-1- Coronal Faraday Rotation of Occulted Radio Signals M. K. Bird Argelander-Institut für Astronomie, Universität Bonn International Colloquium on Scattering.

Slides:

Advertisements

Similar presentations

Uncovering the Global Slow Solar Wind Liang Zhao and Thomas H. Zurbuchen Department of Atmospheric, Oceanic and Space Sciences, University of Michigan.

Advertisements

On the link between the solar energetic particles and eruptive coronal phenomena On the link between the solar energetic particles and eruptive coronal.

THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE CRISM- 2011, Montpellier, 27 June – 1 July, Collaborators:

Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.

Valbona Kunkel June 18, 2013 Hvar, Croatia NEW THEORITICAL WORK ON FLUX ROPE MODEL AND PROPERTIES OF MAGNETIC FIELD.

Plasmas in Space: From the Surface of the Sun to the Orbit of the Earth Steven R. Spangler, University of Iowa Division of Plasma Physics, American Physical.

Interaction of coronal mass ejections with large-scale structures N. Gopalswamy, S. Yashiro, H. Xie, S. Akiyama, and P. Mäkelä IHY – ISWI Regional meeting.

Measuring Dispersion in Signals from the Crab Pulsar Jared Crossley National Radio Astronomy Observatory Tim Hankins & Jean Eilek New Mexico Tech Jared.

Reviewing the Summer School Solar Labs Nicholas Gross.

M. J. Reiner, 1 st STEREO Workshop, March, 2002, Paris.

NoRH Visit February, 2005Angelos Vourlidas, NRL On Deriving Mass & Energetics of Coronal Mass Ejections Angelos Vourlidas NRL A Tutorial.

CME-driven Shocks in White Light Observations SOHO/LASCO C3 – CME May 5 th, 1999 CME-driven Shock We demonstrate that CME-driven shocks: (1) can be detected.

Solar wind in the outer heliosphere: IPS observations at the decameter wavelengths. N.N. Kalinichenko, I.S. Falkovich, A.A. Konovalenko, M.R. Olyak, I.N.

Galactic Magnetic Field Research with LOFAR Wolfgang Reich Max-Planck-Institut für Radioastronomie Bonn, Germany.

Solar Activity and VLF Prepared by Sheila Bijoor and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global AWESOME.

The Potential for Tracking Transient Events Through the Heliosphere to Geospace With Emerging Low-Frequency Radio Telescopes Justin C. Kasper *,1, Divya.

Measuring the Magnetic Field in the Sun and the Interstellar Medium Steven R. Spangler… University of Iowa.

RT Modelling of CMEs Using WSA- ENLIL Cone Model

EISCAT Tromsø. Progress in Interplanetary Scintillation Bill Coles, University of California at San Diego A. The Solar Wind: B. Radio Scattering: C. Observations:

Radioastronomical Remote Sensing of Turbulence and Current Sheets in the Solar Corona Steven R. Spangler Department of Physics and Astronomy University.

The Effect of Solar Wind on Pulsar Observations Xiaopeng YOU Southwest University, Chongqing, China.

What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory,

The Solar Corona Steven R. Spangler Department of Physics and Astronomy University of Iowa.

Shock wave formation heights using 2D density and Alfvén maps of the corona ABSTRACT Coronal shock waves can produce decametric radio emission known Type.

The Sun and the Heliosphere: some basic concepts…

1 Interpreting SECCHI White Light Images: FOV Sensitivity & Stereo Viewing Paulett Liewer, JPL; Russ Howard & Dennis Socker, NRL SECCHI Consortium Meeting.

Radio Remote Sensing of the Corona and the Solar Wind Steven R. Spangler University of Iowa.

Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)

OBSERVATION OF THE JANUARY 1997 CORONAL MASS EJECTION NEAR THE SUN USING RADIO SOUNDING TECHNIQUE WITH GALILEO SPACECRAFT A.I. Efimov, L.N. Samoznaev,

Remote Radio Sounding Science For JIMO J. L. Green, B. W. Reinisch, P. Song, S. F. Fung, R. F. Benson, W. W. L. Taylor, J. F. Cooper, L. Garcia, D. Gallagher,

1 Determination of CME 3D Trajectories using COR Stereoscopy + Analysis of HI1 CME Tracks P. C. Liewer, E. M. DeJong, J. R. Hall, JPL/Caltech; N. Sheeley,

ECE 5233 Satellite Communications Prepared by: Dr. Ivica Kostanic Lecture 15: Secondary atmospheric losses effects (Section ) Spring 2011.

