vortex. High Latitude Ionosphere

Michael Rietveld EISCAT Scientific Association, Ramfjordmoen, Norway SWE Impact on GNSS Incoherent Scatter Radars (ISR) are powerful Botho Graf zu Eulenburg radars with large antennas operating in the AXIO-NET GmbH, Germany VHF and UHF bands with the ability to pro- vide detailed ionospheric parameters from Precise GNSS measurements with cm accura- altitudes as low as 50 km to over 1000 km. cy rely on resolving phase ambiguities of sat- The principles of their operation, some of the ellites signals received. The and reliabil- background theory, and the resulting meas- ity of achieving a so called “fixed solution” or urements will be described. The two EISCAT “RTK solution” strongly depends on iono- radars (at 224 and 931 MHz) operating in spheric conditions. northern Scandinavia and a third (at 500 MHz) The current prediction for ionospheric activity operating on Svalbard will be used as primary (Sunspot solar cycle) estimates a maximum in examples but newer radar systems in Alaska 2013. During the last solar cycle, in particular and Canada will also be described. Although in 2002, a strong correlation could be ob- primarily used to study the natural ionosphere served between ionospheric activity and user and upper atmosphere, they can also be used performance in GNSS network operation. An to study the effects of artificial perturbations RTK user needed a long time to get an RTK

(often similar to space weather effects) pro- solution, and on some cases it was not possi- duced by radio-wave heating from specialized ble to work with GNSS at high precision. powerful HF transmitters, which will also be illustrated using the HF-facility operated by An unusually intense observed by EISCAT. NASA space observatory on 7 June 2011 The limitations of the present second- could cause significant disruptions to satellite generation 20 to 30 year old radars, particular- communications and power lines on the Earth ly in the inability to observe different direc- so officials said (Space Weather Prediction tions of the sky simultaneously, and the diffi- Centre). In some German media (newspapers, culties associated with running these radars TV) this got major publicity as a huge cloud continuously, have led to proposals to build of particles was released and was placed over new types of radar based on phased-array an- an area of nearly half the size of the solar sur- Joint Space Weather Space Joint Summer Camp tennas instead of the traditional dish antennas. face.

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Solar flares can cause geomagnetic storms, Radio Observations of the Sun including disturbances in satellite navigation. with LOFAR This is what an RTK service provider as AX- IO-NET is would like to know in advance or Gottfried Mann immediately when such an event occurs, in Leibniz Institute for Astrophysics Potsdam order to provide its customers with relevant (AIP), Potsdam information how to prevent irregular results from satellite navigation. The Sun is an intense radio source in sky. The In fact there were no such influences seen as Sun is an active star, which manifest not only predicted. in the variation of Sun spots and flares, but Available forecasts currently are inaccurate also a virulent variation of its radio radiation. with respect to the influence on GNSS-RTK. Bursts of the radio emission from the Sun are Possible effects are well known, but when closely related to flares. Basically, flares are does a solar flare significantly influence pre- defined as a strong enhancement of the emis- cise positioning applications with GNSS? sion of electromagnetic waves covering from the radio up to the gamma-ray range. Thus, Reliable forecast products are needed for such the observation of the Sun's radio emission is Space Weather incidents. A growing user a sensitive tool for studying flare physics. community (e.g. surveyors, construction and The new European radio telescope LOFAR agriculture) is depending on reliable use of (Low Frequency Array) is able to measure the GNSS and on precise forecasts of Space Sun's radio radiation with a highly spatial and Weather events. temporal resolution. Few examples of flares

are presented to demonstrate the close rela- tionship between the various flare phenomena with the Sun's radio radiation. Ionization Processes in the Heliosphere

Klaus Scherer Monday, August 12 Copernicus Gesellschaft e.V., Germany

In the heliosphere, especially in the inner heli- ______osheath, mass-, momentum-, and energy load- ing induced by the ionization of neutral inter- stellar species plays an important and for some | species, especially He, an underestimated role. Cosmic Rays on Their Route Through the I discuss the implementation of charge ex- Magnetosphere and Atmosphere - change and electron impact processes for in- Theory and Experiment terstellar neutral Hydrogen and Helium and their implications for further modeling. Espe- cially, the importance of electron impact and a Bernd Heber more sophisticated numerical treatment of the Institute for Experimental and Applied Phys- charge exchange reactions will be discussed. ics, Christian-Albrechts-University of Kiel On their way to Earth cosmic rays encounter

