Ambient Solar Wind Simulation of ambient solar wind driven by modified daily-updated WSA model:  Latitudinal distribution of the outflow velocity at 21.5.

Slides:



Advertisements
Similar presentations
SEP Data Analysis and Data Products for EMMREM Mihir I. Desai & Arik Posner Southwest Research Institute San Antonio, Texas Mihir I. Desai & Arik Posner.
Advertisements

Assume the axial symmetric CR density distribution with the minimum along with the axis of a cylinder Then the observed –G points toward the density minimum.
H.-S. Yu Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA 3D-MHD Models Driven by IPS
Reviewing the Summer School Solar Labs Nicholas Gross.
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.
Predictability of Japan / East Sea (JES) System to Uncertain Initial / Lateral Boundary Conditions and Surface Winds LCDR. Chin-Lung Fang LCDR. Chin-Lung.
Assessing the Contribution of Heliospheric Imaging in Improving Space Weather Prediction SHINE Session 6 Simon Plunkett and Doug Biesecker Thursday Morning.
Heliospheric MHD Models (for the LWS Community) LWS Workshop, Boulder, CO, March 23-26, 2004 Dusan Odstrcil 1,2 and Vic Pizzo 2 1 University of Colorado/CIRES,
Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004 Dusan Odstrcil University of Colorado/CIRES &
Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.
Tucson MURI SEP Workshop March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling.
Magnetic Reconnection in the Solar Wind Gosling, Phan, et al.
Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.
1 WSA Model and Forecasts Nick Arge Space Vehicles Directorate Air Force Research Laboratory.
C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.
CISM solar wind metrics M.J. Owens and the CISM Validation and Metrics Team Boston University, Boston MA Abstract. The Center for Space-Weather Modeling.
Hybrid simulations of parallel and oblique electromagnetic alpha/proton instabilities in the solar wind Q. M. Lu School of Earth and Space Science, Univ.
Forbes CME Hones TPE Distance in Rs Acceleration (m/s 2 ) CME Acceleration Solar Wind.
Solar system science using X-Rays Magnetosheath dynamics Shock – shock interactions Auroral X-ray emissions Solar X-rays Comets Other planets Not discussed.
When will disruptive CMEs impact Earth? Coronagraph observations alone aren’t enough to make the forecast for the most geoeffective halo CMEs. In 2002,
Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results S. A. Ledvina 1, D. Odstrcil 2 and J. G. Luhmann 1 1.Space Sciences.
ENLIL 3D-MHD Modeling Support of Heliospheric Missions European Space Weather Week, Liege, Belgium, November 2014 Dusan Odstrcil (GMU & NASA/GSFC)
1/18 Buoyant Acceleration: from Coronal Mass Ejections to Plasmoid P. Wu, N.A. Schwadron, G. Siscoe, P. Riley, C. Goodrich Acknowledgement: W.J.Hughes,
C. May 12, 1997 Interplanetary Event. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia,
Coronal and Heliospheric Modeling of the May 12, 1997 MURI Event MURI Project Review, NASA/GSFC, MD, August 5-6, 2003 Dusan Odstrcil University of Colorado/CIRES.
The “cone model” was originally developed by Zhao et al. ~10 (?) years ago in order to interpret the times of arrival of ICME ejecta following SOHO LASCO.
Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,
Predictions of Solar Wind Speed and IMF Polarity Using Near-Real-Time Solar Magnetic Field Updates C. “Nick” Arge University of Colorado/CIRES & NOAA/SEC.
RT Modelling of CMEs Using WSA- ENLIL Cone Model
Numerical simulations are used to explore the interaction between solar coronal mass ejections (CMEs) and the structured, ambient global solar wind flow.
Evolution of the 2012 July 12 CME from the Sun to the Earth: Data- Constrained Three-Dimensional MHD Simulations F. Shen 1, C. Shen 2, J. Zhang 3, P. Hess.
R. Oran csem.engin.umich.edu SHINE 09 May 2005 Campaign Event: Introducing Turbulence Rona Oran Igor V. Sokolov Richard Frazin Ward Manchester Tamas I.
Comparison of the 3D MHD Solar Wind Model Results with ACE Data 2007 SHINE Student Day Whistler, B. C., Canada C. O. Lee*, J. G. Luhmann, D. Odstrcil,
Arrival time of halo coronal mass ejections In the vicinity of the Earth G. Michalek, N. Gopalswamy, A. Lara, and P.K. Manoharan A&A 423, (2004)
