2001/02/08T E Moore - SW Interactions via LENA1 Solar Wind-Magnetosphere Interactions via Low Energy Neutral Atom Imaging T E Moore[1], M R Collier[1],

Slides:

Advertisements

Similar presentations

Abstract Real-time images of Earths space environment from NASAs IMAGE satellite will soon be available on the NOAA Space Environment Center Web site.

Advertisements

First composition measurements of energetic neutral atoms A. T. Y. Lui et al., GRL, Vol 23, pages: , 1996.

U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Direct measurements of chorus wave effects on electrons in the.

Anti-Parallel Merging and Component Reconnection: Role in Magnetospheric Dynamics M.M Kuznetsova, M. Hesse, L. Rastaetter NASA/GSFC T. I. Gombosi University.

Ion Equatorial Distributions from Energetic Neutral Atom Images Obtained From IMAGE during Geomagnetic Storms Zhang, X. X., J. D. Perez, M.-C. Fok D. G.

ESS 7 Lecture 14 October 31, 2008 Magnetic Storms

The role of solar wind energy flux for transpolar arc luminosity A.Kullen 1, J. A. Cumnock 2,3, and T. Karlsson 2 1 Swedish Institute of Space Physics,

Spatial distribution of the auroral precipitation zones during storms connected with magnetic clouds O.I. Yagodkina 1, I.V. Despirak 1, V. Guineva 2 1.

Magnetopause flow vortices revealed during high speed solar wind streams Mona Kessel (NASA GSFC), Yaireska Collado-Vega (University of Puerto Rico), Xi.

Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,

Non-Equilibrium Ionization Modeling of the Current Sheet in a Simulated Solar Eruption Chengcai Shen Co-authors: K. K. Reeves, J. C. Raymond, N. A. Murphy,

Identification and Analysis of Magnetic Substorms Patricia Gavin 1, Sandra Brogl 1, Ramon Lopez 2, Hamid Rassoul 1 1. Florida Institute of Technology,

Summer student work at MSSL, 2009 Kate Husband – investigation of magnetosheath electron distribution functions. Flat-topped PSD distributions, correlation.

Storm-Time Dynamics of the Inner Magnetosphere: Observations of Sources and Transport Michelle F. Thomsen Los Alamos National Laboratory 27 June 2003.

CISM Radiation Belt Models CMIT Mary Hudson CISM Seminar Nov 06.

Lecture 3 Introduction to Magnetic Storms. An isolated substorm is caused by a brief (30-60 min) pulse of southward IMF. Magnetospheric storms are large,

Solar system science using X-Rays Magnetosheath dynamics Shock – shock interactions Auroral X-ray emissions Solar X-rays Comets Other planets Not discussed.

What DMSP Data Tell us About the Thermosphere Response to Solar Wind Forcing Delores Knipp CU Aerospace Engineering Sciences and NCAR HAO With Assistance.

Location of Magnetopause Reconnection S M Petrinec 1, S A Fuselier 1, K J Trattner 1, and J Berchem 2 1 Lockheed Martin Advanced Technology Center, Palo.

Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland

Benoit Lavraud CESR/CNRS, Toulouse, France Uppsala, May 2008 The altered solar wind – magnetosphere interaction at low Mach numbers: Magnetosheath and.

The Sun and the Heliosphere: some basic concepts…

1 Saturn Aurora: The ionospheric and magnetospheric fingerprint, and a manifestation of interactions beyond. Saturn Aurora: The ionospheric and magnetospheric.

Numerical simulations are used to explore the interaction between solar coronal mass ejections (CMEs) and the structured, ambient global solar wind flow.

Computer Simulations in Solar System Physics Mats Holmström Swedish Institute of Space Physics (IRF) Forskarskolan i rymdteknik Göteborg 12 September 2005.

The First Two Years of IMAGE Jim Burch Southwest Research Institute Magnetospheric Imaging Workshop Yosemite National Park, California February 5-8, 2002.

Magnetosphere-Ionosphere coupling processes reflected in

14 May JIM M. RAINES University of Michigan DANIEL J. GERSHMAN, THOMAS H. ZURBUCHEN, JAMES A. SLAVIN, HAJE KORTH, and BRIAN J. ANDERSON Magnetospheric.

