(ISIS): Design of the Energetic Particle Investigation
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Program Book Update
15th Annual International Astrophysics Conference Cape Coral, FL – April 3-8, 2016 AGENDA SUNDAY, APRIL 3 5:00 PM – 8:00 PM Registration – Tarpon Terrace 6:00 PM – 9:00 PM Welcome Reception - Tarpon Terrace MONDAY, APRIL 4 7:00 AM - 5:00 PM Registration – Grandville Ballroom 8:00 AM – 6:00 PM GENERAL SESSION – Grandville Ballroom CHAIR: Zank 7:45 AM - 8:00 AM GARY ZANK WELCOME 8:00 AM - 8:25 AM Chen, Bin Particle Acceleration by a Solar Flare Termination Shock 8:25 AM - 8:50 AM Bucik, Radoslav Large-scale Coronal Waves in 3He-rich Solar Energetic Particle Events Element Abundances and Source Plasma Temperatures of 8:50 AM - 9:15 AM Reames, Donald Solar Energetic Particles 9:15 AM - 9:40 AM Manchester, Ward Simulating CME-Driven Shocks and Implications for SEPs STEREO and ACE SEP Science- Transforming Space Weather 9:40 AM - 10:05 AM Luhmann, Janet Prospects 10:05 AM - 10:30 AM Morning Break - Ballroom Foyer CHAIR: Zirnstein 11 years of ENA imaging with Cassini/INCA and in-situ ion Voyager1 & 10:30 AM - 10:55 AM Krimigis, Stamatios 2/LECP measurements Investigating the Heliospheric Boundary at Energies down to 10eV with 10:55 AM - 11:20 AM Wurz, Peter Neutral Atom Imaging by IBEX. In-situ and Remote Sensing Studies of Solar Wind Origin and 11:20 AM - 11:45 AM Landi, Enrico Acceleration The Sun’s Dynamic Influence on the Outer Heliosphere, the Heliosheath, 11:45 AM - 12:10 PM Intriligator, Devrie and the Local Interstellar Medium 12:10 PM – 1:30 PM Lunch Break – Ballroom Foyer CHAIR: Fichtner 1:30 PM - 1:55 PM McNutt, Ralph Making Interstellar -
Spaceflight a British Interplanetary Society Publication
SpaceFlight A British Interplanetary Society publication Volume 61 No.2 February 2019 £5.25 Sun-skimmer phones home Rolex in space Skyrora soars ESA uploads 02> to the ISS 634089 From polar platform 770038 to free-flier 9 CONTENTS Features 18 Satellites, lightning trackers and space robots Space historian Gerard van de Haar FBIS has researched the plethora of European payloads carried to the International Space Station by SpaceX Dragon capsules. He describes the wide range of scientific and technical experiments 4 supporting a wide range of research initiatives. Letter from the Editor 24 In search of a role Without specific planning, this Former scientist and spacecraft engineer Dr Bob issue responds to an influx of Parkinson MBE, FBIS takes us back to the news about unmanned space vehicles departing, dying out and origins of the International Space Station and arriving at their intended explains his own role in helping to bring about a destinations. Pretty exciting stuff British contribution – only to see it migrate to an – except the dying bit because it unmanned environmental monitoring platform. appears that Opportunity, roving around Mars for more than 14 30 Shake, rattle and Rolex 18 years, has finally succumbed to a On the 100th anniversary of the company’s birth, global dust storm. Philip Corneille traces the international story Some 12 pages of this issue are behind a range of Rolex watches used by concerned with aspects of the astronauts and cosmonauts in training and in International Space Station, now well into its stride as a research space, plus one that made it to the Moon. -
Solar Probe Plus (SPP)
Pre-decisional – For NASA Internal Use Only Solar Probe Plus (SPP) Committee on Solar and Space Physics 5 October 2016 Joe Smith Program Executive NASA Headquarters 5 October 2016 1 Solar Probe Plus (SPP) Overview Using in-situ measurements made closer to the Sun than by any previous spacecraft, SPP will determine the mechanisms that produce the fast and slow solar winds, coronal heating, and the transport of energetic particles. Solar Probe Plus will fly to less than 10 solar radii (Rs) of the Sun, having “walked in” from 35 Rs over 24 orbits. Milestones • Sponsor: NASA/GSFC LWS Pre-Phase A: 07/2008 – 11/2009 • LWS Program Manager – Nick Chrissotimos GSFC • LWS Deputy Program Manager – Mark Goans, GSFC Phase A: 12/2009 – 01/2012 • Project Manager – Andy Driesman, APL Phase B: 02/2012 – 03/2014 • Project Scientist – Nicky Fox, APL Phase C/D: 03/2014 – 09/2018 • Spacecraft Development/Operations – APL LRD: 31 July 2018 • Investigations selected by AO: • FIELDS – University of California Phase E: 10/2018 – 09/2025 • ISIS – Princeton University/SwRI • SWEAP – Smithsonian Astrophysical Obs Management Commitment: $1,366M • WISPR – Naval Research Laboratory Category 1, Risk Classification B • HelioOrigins – Jet Propulsion Laboratory 5 October 2016 Solar Probe Plus CSSP 2 50 years into the space age and we still don’t understand the corona and solar wind . The concept for a “Solar Probe” dates back to “Simpson’s Committee” of the Space Science Board (National Academy of Sciences, 24 October 1958) ‒ The need for extraordinary knowledge of Sun from remote observations, theory, and modeling to answer the questions: – Why is the solar corona so much hotter than the photosphere? – How is the solar wind accelerated? . -
David J. Mccomas - Refereed Publications
David J. McComas - Refereed Publications 1982 1. McComas, D.J. and S.J. Bame, Radially Uniform Electron Source, Rev. of Sci. Instrum., 53, 1490-1491, 1982. 2. Feldman, W.C., S.J. Bame, S.P. Gary, J.T. Gosling, D.J. McComas, M.F. Thomsen, G. Paschmann, N. Sckopke, M.M. Hoppe, C.T. Russell, Electron Heating Within the Earth's Bowshock, Phys. Rev. Lett., 49, 199-201,1982. 1983 3. Feldman, W.C., R.C. Anderson, S.J. Bame, S.P. Gary, J.T. Gosling, D.J. McComas, M.F. Thomsen, G. Paschmann, M.M. Hoppe, Electron Velocity Distributions Near the Earth's Bowshock, J. Geophys. Res., 88, 96-110, 1983. 4. Bame, S.J., R.C. Anderson, J.R. Asbridge, D.N. Baker, W.C. Feldman, J.T. Gosling, E.W. Hones, Jr., D.J. McComas, R.D. Zwickl, Plasma Regimes in the Deep Geomagnetic Tail: ISEE-3, Geophys. Res. Lett., 10, 912-915, 1983. 1984 5. McComas, D.J. and S.J. Bame, Channel Multiplier Compatible MaterialsLifetime Tests, Rev. Sci. Inst., 55, 463-467, 1984. 6. Hones, Jr., E.W., D.N. Baker, S.J. Bame, W.C. Feldman, J.T. Gosling, D.J. McComas, R.D. Zwickl, J.A. Slavin., E.J. Smith, B.T. Tsurutani, Structure of the Magnetotail at 220RE its Response to Geomagnetic Activity, Geophys. Res. Lett., 11, 5-7, 1984. 7. Baker, D.N., S.J. Bame, W.C. Feldman, J.T. Gosling, P.R. Higbie, E.W. Hones, Jr., D.J. McComas, R.D. Zwickl, Correlated Dynamical Changes in the Near Earth and Distant Magnetotail Regions: ISEE-3, J. -
WISPR (Wide Field Imager for Solar Probe Plus)
WISPR (Wide Field Imager for Solar Probe Plus) V. Bothmer, R. A. Howard (WISPR PI), A. Vourlidas 22 May 2015 Solar Probe Plus A NASA Mission to Touch the Sun HELCATS First Annual Open Workshop What is Solar Probe Plus (SPP) . Goes to the last unexplored region of the solar system and enter the solar corona as close as 9.86 Rs . Will answer fundamental questions of Heliophysics: The heating of the solar corona The origin, structure and evolution of the solar wind Origin of solar energetic particles . Investigations: FIELDS: measurements of magnetic fields, AC/DC electric fields SWEAP: measurements of flux of electrons, protons and alphas ISIS: measurement of solar energetic particles WISPR: measurement of coronal structures Observatory Scientist HELCATS First Annual Open Workshop SPP Mission Scenario – Observations from 0.25 AU to 9.86 RS HELCATS First Annual Open Workshop 3 SPP Near Sun Perihel Passages Number of Perihel passages < 30 RS (0.14 AU): • First Perihel at 35 RS (0.16 AU) after 88 days • 24 Perihel-passages over the time periofd of 7 years after launch in July 2018 • 1000 hrs of measurements at distances < 20 RS Ref.: NASA STDT HELCATS First Annual Open Workshop 4 Solar Probe Plus Encounter Portion of the Orbit 9.86 Rs HELCATS First Annual Open Workshop Figure 4.2 – Encounter Pass Geometry and Timeline The Deep Space Network (DSN) will be used to communicate with the SPP observatory and collect data required for navigation. Mission operations will be conducted at APL from a single Mission Operations Center (MOC), located at the Johns Hopkins University Applied Physics Laboratory (JHU/APL) in Laurel, Maryland. -
