Transformation of MHD waves in sunspots and simulation of HMI level1 data Konstantin Parchevsky, Sebastien Couvidat, Richard Wachter, Alexander Kosovichev.

Slides:

Advertisements

Similar presentations

Magnetic Fields & Magnetic Field Strength We have seen that magnets can exert a force on objects without touching them. For this reason we speak of a.

Advertisements

SDO/HMI multi-height velocity measurements Kaori Nagashima (MPS) Collaborators: L. Gizon, A. Birch, B. Löptien, S. Danilovic, R. Cameron (MPS), S. Couvidat.

Numerical Simulations of Supergranulation and Solar Oscillations Åke Nordlund Niels Bohr Institute, Univ. of Copenhagen with Bob Stein (MSU) David Benson,

HMI OBSERVATIONS OF TRANSIENT PHENOMENA Juan Carlos Martínez Oliveros Space Sciences Laboratory, UC Berkeley Charles Lindsey, Hugh Hudson, S. Couvidat,

1/22/2001Physics 222 Special Relativity Lecture 3.

Molecular Tracers of Turbulent Shocks in Molecular Clouds Andy Pon, Doug Johnstone, Michael J. Kaufman ApJ, submitted May 2011.

Emerging Flux Simulations Bob Stein A.Lagerfjard Å. Nordlund D. Benson D. Georgobiani 1.

Modeling Generation and Nonlinear Evolution of Plasma Turbulence for Radiation Belt Remediation Center for Space Science & Engineering Research Virginia.

Initial Analysis of the Large-Scale Stein-Nordlund Simulations Dali Georgobiani Formerly at: Center for Turbulence Research Stanford University/ NASA Presenting.

ACAT-2002 The Evolutionary Model of Physics Large-Scale Simulation on Parallel Dataflow Architecture Dr. Andrey V. Nikitin Dr. Ludmila I. Nikitina Lomonosov.

Solar Convection Simulations Bob Stein David Benson.

TIME-DISTANCE ANALYSIS OF REALISTIC SIMULATIONS OF SOLAR CONVECTION Dali Georgobiani, Junwei Zhao 1, David Benson 2, Robert Stein 2, Alexander Kosovichev.

HMI & Photospheric Flows 1.Review of methods to determine surface plasma flow; 2.Comparisons between methods; 3.Data requirements; 4.Necessary computational.

What Simulations Could Provide for Ring Analysis Estimates of the p-mode line shape in the presence of: magnetism turbulent convection Verification of.

1 Chromospheric UV oscillations depend on altitude and local magnetic field Noah S. Heller and E.J. Zita, The Evergreen State College, Olympia, WA

Hybrid Simulation of Ion-Cyclotron Turbulence Induced by Artificial Plasma Cloud in the Magnetosphere W. Scales, J. Wang, C. Chang Center for Space Science.

Data for Helioseismology Testing: Large-Scale Stein-Nordlund Simulations Dali Georgobiani Michigan State University Presenting the results of Bob Stein.

Summary. Two directions in modeling Adopting physical (realistic) models Creating artificial data sets with simplified physics.

From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University.

Generation of Artificial Data in Support of SDO-HMI Nagi N. Mansour, NASA ARC Alan Wray, NASA ARC Thomas Hartlep, Stanford CTR Alexander Kosovichev, Stanford.

1 Fringe fields for stage V Iouri Ivaniouchenkov, Jim Rochford RAL MICE Video Conference, 9 April 2003.

Tsing Hua University, Taiwan Measurements of Acoustic Waves Scattered by Sunspots (Stanford, April 2011, LoHCo Workshop) Dean-Yi Chou Hui Zhao Ming-Hsu.

Flows in Active Regions Inferred from the Time-distance and the DAVE4VM.

Why does the temperature of the Sun’s atmosphere increase with height? Evidence strongly suggests that magnetic waves carry energy into the chromosphere.

Numerical simulation of effects of reduced excitationof 5-min.solar oscillations in sunspots Konstantin Parchevsky, Alexander Kosovichev Stanford University,

ob/data.html 1. Emerging Flux Simulations & proto Active Regions Bob Stein – Michigan State U. A.Lagerfjärd – Copenhagen U.

Near-surface simulations of the acoustic field Konstantin Parchevsky Stanford University, HEPL.

Detection of Emerging Sunspot Regions in the Solar Interior Stathis Ilonidis, Junwei Zhao, and Alexander Kosovichev Stanford University LoHCo Workshop.

MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.

Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn Big Bear solar Observatory of NJIT, CA 2 – CSPAR, Univ. of Alabama in Nuntsville,

Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Amanda Persichetti Aad.

Inversions from one of Konstantin’s Simulations Birch, Braun, & Crouch Data from Parchevsky & Kosovichev.

Sensitivity Kernels for Local Helioseismology Aaron Birch NWRA, CoRA Division.

ASCI/Alliances Center for Astrophysical Thermonuclear Flashes FLASH MHD Timur Linde FLASH MHD Timur Linde This work was supported by the ASCI Flash Center.