after passing the galaxy and the heliosphere

the Earth’s magnetic field and, if they succeed Weather Space Joint Summer Camp

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to go beyond, the atmosphere. The magnetic Out of the classroom-Into the Lab! field is shaped by electric currents in the Earth's core and by the interaction with the Dirk Stiefs solar wind. Cosmic rays coming from outside DLR_School_Lab Bremen will due to the Lorentz force undergo compli- cated in the magnetic field and The German Aerospace Center (DLR) invites may even be prevented from getting access to students and their teachers to visit its high- the atmosphere. The DOSimetry Telescope tech student laboratories, the DLR_School_ orbits the Earth aboard the International Space Labs. This is where young people and students Station in a height of about 400 km. Its func- have an opportunity to actively discover the tionality as well as typical data will be dis- fascinating world of research and technology. cussed. We will in addition show that the fil- The special feature of our concept: in the au- tering by the magnetosphere gives us thus the thentic environment of a research institution possibility to derive the spectra and arrival the students themselves can carry out experi- directions of cosmic rays. ments which are specifically related to ongo- When the enters the Earth’s at- ing projects in the fields of aeronautics, space, mosphere, it encounters atoms and molecules, transportation and energy. And so they experi- especially nitrogen and oxygen. Collisions ence in a relaxed way how exciting the natural will create secondary particles of different sciences and research can be. energies. Of special interest to aircraft person- In DLR_School_Lab Neustrelitz and al are neutrons. PING is a detector developed DLR_School_Lab Bremen the main topic of to measure neutrons with energies up to a few the experiments is space. A special focus of an tenth of MeV. In a practical unit of the course experiment both school labs have in common we will take data with the instrument and dis- is space weather. Mr. Stiefs will give a short cuss the outcome. overview about the concept of the DLR_ Some of the secondary particles in the atmos- School_Labs and space weather activities. phere may reach the ground, where one can Afterwards the audience can try some special measure them by e.g. a . De- selected hands on experiments. spite their decades of tradition, ground based neutron monitors (NMs) remain the state-of- the-art instrumentation for measuring cosmic History of Space Weather Observations rays, and they play a key role as a research and Research tool in the field of space physics, solar- terrestrial relations, and space weather appli- Kristian Schlegel

cations. They are sensitive to cosmic rays

penetrating the Earth's atmosphere with ener- Copernicus Gesellschaft e.V., Germany gies from about 0.5-20 GeV. In two projects, funded by the EU, SEPSErver and NMDB we Centuries ago, people were not aware of will compare data from spacecraft with the “space weather“, but observed two important one from neutron monitors. related phenomena: and sunspots. Thus a history of space weather exploration starts with the history of such observations. In the 18th century scientists began to explore the geomagnetic field and realized a connec- tion with aurora. It took more than 200 years to clarify and explain this relationship. Before, Joint Space Weather Space Joint Summer Camp the fundamentals of electricity, had to be es-

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tablished after the discovery of the electron in the lower ionosphere and cause radio wave 1897. The discovery of the ionosphere at the propagation and attenuation, similar as en- beginning of the 20th century was another hanced solar x-ray emissions. important step in understanding solar terrestri- Another important space weather effect is the al relations. With the introduction of magnetic excitation of plasma instabilities in the iono- indices by Julius Bartels in 1938 space weath- sphere causing density irregularities, which er effects could be characterized quantitative- affect radio waves as well. ly. The above effects are mainly observed at high The first effects of space weather on technical geographic latitudes. At mid latitudes so systems were observed at the end of the 19th called positive and negative century: disturbances on telegraph lines. effects cause an enhancement/de-pletion of About hundred years later the first effects on electron density. power lines were reported. A true breakthrough of space weather explora- tion occurred towards the end of the 20th cen- tury with observations from satellites and space probes carrying sophisticated instru- mentation and cameras. Tuesday, August 13 The presentation summarizes these steps and highlights important milestones. ______

Ionospheric Response to Geomagnetic Variations, Activity Indices, Space Weather and Thermospheric Response to Magnetic storms Kristian Schlegel Copernicus Gesellschaft e.V., Germany Hermann Lühr After presenting basic facts of the terrestrial German Research Centre for Geosciences ionosphere, a flow chart of impacts of space (GFZ Potsdam) weather on the ionosphere is used to review Most space weather events are accompanied the most important related phenomena: parti- by rapid variations of the geomagnetic field. | cle precipitation and . They both Strong electric currents in the ionosphere and intensify the current systems in the iono- the magnetosphere cause these changing sphere. Besides magnetic disturbances meas- fields. Particularly intense currents flow at urable on the ground, the enhanced currents auroral latitudes in connection with northern cause a heating of the ionosphere, which even- lights. There are a number of geomagnetic tually leads to a heating of the neutral atmos- indices that help to quantify the degree of phere. In addition, magnetospheric convection activity. The Dst index characterises the affects the high altitude wind system. strength of a magnetic storm. At high lati- Another effect related to particle precipitation tudes there is the AE index quantifying the are , their formation will be briefly intensity of the auroralelectrojet. It is a summarized. Precipitation of high-energy measure for the strength. The most electrons and protons after solar flares affect widely used index is Kp. It reflects the gen- Weather Space Joint Summer Camp