Parker Solar Probe Project Scientist JHU/Applied Physics Laboratory Parker Solar Probe
The Coolest, Hottest Mission under the Sun!! Dr. Nicola J. Fox Parker Solar Probe Project Scientist JHU/Applied Physics Laboratory Parker Solar Probe A NASA Mission to Touch the Sun We are PARKER SOLAR PROBE! Parker, meet Parker December 12, 2017 Parker Solar Probe– Fall AGU 2017 Why haven’t we gone to the Sun yet? It took the same technological leap from a rotary phone to an iPhone X for Parker Solar Probe to become a reality December 12, 2017 Parker Solar Probe– Fall AGU 2017 Parker Solar Probe Science . To determine the structure and dynamics of the Sun’s coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what mechanisms accelerate and transport energetic particles. Detailed Science Objectives • Trace the flow of energy that heats and accelerates the solar corona and solar wind. • Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind. • Explore mechanisms that accelerate and transport energetic particles. November 16, 2017 Parker Solar Probe Mission Briefing Modeling: Providing the missing piece . In-situ data from within 0.25 AU will be available Manchester 2014 shortly after each orbit for ingestion into the coronal, solar wind and global heliospheric models . PSP would also benefit invaluably from knowing the mapping between the spacecraft and the solar surface though each orbit . Global simulations of CMEs would provide critical context when we fly through CMEs . Contact [email protected] or [email protected] Baker -
Parker Solar Probe Through the First Two Solar Orbits
30th Annual Thermal & Fluids Analysis Workshop TFAWS 2019, 26-30 August 2019 Newport News, VA Post-Launch and Early Mission Thermal Performance of Parker Solar Probe through the First Two Solar Orbits TFAWS19-AT-07 Carl J Ercol [email protected] G. Allan Holtzman Parker Solar Probe [email protected] A NASA Mission to Touch the Sun 30th Annual Thermal & Fluids Analysis Workshop 26-30 August 2019, Newport News, VA Parker Solar Probe Mission Summary Overview Using in-situ measurements made closer to the Sun than by any previous spacecraft, Parker Solar Probe (PSP) will determine the mechanisms that produce the fast and slow solar winds, coronal heating, and the transport of energetic particles. PSP will fly to 9.86 solar radii (Rs) of the Sun, having “walked in” from 35.7 Rs over 24 orbits, two of which have been completed to date. Sponsor: NASA SMD/Heliophysics Div Preliminary Mission Milestones • Program Office – GSFC/LWS • Project Scientist - APL Pre-Phase A: 07/2008 – 11/2009 • Project Management - APL Phase A: 12/2009 – 01/2012 • S/C Development & Operations – APL Phase B: 02/2012 – 03/2014 • Science Investigations selected by AO: Phase C/D: 03/2014 – 12/2018 • SWEAP - Smithsonian Astrophysical Observatory • FIELDS - UC Berkeley Phase E: 01/2019 – 09/2025 • WISPR - Naval Research Laboratory Launched: August 12, 2018, 07:31 UTC • ISʘIS – Southwest Research Institute 30th Annual Thermal & Fluids Analysis Workshop 26-30 August 2019, Newport News, VA Trajectory: 9.86Rs Minimum Perihelion . Launch 13-day launch period from Aug 11 to Aug 23, 2018 Maximum launch C3 of 154 km2/s2 S/C wet mass 685 kg Launch system: Delta-IVH Class + Star48 BV . -
MULTI-SCALE THERMAL and STRUCTURAL CHARACTERIZATION of CARBON FOAM for the PARKER SOLAR PROBE THERMAL PROTECTION SYSTEM by Eliza
MULTI-SCALE THERMAL AND STRUCTURAL CHARACTERIZATION OF CARBON FOAM FOR THE PARKER SOLAR PROBE THERMAL PROTECTION SYSTEM by Elizabeth Ann Congdon A dissertation submitted to the Johns Hopkins University in conformity with the requirements for the degree of Doctor of Philosophy Baltimore, Maryland February 2021 ABSTRACT Since the founding of the National Aeronautics and Space Administration (NASA), a top mission priority has been to study the Sun in situ. For sixty years, this mission remained just an aspiration of heliophysicists due to the inherent limitations of the engineering technology required to make the mission possible. One critical spacecraft element is the thermal protection system (TPS) or heat shield, a low mass