Faraday Rotation: Unique Measurements of Magnetic Fields in the Outer Corona Justin C. Kasper (UM), Ofer Cohen (SAO), Steven Spangler (Iowa), Gaetan Le.

Localized Thermospheric Energy Deposition Observed by DMSP Spacecraft D. J. Knipp 1,2, 1 Unversity of Colorado, Boulder, CO, USA 2 High Altitude Observatory,

PAPER I. ENA DATA ANALYSIS RESULTS. The Imager for Magnetopause-to- Aurora Global Exploration (IMAGE) missionis the first NASA Mid-size Explorer (MIDEX)

POST CME EVENTS: COOL JETS AND CURRENT SHEET EVOLUTION A. Bemporad, G. Poletto, S. T. Suess IAU Symposium 226 Coronal and Stellar Mass Ejections September.

Earth’s Magnetosphere NASA Goddard Space Flight Center

Universal Processes in Neutral Media Roger Smith Chapman Meeting on Universal Processes Savannah, Georgia November 2008.

Effective drift velocity and initiation times of interplanetary type-III radio bursts Dennis K. Haggerty and Edmond C. Roelof The Johns Hopkins University.

Scott Thaller Van Allen Probes EFW meeting University of Minnesota June 10-12, 2014.

Guan Le NASA Goddard Space Flight Center Challenges in Measuring External Current Systems Driven by Solar Wind-Magnetosphere Interaction.

Space Weather in Earth’s magnetosphere MODELS  DATA  TOOLS  SYSTEMS  SERVICES  INNOVATIVE SOLUTIONS Space Weather Researc h Center Masha Kuznetsova.

NASA NAG Structure and Dynamics of the Near Earth Large-Scale Electric Field During Major Geomagnetic Storms P-I John R. Wygant Assoc. Professor.

Global Structure of the Inner Solar Wind and it's Dynamic in the Solar Activity Cycle from IPS Observations with Multi-Beam Radio Telescope BSA LPI Chashei.

The observed direction of the interstellar neutral atoms will be in the direction of their velocity vectors (tangent to the orbit); the magnitude of the.

IMAGE: Imager for Magnetopause-to-Aurora Global Exploration Goddard Space Flight Center Scientific Colloquium February 23, 2001.

Multi-Spacecraft Observation of Compressional Mode ULF Waves Excitation and Relativistic Electron Acceleration X. Shao 1, L. C. Tan 1, A. S. Sharma 1,

The effects of the solar wind on Saturn’s space environment

Magnetically Self-Consistent Simulations of Ring Current with Implications for Diffuse Aurora and PIXIE Data Interpretation Margaret W. Chen 1 and Michael.

1 CHARM: MAPS highlights CHARM: MAPS highlights 2010.

SS Special Section of JGR Space Physics Marks Polar’s 5th Anniversary September 4, 1996 This April special section is first of two Polar special sections.

Space Science MO&DA Programs - April Page 1 SS Special Section of JGR Space Physics Marks Polar’s 5th Anniversary September 4, 1996 This April special.

Energy inputs from Magnetosphere to the Ionosphere/Thermosphere ASP research review Yue Deng April 12 nd, 2007.

Earth’s Magnetosphere Space Weather Training Kennedy Space Center Space Weather Research Center.

30 April 2009 Space Weather Workshop 2009 The Challenge of Predicting the Ionosphere: Recent results from CISM. W. Jeffrey Hughes Center for Integrated.

A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.

Source and seed populations for relativistic electrons: Their roles in radiation belt changes A. N. Jaynes1, D. N. Baker1, H. J. Singer2, J. V. Rodriguez3,4.