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eral degree of magnetic activity. In recent discussed. Examples of lower atmosphere years researchers make preferably use of wave signatures in the ionosphere are shown. direct measurements in the solar wind and in Another source of upper atmosphere variabil- the magnetosphere for modelling space ity is long-term cooling due to changes of mi- weather phenomena, rather than using indi- nor atmospheric constituents like carbon diox- ces. Electric fields set up by the solar wind in ide and ozone. Results of observations and the outer magnetosphere are mapped down modelling are presented. along field lines and cause currents in the auroral ionosphere. The electric currents cause besides the varying magnetic field also a significant heating of the upper atmosphere. As a consequence, air is uplifted and the mass density at given height Wednesday, August 14 is rising. This effect can causes a markedly enhanced air for spacecraft and thus a more rapid orbit decay. The response of the ______neutral thermosphere to magnetic activity will be presented. Cosmic Rays-Fundamentals and Space Weather Effects

Neutral Atmosphere Signature Seen in Ionospheric Variability Erwin O. Flückiger University of Bern

Christoph Jacobi The energy input from cosmic rays into the Leipzig University, Germany system Earth is small, roughly the same as that of starlight. However, continuous galactic and Changes of the upper atmosphere/ionosphere sporadic solar cosmic rays have a multitude of system at different time scales are mainly due effects on terrestrial, biological, and techno- to solar and extraterrestrial variability. How- logical systems. In all scenarios for space ever, the ionosphere is also influenced by weather services cosmic ray measurements are forcing from the neutral atmosphere below, included as a monitoring instrument, as an which may, e.g., lead to additional uncertainty additional forecasting tool, and as a provider in navigation and communication systems. of key input parameters for real time applica-

This forcing is mainly due to atmospheric tions and post-event analysis. The first part of waves at different temporal and spatial scales. the review talk summarizes fundamentals of Waves originating from the lower atmosphere cosmic rays and of their interaction with the may propagate to the upper atmosphere direct- geospace environment. Emphasis is given to ly or indirectly. the role of cosmic ray measurements taken by An overview of neutral atmospheric waves – the global network of ground-based detectors, gravity waves, tides, and planetary waves – is such as neutron monitors. In the second part, presented, including their forcing mechanisms after a general overview of cosmic ray space and climatology. Some of these waves cannot weather effects, the relevance of cosmic ray directly propagate to the ionosphere, and indi- data within space weather programs is dis- rect mechanisms leading to the presence of cussed. Real time ground based cosmic ray

Joint Space Weather Space Joint Summer Camp their signature in the upper atmosphere are observations and advanced analysis methods

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are significant as forecasting tools for geo- al dosimetry for the astronauts is a mandatory magnetic storms, as an alert and monitoring part of the measurement program, which be- instrument of the variability of particle radia- sides the physical characterisation of the ra- tion at the Earth, and as a key element in the diation field has as main task provision of assessment of the radiation do seat aircraft radiation protection measures for the astro- altitude during energetic solar particle events. naut. The measurements are completed by the This will be illustrated, based on selected ex- use of phantoms (spherical and anthromor- amples. phic) to relate the quantities measured by en- vironmental and personal dose meters to ra- diation protection quantitites. The ESA multi- user facility MATROSHKA was designed to Radiation Exposures in Space and provide accurate information on the radiation Aviation Altitudes doses in human organs. The key part of MA- TROSHKA is a human phantom upper torso, equipped with numerous radiation detectors at

the surface and inside the phantom. The facili- Günther Reitz ty therefore allows the determination of the German Aerospace Center (DLR), Cologne empirical relations between measurable ab-