V.I. Vasiliev, Yu.A. Kostsov, K.M. Lobanov, L.P. Makarova, A.B. Mineev, D.V.Efremov Scientific Research Institute of Electrophysical Apparatus, St.-Petersburg,

Multi-level observations of magneto- acoustic cut-off frequency Ding Yuan Department of Physics University of Warwick Coventry CV4 7AL, UK

Decay of a simulated bipolar field in the solar surface layers Alexander Vögler Robert H. Cameron Christoph U. Keller Manfred Schüssler Max-Planck-Institute.

Using Realistic MHD Simulations for Modeling and Interpretation of Quiet Sun Observations with HMI/SDO I. Kitiashvili 1,2, S. Couvidat 2 1 NASA Ames Research.

Comparison of time- distance and holography Junwei Zhao and Alexander G. Kosovichev W. W. Hansen Experimental Physics Laboratory, Stanford University,

Holography far-side images with HMI Irene Gonzalez Hernandez Charlie Lindsey Richard Bogart Phil Scherrer Sebastian Couvidat, and the calibration team.

Area of Plane Shapes Area of Compound Shapes 8 m 2 m 5 m 2 m Not to scale 4 m 3 m ? ? 16 m 2 20 m 2 6 m 2 Area = = 42 m 2.

Photospheric MHD simulation of solar pores Robert Cameron Alexander Vögler Vasily Zakharov Manfred Schüssler Max-Planck-Institut für Sonnensystemforschung.

Tests of the Ring-Diagram Inversions A. Kosovichev.

Emerging Flux Simulations & semi-Sunspots Bob Stein A.Lagerfjärd Å. Nordlund D. Georgobiani 1.

The Current Status of Sunspot Seismology H. Moradi, H. Schunker, L. Gizon (Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany)

Chapter 26 Electromagnetism. Mass of Electron Determined by J.J. Thomson Determined by the deflection of the electron in a cathode ray tube.

The Helioseismic and Magnetic Imager (HMI) on NASA’s Solar Dynamics Observatory (SDO) has continuously measured the vector magnetic field, intensity, and.

Spectral Line Performance Using Inversion Codes J. Graham, A. Norton, S. Tomczyk, A. Lopez Ariste, H. Socas-Navarro, B. Lites NCAR/HAO Goal: Characterize.

Simulations of Solar Convection Zone Nagi N. Mansour.

Horizontal Flows in the Photosphere and the Subphotosphere in Two Active Regions Yang Liu, Junwei Zhao, Peter W. Schuck.

Helioseismology for HMI Science objectives and tasks* Data analysis plan* Helioseismology working groups and meetings *HMI Concept Study Report, Appendix.

Radiative Transfer in 3D Numerical Simulations Robert Stein Department of Physics and Astronomy Michigan State University Åke Nordlund Niels Bohr Institute.

Stability of magnetic fields in stars Vienna 11 th September 2007 Jonathan Braithwaite CITA, Toronto.

10 mm is the same as... 1 cm. 20 mm is the same as... 2 cm.

Simulations and radiative diagnostics of turbulence and wave phenomena in the magnetised solar photosphere S. Shelyag Astrophysics Research Centre Queen’s.

Diagnosing kappa distribution in the solar corona with the polarized microwave gyroresonance radiation Alexey A. Kuznetsov1, Gregory D. Fleishman2 1Institute.

WG1 – Sub-surface magnetic connections

Hyperspectral Wind Retrievals Dave Santek Chris Velden CIMSS Madison, Wisconsin 5th Workshop on Hyperspectral Science 8 June 2005.

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)

How The Faraday Motor Works

Coronal Loop Oscillations observed by TRACE

Observations of emerging and submerging regions with ASP and Solar-B

ConcepTest 19.1a Magnetic Force I

Forward Modeling for Time-Distance Helioseismology

Soothing Massage of HMI Magnetic Field Data

Atmosphere and the Electromagnetic spectrum

Area of a triangle Sunday, 16 June 2019.

Area of a triangle Sunday, 21 July 2019.

travel-time maps of sunspots: surface effects and artifacts?

106.13: A Makeover for HMI Magnetic Field Data

Presentation transcript:

Transformation of MHD waves in sunspots and simulation of HMI level1 data Konstantin Parchevsky, Sebastien Couvidat, Richard Wachter, Alexander Kosovichev Stanford University LoHCo Workshop, Stanford University, February 08-09, 2011

TD for Lsource = 6 Mm

TD for Lsource = 12 Mm

Simulated I+V, I-V profiles A B C

Magnetic field lg  = -2.2 HMI algorithm

Magnetic field strength vs. line shape pixel A B C line C B A

Reconstructed wavefield lg  = -2.2 H = 50 km from the line

Conclusion  MHD wave transformation can be seen in velocity components parallel and perpendicular to the magnetic field lines. Transformation exists even in case when the source is initially located completely outside of the magnetic region.  We simulated artificial HMI level 1 data from a given numerically simulated velocity field using 1D LTE radiative transfer SPINOR code.  Magnetic and velocity fields, reconstructed from these artificial data, show good agreement with the model data taken from the height of about 280 km above  =1 level.