Interplanetary proton and electron enhancements associated with radio-loud and radio-quiet CME-driven shocks P. Mäkelä 1,2, N. Gopalswamy 2, H. Xie 1,2,

Dynamics of the auroral bifurcations at Saturn and their role in magnetopause reconnection LPAP - Université de Liège A. Radioti, J.-C. Gérard, D. Grodent,

Data-Model Comparisons

CEDAR Frontiers: High-Latitude Neutral Outflow Larry Gardner – Utah State University – Robert Schunk – Utah State University –

The Ionosphere and Thermosphere GEM 2013 Student Tutorial

Characterization of Field Line Topologies Near the Magnetopause Using Electron Pitch Angle Measurements D. S. Payne1, M. Argall1, R. Torbert1, I. Dors1,

GOMOS measurements of O3, NO2, and NO3 compared to model simulations

Global MHD Simulations of Dayside Magnetopause Dynamics.

Introduction to Space Weather Interplanetary Transients

Energetic Neutral Atom Imaging of

THEMIS multi-spacecraft observations of a 3D magnetic

Effects of Dipole Tilt Angle on Geomagnetic Activities

Solar and Heliospheric Physics

High Latitude Oxygen LENA

F. Brent Sadler1, A. Otto2, Marc R. Lessard1, Eric Lund1, H. Lühr3 , J

Richard B. Horne British Antarctic Survey Cambridge UK

by Andreas Keiling, Scott Thaller, John Wygant, and John Dombeck

Presentation transcript:

2001/02/08T E Moore - SW Interactions via LENA1 Solar Wind-Magnetosphere Interactions via Low Energy Neutral Atom Imaging T E Moore[1], M R Collier[1], M-C Fok[1], S A Fuselier[2], D. G. Simpson[1], G. R. Wilson[3], M. O. Chandler[4] 1. NASA’s Goddard Space Flight Center, Interplanetary Physics Branch, Code 692, Greenbelt, MD Lockheed Martin Advanced Technology Center, Dept. H1-11, Bldg. 255, Palo Alto, CA Mission Research Corporation, 589 W. Hollis St., Suite 201, Nashua, NH National Space Science and Technology Center, NASA MSFC SD50, Huntsville AL LENA was motivated by need for time-resolved ionospheric outflow observations. Also responds to neutral atoms with energies up to a few keV (from sputtering). As a result, we have been able to: -Show that ionospheric outflow responds to solar wind dynamic pressure variations. -Observe that the response is prompt. -Infer a heating source below 1000 km altitude for the larger flux events. -Use neutral atom emissions to reveal the magnetosheath, with cusp-related structures. -Infer dayside structure in the geocorona.. -Measured the annual variation of the neutral solar wind. -Probe the interstellar gas and dust in the inner solar system. -Directly observe the interstellar neutral atom focusing cone at 1 AU. LENA imaging has thus proven to be a promising new tool for studying the interplanetary medium and its interaction with the magnetosphere, even from inside the magnetosphere.

2001/02/08T E Moore - SW Interactions via LENA2 Low Energy Neutral Atoms (LENA) CME/Storm Onset and Response Solar Wind LENA increase marks CME arrival at 0915 hrs. Earth sector LENA respond within travel time of 35eV O 0. Hr Before Hr After Snap Perigee

2001/02/08T E Moore - SW Interactions via LENA3 Comparison with Ion Outflows Preliminary comparisons: -Some spatial correspondence (day - night here) -Flux comparison indicates low altitude source region -Best correspondence w/ auroral oval from transverse views (not shown) -Posters AGUsm01: SM72A-14 (Coffey et al.), -15(Wilson et al.) LENA H/O/Total ImagesTIDE Polar Ion OutflowsNeutral Fraction vs Source Altitude

2001/02/08T E Moore - SW Interactions via LENA4 Simulated LENA Emissions Auroral zone emissions Uniform polar emissions

2001/02/08T E Moore - SW Interactions via LENA5 Sources of Indirect SW-LENA Collier et al. Nov JGR p.24,893

2001/02/08T E Moore - SW Interactions via LENA6 Solar LENA flux profile Strong similarity to ram pressure profile observed at WIND. Tracking observed at some time scales, not others.