sorbed doses at the skin and the tissue ab- For long term human missions the main con- sorbed doses in different depth inside the cerns are the human physiological responses phantom. to microgravity and radiation. For missions Calculation of radiation risks in the ISS orbits outside the magnetosphere ionising radiation is therefore based on quite reliable data. This is recognized as the key factor through its im- is not the case for interplanetary missions pact on crew health and performance. Of ma- where the exposure rates for planned future jor concern is the exposure of humans by Ga- missions are mostly based on calculations so lactic Cosmic Rays (GCR), because of the still far. Most recently, the radiation assessment in large parts unresolved questions about detector has provided first measurements on unique radiobiological aspects of irradiation the cruise to which no allow to bench- by heavy ions, which results in high uncertain- mark calculations. ties of radiation risk estimates for late radia- Whereas in space radiation exposures can ap- tion effects, like cancer. Solar energetic parti- proach or even exceed radiation limits set for cles released in coronal mass ejections are a radiation workers on Earth, in aviation alti- further concern because exposures are possi- tudes we are far away from such limits, alt- |

ble which can be life threatening if no appro- hough civil aircrew is the highest exposed priate countermeasures are performed. In avia- cohort at all. Exposures here are strongly de- tion altitudes the exposure is dominated by the pending on flight altitudes and latitudes and secondary radiation produced in interactions on the solar activity. of the incoming protons with the molecules of The presentation reviews the physical features the atmosphere, such as neutrons, secondary of the radiation field as far as they relevant for protons, electrons and gamma rays. radiation protection followed by an overview On the ISS a huge set of radiation instruments on exposure data gathered mainly on the ISS is used to monitor the radiation environment and with the Radiation Assessment Detector for a fixed inclination in dependence on alti- of the Mars Science Laboratory (MSL) to- tude, solar activity and shielding distribution. gether with calculations for future human mis- Besides environmental dosimetry also person- sions. Finally, the unique features of heavy Weather Space Joint Summer Camp

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ions will be described, radiobiological effects can be fixed to their integer values. Fugro has observed from space radiation and radiation set up several test beds to investigate the fea- risks for different mission profiles are shown. sibility of this concept, usually referred to as PPP RTK (Real-Time Kinematic) or PPP IAR (Integer Ambiguity Resolution).

Apart from the GNSS signals themselves, the services also rely on correction signals, broad- Thursday, August 15 cast e.g. by geostationary satellites, using fre- quency bands similar to GNSS. A lot of Fugro’s activities take place in areas ______at or near the geomagnetic equator, such as Brazil, West Africa and Southeast Asia. As a Offshore GNSS Positioning result, the GNSS and correction signals are often disturbed or even completely lost, due to Kees de Jong e.g. ionospheric scintillations. Using more Fugro Intersite BV., Netherlands satellite systems, such as GPS, Glonass, Gali- leo and , may help, but it would also Fugro’s mission is to be the world’s leading be beneficial to be able to predict when the service provider for the collection and inter- ionosphere will start behaving badly and pretation of data relating to the Earth’s surface which signals will be affected. and sub-surface, and for associated services In this contribution, we will give an overview and advice in support of infrastructure devel- of Fugro’s current positioning services and opments on land, along the coast and on the present initial results from including BeiDou seabed. Fugro’s activities are carried out and Galileo. We will also present results from across the world, both onshore and offshore, PPP RTK, obtained from a test bed in the Gulf and are primarily aimed at the oil and gas in- of Mexico. Next, we will give a description of dustry, the construction industry and the min- the network monitoring activities. We will ing sector. All these activities require precise conclude with an overview of the activities and reliable positioning, usually in real-time. related to ionospheric monitoring and predic- Fugro provides a number of GNSS (Global tion of scintillations. Navigation Satellite System) positioning ser- vices, mainly for use offshore. In the early 2000’s it introduced the differential, carrier

based HP service, followed by XP, a GPS

only Precise Point Positioning (PPP) service, a Impact of Solar Activity on satellite few years later. In 2009 G2, based on integrat- ed use of GPS and Glonass, became opera- Electronics tional. Current research at Fugro focuses on includ- Stefan Metzger ing the Chinese BeiDou and the European Fraunhofer Institute for Technological Trend Galileo systems in its PPP services. Once Analysis, Germany these systems are operational, more than 100 satellites will be available for high precision positioning applications. Space crafts are vulnerable to space weather Precision can be further improved once the through its influence on the space environ- Joint Space Weather Space Joint Summer Camp ambiguities of the GNSS carrier observations ment. During solar events like flares or coro-

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nal mass ejection the fluxes of high energetic particles in the earth radiation belts can in- crease several orders of magnitude. In addition the flux of galactic cosmic rays is modulated in antiphase with the 11-year solar cycle. As a result the space radiation environment de- pends strongly on the actual space weather. The particles that compose the radiation envi- ronment produce a variety of effects including total dose, lattice displacement damage and single event effects (SEE) as well as noise in sensors. Examples of all the above effects will be given from observed spacecraft anomalies or on-board dosimetry and these demonstrate the need for increased understanding and pre- diction accuracy for space weather as well as the need for protection from the induced phe- nomena. The induced effects are often the origin of satellite anomalies which can at worst lead to the total loss of a satellite.