self- supporting structure that required implementation of a structurally integral insulation sandwich panel. For this multifunctional sandwich panel approach to be successful, the thermal and structural properties of the main insulative core, carbon foam, needed to be understood to validate that the TPS could survive the launch loading and the extreme temperatures at its perihelion. An extensive test program including coupon, subscale and full-scale evaluation was undertaken to determine the properties of this low-density lattice and to compliment full-scale modeling. Candidate foams, ranging from 3% to 10% relative density, were evaluated using both the guarded hot plate method and thermal diffusivity methods for effective thermal conductivity. The effective thermal conductivity was primarily driven by solid conductivity around room temperature and shown to follow simple Gibson and Ashby predictions. At temperatures beyond 900°C, radiation was much more important and the test data diverged from the model. -
A Mission to Touch the Sun
A Mission to Touch the Sun Presented by: David Malaspina Based on a huge amount of work by the NASA, APL, FIELDS, SWEAP, WISPR, ISOIS teams Who am I? Recent Space Plasma Group Missions: Van Allen Probes Assistant Professor in: Magnetospheric MultiScale (MMS) Professional Researcher in the Space Plasma Group (SPG) at: Parker Solar Probe Space Plasma Physicist Studying: The Solar Wind Planetary Magnetospheres Planetary Ionospheres Plasma Waves MAVEN Electric Field Sensors Spacecraft Charging A Tale in Four Acts [1] History - How do we know that a solar wind exists? - Why do we care? - What have we learned about the solar wind? [2] Solar Wind Science - Key unanswered questions - The need for a Solar Probe [3] Preparing a Mission - A battle for funding - Mission design - Instrument design [4] A Mission to Touch the Sun - Launch - First orbits - First results Per Act: The future ~10-15 min talk + - ~5-10 min questions Act 0: Terminology Plasma: A gas so hot, the atoms separate into electrons and ions - Ionization Common plasmas: - The Sun - Lightning plasma - Neon signs, fluorescent lights - TIG welders / Plasma cutters Plasmas have complicated motions: Fluid motion and electromagnetic motion Magnetic Field Simplest magnetic fields are dipoles north and south pole Iron filings “trace” magnetic field of a bar magnet by aligning with the field Sun Plasmas and magnetic fields Electrons and ions follow magnetic field lines in helical paths Earth Plasmas “trace” magnetic field lines Act 1: History Where to start? 1859 : The Colorado Gold Rush In 1858: 620 g of gold found in Little Dry Creek (now Englewood, CO) By 1860: ~100,000 gold-seekers had moved to Colorado 1858: City of Denver founded 1859: Boulder City Town Company organized https://en.wikipedia.org/wiki/History_of_Denver https://bouldercolorado.gov/visitors/history ‘‘On the night of [September 1] we were high up on the Rocky Mountains sleeping in the open air. -
19Th Annual International Astrophysics Conference Oral Abstracts
19TH ANNUAL INTERNATIONAL ASTROPHYSICS CONFERENCE ORAL ABSTRACTS Adhikari, Laxman Evolution of Entropy and Mediation of the Solar Wind by Turbulence Laxman Adhikari, CSPAR/UAH, USA Gary P. Zank, UAH/CSPAR, USA Lingling Zhao, CSPAR/UAH, USA Gary M. Webb, CSPAR/UAH, USA We study the evolution of solar wind entropy based on a conservative formulation of solar wind and turbulence transport model equations, and compare the model results to Voyager 2 measurements. For a polytropic index of γ = 5/3 (> 1), entropy increases with distance due to the dissipation of turbulence, being about 12.84% higher at 75 au than at 1 au. However, if the polytropic index satisfies γ < 1, entropy decreases. We show that not only the creation of pickup ions, but also stream‐shear leads to a decrease of the solar wind speed. We show that the sum of the solar wind flow energy (kinetic plus enthalpy) and turbulent (magnetic) energy is constant, indicating that kinetic solar wind energy is transferred into turbulent energy via stream‐shear and pickup ion isotropization, which then