AFRL/CISM Collaborations
29 August, 2011 Beijing, China Space science missions related to ILWS in China
Space weather forecasters perspective: UK David Jackson and Mark Gibbs SEREN Bz workshop, Abingdon, 9-10 July 2014.
Ionospheric Electrodynamics & Low-Earth Orbiting Satellites (LEOS) J-M Noël, A. Russell, D. Burrell & S. Thorsteinson Royal Military College of Canada.
Validation of the SWMF Coupled Model for Solar Corona – Inner Heliosphere – CME With the Observations of the May 12, 1997 Event Ofer Cohen(1), Igor V.
Lessons for STEREO - learned from Helios Presented at the STEREO/Solar B Workshop, Rainer Schwenn, MPS Lindau The Helios.
Acoustic wave propagation in the solar subphotosphere S. Shelyag, R. Erdélyi, M.J. Thompson Solar Physics and upper Atmosphere Research Group, Department.
Synoptic Network Workshop (HAO/NCAR, April 2013) Space Weather and Synoptic Observations V J Pizzo – NOAA/SWPC.
Modeling of CME-driven Shock propagation with ENLIL simulations using flux-rope and cone-model inputs Using observations from STEREO/SECCHI and SOHO/LASCO,
CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008.
Modeling 3-D Solar Wind Structure Lecture 13. Why is a Heliospheric Model Needed? Space weather forecasts require us to know the solar wind that is interacting.
Heliospheric Simulations of the SHINE Campaign Events SHINE Workshop, Big Sky, MT, June 27 – July 2, 2004 Dusan Odstrcil 1,2 1 University of Colorado/CIRES,
ENLIL Modeling for the interaction event: Effect of Interacting CMEs on SEP Intensity NASA/GSFC H. Xie, N. Gopalswamy, P. Makela, S. Yashiro.
Shocks in the IPS Wageesh Mishra Eun-kyung Joo Shih-pin Chen.
Multi-Point Observations of The Solar Corona for Space weather Acknowledgements The forecasting data was retrieved from NOAA SWPC products and SIDC PRESTO.
State of NOAA-SEC/CIRES STEREO Heliospheric Models STEREO SWG Meeting, NOAA/SEC, Boulder, CO, March 22, 2004 Dusan Odstrcil University of Colorado/CIRES.
1 Test Particle Simulations of Solar Energetic Particle Propagation for Space Weather Mike Marsh, S. Dalla, J. Kelly & T. Laitinen University of Central.
1 Pruning of Ensemble CME modeling using Interplanetary Scintillation and Heliospheric Imager Observations A. Taktakishvili, M. L. Mays, L. Rastaetter,
Date of download: 6/26/2016 Copyright © ASME. All rights reserved. From: Partial Differential Equation-Based Process Control for Ultraviolet Curing of.
Aerospace Structures Laboratory Seoul National University School of Mechanical and Aerospace Engineering A erospace S tructures aboratory L Mechanics of.
Driving 3D-MHD codes Using the UCSD Tomography
ESA SSA Measurement Requirements for SWE Forecasts
THE SUN The star we see by day.
Y. C.-M. Liu, M. Opher, O. Cohen P.C.Liewer and T.I.Gombosi
Xuepu Zhao Oct. 19, 2011 The Base of the Heliosphere: The Outer (Inner) Boundary Conditions of Coronal (Heliospheric) models.
D. Odstrcil1,2, V.J. Pizzo2, C.N. Arge3, B.V.Jackson4, P.P. Hick4
Tips Need to Consider When Organizing a College Event
Forecasting the arrival time of the CME’s shock at the Earth
Abstract We simulate the twisting of an initially potential coronal flux tube by photospheric vortex motions. The flux tube starts to evolve slowly(quasi-statically)
Forbush Decreases and Interplanetary Coronal Mass Ejections at Earth and Mars Mark Lester1, Beatriz Sanchez-Cano1, Emma Thomas1, Adam Langeveld1, Jingnan.
Understanding the Structure and Morphology of Coronal Mass Ejections by Integrating Observations and Modeling Scene Setting Talks: Miho Janvier (IAS) &
ماجستير إدارة المعارض من بريطانيا
SIDC Space Weather briefing
788.11J Presentation “Atmospheric Observatory”
Taiyou Zasshikai on May 17, 2004
Modified at -
Presentation transcript:

Ambient Solar Wind Simulation of ambient solar wind driven by modified daily-updated WSA model:  Latitudinal distribution of the outflow velocity at 21.5 Rs (top panel)  Predicted evolution at Earth (solid line) together with actually observed values(dots) by Wind spacecraft (bottom panel)

Solar Wind at Source Boundary

Solar Wind at Earth

Solar Wind at Earth – Effect of Grid Resolution Low resolutionMedium resolution

2005 May 13 CME Event LASCO/C2LASCO/C3Projected Velocity

Solar Wind Predictions – Effect of ICMEs