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Project work in Neustrelitz Project 2 Ionospheric Modelling ______

Mainul M. Hoque German Aerospace Center (DLR), Neustrelitz Project 1 SOFIE – Development and Test of a Single frequency users of Global Navigation VLF-receiver for Monitoring Solar Flares Satellite Systems (GNSS) need to correct link related ionospheric range errors of up to

100m. Since this range error is proportional to Lutz Heinrich, Wolfgang Andree the Total Electron Content (TEC) of the iono- DLR_Project_Lab, Neustrelitz sphere, correction information can be provid- ed by TEC maps deduced from corresponding Natural disturbances of radio communication GNSS measurements or by correction model are known to be connected with space weather values. In this project work, the students will phenomena. Solar Flares can influence long learn about different ionospheric correction waves (LW) over large distances. A simple models such as the NeQuick, the NTCM VLF receiver allows continuous monitoring of (Neustrelitz TEC Model), the GPS Ionospher- signals from far distant transmitters. The anal- ic Correction Algorithm (ICA) also known as ysis of the signal enables simultaneous inves- the Klobuchar model and the International tigation of different space weather related Reference Ionosphere (IRI) model as well as physical phenomena. about TEC maps deduced from GNSS meas- The DLR project lab offers participants to set urements at DLR Neustrelitz. The ionospheric up their own VLF receiver with professional parameters dependencies on solar activity lev- guidance of a school lab supervisor. Partici- el, their annual, semi-annual variation, local pants learn about technical requirements for time variation and varia- receiver and antenna. Each component of the tion will be studied in details. The students receiver and its specific use will be presented will compare TEC values derived from the in detail. One main point is the proper integra- Klobuchar model, the NeQuick model and the tion of single components to the printed circuit NTCM-GL global model with reconstructed board (PC-board) of the receiver. The required TEC map values during daytime and solder techniques will be trained and applied. nighttime in high and low solat activity peri- Afterwards all components will be balanced ods.

and the whole instrument is put into operation.

Finally, after the successful receiver set up, data management is emphasised. The partici- pants learn how to deal with different data formats, the required software and data trans- fer issues. At the end of the project a regular operation is planned, where external users can access data records of a large amount of VLF- receiver at different positions.

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Project 3 rarily lead to increased dose rates at aviation altitudes as well. For the operational dose assessment of air- Scintillation Monitoring crew, computer programs are used, which are Nikolai Hlubek regularly verified and improved by concomi- German Aerospace Center (DLR), Neustrelitz tant measuring flights that allow spot checks of the calculated doses by measuring this Global Navigation Satellite Systems (GNSS) cosmic radiation field with different types of such as GPS, Galileo or Glonass can be heavi- detectors. This project work will give an in- ly disturbed by space weather hazards. Severe sight into the field of radiation protection in temporal and spatial changes of the electron aviation by evaluating such a measuring flight. density in the ionosphere can lead to strong The students learn which dosimetric quantities GNSS signal fluctuations in phase and ampli- can be measured by various detectors and de- tude – so-called scintillations. These scintilla- termine the relevant characteristics of the radi- tions can reduce the positioning accuracy sig- ation field at cruising altitudes. Finally, the nificantly and in the worst cases lead to a re- space weather situation during the flight is to ceiver loosing lock of the satellite signal. be considered. The scintillation indices S4 and σφ provide a characteristic quantity that shows the strength of the scintillation. In this project work the students will learn how to derive and visualize said indices from real data sets using the Py- thon programming language.

Project 4 Aviation Dosimetry Nicole Santen

German Aerospace Center (DLR), Cologne

| The determination of the radiation exposure of aircrew at aviation altitudes, generated by in- teractions of primary high-energetic particles of cosmic origin with atoms in upper layers of the Earth’s atmosphere, has been part of the radiation protection standards in the EU for more than ten years. The corresponding radia- tion field is very complex in both particle composition and energy distribution. The cor- responding intensity depends on altitude, ge- omagnetic latitude and solar activity. Further-

more, Solar Particle Events (SPEs) can tempo- Weather Space Joint Summer Camp

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