in turn heats the solar wind via the dissipation of turbulence. We compare the theoretical solutions of the solar wind entropy, the solar wind density, the thermal gas pressure, the solar wind proton temperature, and the fluctuating magnetic energy with those measured by Voyager 2. The results show that the theoretical results are in good agreement with the observed results. Asgari‐Targhi, An Observational Study of the Role of Flux Emergence, Flux Cancellation, and Non‐Potential Fields in the Heating of Active‐Region Loops Mahboubeh Mahboubeh Asgari‐Targhi, Harvard‐Smithsonian Center for Astrophysics, USA We study the high‐temperature (T>4 MK) emissions from mostly non‐flaring active regions using extreme ultraviolet images from the Atmospheric Imaging Assembly on the Solar Dynamic Observatory (SDO). -
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Kasper, Justin C., Robert Abiad, Gerry Austin, Marianne Balat- Pichelin, Stuart D. Bale, John W. Belcher, Peter Berg, et al. “Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus.” Space Sci Rev (October 29, 2015). As Published http://dx.doi.org/10.1007/s11214-015-0206-3 Publisher Springer Netherlands Version Final published version Citable link http://hdl.handle.net/1721.1/107474 Terms of Use Creative Commons Attribution Detailed Terms http://creativecommons.org/licenses/by/4.0/ Space Sci Rev DOI 10.1007/s11214-015-0206-3 Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus Justin C. Kasper1,2 · Robert Abiad3 · Gerry Austin2 · Marianne Balat-Pichelin4 · Stuart D. Bale3 · John W. Belcher5 · Peter Berg3 · Henry Bergner2 · Matthieu Berthomier6 · Jay Bookbinder2 · Etienne Brodu4 · David Caldwell2 · Anthony W. Case2 · Benjamin D.G. Chandran7 · Peter Cheimets2 · Jonathan W. Cirtain8 · Steven R. Cranmer9 · David W. Curtis3 · Peter Daigneau2 · Greg Dalton3 · Brahmananda Dasgupta10 · David DeTomaso11 · Millan Diaz-Aguado3 · Blagoje Djordjevic3 · Bill Donaskowski3 · Michael Effinger8 · Vladimir Florinski10 · Nichola Fox11 · Mark Freeman2 · Dennis Gallagher8 · S. Peter Gary12 · Tom Gauron 2 · Richard Gates2 · Melvin Goldstein13 · Leon Golub2 · Dorothy A. Gordon3 · Reid Gurnee11 · Giora Guth2 · Jasper Halekas14 · Ken Hatch3 · Jacob Heerikuisen10 · George Ho11 · Qiang Hu10 · Greg Johnson3 · Steven P. -
Design and Optimization of a High-Time-Resolution Magnetic Plasma Analyzer (MPA)
applied sciences Article Design and Optimization of a High-Time-Resolution Magnetic Plasma Analyzer (MPA) Benjamin Criton 1,*,† , Georgios Nicolaou 1,2 and Daniel Verscharen 1,3 1 Mullard Space Science Laboratory, Department of Space and Climate Physics, University College London, Dorking, Surrey RH5 6NT, UK; [email protected] (G.N.); [email protected] (D.V.) 2 Southwest Research Institute, San Antonio, TX 78238, USA 3 Space Science Center, University of New Hampshire, Durham, NH 03824, USA * Correspondence: [email protected] † Current address: IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France. Received: 3 November 2020; Accepted: 24 November 2020; Published: 27 November 2020 Featured Application: This instrument concept is designed to analyze plasma onboard scientific spacecraft. Its measurements allow the construction of the velocity distribution functions of protons and a-particles with high cadence to understand the small-scale kinetic processes in space plasmas. Abstract: In-situ measurements of space plasma throughout the solar system require high time resolution to understand the plasma’s kinetic fine structure and evolution. In this context, research is conducted to design instruments with the capability to acquire the plasma velocity distribution and its moments with high cadence. We study a new instrument design, using a constant magnetic field generated by two permanent magnets, to analyze solar wind protons and a-particles with high time resolution. We determine the optimal configuration of the instrument in terms of aperture size, sensor position, pixel size and magnetic field strength. We conduct this analysis based on analytical calculations and SIMION simulations of the particle trajectories in our instrument.