2001/02/08T E Moore - SW Interactions via LENA7 Simulation of Indirect LENAs Simulations performed by M.-C. Fok using MHD magnetosheath. Analogous to ring current ENA simulations, using an CCMC (BatsRUS) MHD model of the magnetosheath, and looking out. LOS integration from 8 to 50 R E, excepting antisunward 90° cone. Images collapsed in polar angle, for IMAGE. No true solar LENAs assumed to arrive in solar wind here. Dawn-Dusk Orbit Noon-Midnight Orbit Dawn-Dusk Orbit 200 eV4000 eV

2001/02/08T E Moore - SW Interactions via LENA8 Solar wind flux or dynamic pressure increases produce a big reaction in LENA. A brightening is seen especially between the sun pulse and the Earth (white line here). Is this the expected relation between solar wind intensity and ENA emission from this region?

2001/02/08T E Moore - SW Interactions via LENA9 We expect a very strong dependence because so many factors are affected by solar wind flux (and Pd).

2001/02/08T E Moore - SW Interactions via LENA10 Simulation of Magnetosheath CE CCMC Simulations based on BatsRUS Code LOS integration from IMAGE spacecraft by M-C Fok. Consider periods of enhanced Pd solar wind for compressed magnetopause. Remote sensing of cusp and cleft possible with sufficient sensitivity and-or Pd.

2001/02/08T E Moore - SW Interactions via LENA11

2001/02/08T E Moore - SW Interactions via LENA12 Seeing Magnetosheath Structure LENA spin modulation near the peak of the 31 March 2001 event at about 0450UT: CCMC (BatsRUS) MHD simulation of the 31 March 2001 event, showing magnetosheath density distribution along LENA lines of sight at about 0450 UT

2001/02/08T E Moore - SW Interactions via LENA13 Remote-Sensing the Magnetosheath Sun MS Simulations indicate features of the magnetosheath should be visible and are visible from inside the magnetosphere.

2001/02/08T E Moore - SW Interactions via LENA14 Evidence for Geocoronal Erosion? 5-50 RE 5-12 RE Data: LENA background adjusted flux > 30 eV Deflectors

2001/02/08T E Moore - SW Interactions via LENA15 Long term, seasonal variations reflect solar system distribution of neutral gas (interstellar and other sources) Short term, storm variations reflect solar wind intensity variations, CMEs, and distribution of the geocorona.

2001/02/08T E Moore - SW Interactions via LENA16 SW ENA Model of Bzowski et al. Icarus 1996

2001/02/08T E Moore - SW Interactions via LENA17 Limit on Inner Solar System Dust Collier et al., AGU SM2001

2001/02/08T E Moore - SW Interactions via LENA18 Predicted Direct ISN Observations Fuselier, 1997

2001/02/08T E Moore - SW Interactions via LENA19 Direct ISNs, Interpreted?

2001/02/08T E Moore - SW Interactions via LENA20 3D Interstellar Neutral Trajectories

2001/02/08T E Moore - SW Interactions via LENA21 ISN Flux 12/11/12/1 3/1 12/1 1/1 2/1 3/1

2001/02/08T E Moore - SW Interactions via LENA22 Conclusions We have been able to: -Validate earlier statistical inferences that ionospheric heating responds to solar wind dynamic pressure variations. -Observe that the response is prompt, as fast as hydromagnetic wave propagation speeds. -Infer that the heating source must lie lower than 1000 km altitude for the larger flux events. -Use neutral atom emissions to reveal the magnetosheath, with cusp-related structures. -Infer dayside structure in the geocorona, owing to solar wind erosion by charge exchange. -Measure the annual variation of the neutral solar wind. -Interpret annual variation in terms of interstellar neutral gas and dust in the inner solar system. -Directly observe the interstellar neutral atom focusing cone at 1 AU.

2001/02/08T E Moore - SW Interactions via LENA23 Comparison with Dayside Aurora See Fuselier et al., GRL 15 March Before/After images of dayside aurora. IMF Bz generally Northward. Similar in many ways to 24 Sept 98 CME, with resultant Ionospheric Mass Ejection [Moore et al., GRL, 1999] 8 June 2000 CME Arrival

2001/02/08T E Moore - SW Interactions via LENA24 Direct ISNs, Observed

2001/02/08T E Moore - SW Interactions via LENA25