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)

New STEREO/SECCHI Processing for Heliospheric Transients David F. Webb ISR, Boston College, MA, USA New England Space Science Consortium.

Solar Wind and Coronal Mass Ejections

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

Simultaneous VLA and UVCS/SOHO Observations of the Solar Corona Steven R. Spangler (University of Iowa), Mari Paz Miralles, Steven R. Cranmer, and John.

Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,

Solar and STP science with AstroGrid Silvia Dalla School of Physics & Astronomy, University of Manchester A PPARC funded project.

Lessons for STEREO - learned from Helios Presented at the STEREO/Solar B Workshop, Rainer Schwenn, MPS Lindau The Helios.

Forecast of Geomagnetic Storm based on CME and IP condition R.-S. Kim 1, K.-S. Cho 2, Y.-J. Moon 3, Yu Yi 1, K.-H. Kim 3 1 Chungnam National University.

Aristeidis Noutsos University of Manchester. The LOFAR Ionosphere See Ger’s talk, in Hamburg last year. Variations of ~3 rad m –2 were observed in the.

Potential of a Low Frequency Array (LOFAR) for Ionospheric and Solar Observations ABSTRACT: The Low Frequency Array (LOFAR) is a proposed large radio telescope.

Evidence for Anisotropy and Intermittency in the Turbulent Interstellar Plasma Bill Coles, University of California, San Diego 1. It had been thought that.

Fast Magnetosonic Waves and Global Coronal Seismology in the Extended Solar Corona Ryun Young Kwon, Jie Zhang, Maxim Kramar, Tongjiang Wang, Leon Ofman,

Strength and Structure of the Coronal Magnetic Field Steven R. Spangler University of Iowa.

Radio Sounding of the Near-Sun Plasma Using Polarized Pulsar Pulses I.V.Chashei, T.V.Smirnova, V.I.Shishov Pushchino Radio Astronomy Obsertvatory, Astrospace.

Measuring the Magnetic Field in the Solar Corona Steven R. Spangler… University of Iowa.

-1- Solar wind turbulence from radio occultation data Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering.

Transient response of the ionosphere to X-ray solar flares Jaroslav Chum (1), Jaroslav Urbář (1), Jann-Yenq Liu (2) (1) Institute of Atmospheric Physics,

Measuring the Near-Nothingness of Interstellar Space with Radio Astronomy Steven R. Spangler University of Iowa.

Some EOVSA Science Issues Gregory Fleishman 26 April 2011.

A Numerical Study of the Breakout Model for Coronal Mass Ejection Initiation P. MacNeice, S.K. Antiochos, A. Phillips, D.S. Spicer, C.R. DeVore, and K.

Stuart D. BaleFIELDS SOC CDR – Science Requirements Solar Probe Plus FIELDS SOC CDR Science and Instrument Overview Science Requirements Stuart D. Bale.

Probing Coronal Mass Ejections with Faraday Rotation Measurements Steven R. Spangler and Catherine A. Whiting University of Iowa.

Data-constrained Simulation of CME Initiation and Propagation Antonia Savcheva ESPM 2014 September 11, 2014 Collaborators: R. Evans, B. van der Holst,

Probing the Solar Corona with Radioastronomical Observations Steven R. Spangler.

Three-Dimensional Structure of Coronal Mass Ejections From LASCO Polarization Measurements K. P. Dere, D. Wang and R. Howard ApJL, 620; L119-L

The heliospheric magnetic flux density through several solar cycles Géza Erdős (1) and André Balogh (2) (1) MTA Wigner FK RMI, Budapest, Hungary (2) Imperial.

Waves in magnetized plasma

Monitoring of interplanetary and ionosphere scintillations at the frequency 111MHz S.A.Tyul’bashev, V.I.Shishov, I.V.Chashei, I.A.Subaev Pushchino Radio.

Faraday Rotation as a Diagnostic of Cosmic Magnetic Fields

An Introduction to Observing Coronal Mass Ejections

Driving 3D-MHD codes Using the UCSD Tomography

ICME in the Solar Wind from STEL IPS Observations

Jason E. Kooi1,2 and Steven R. Spangler2

Radio Remote Sensing of the Solar Corona

Investigation of Heliospheric Faraday Rotation Due to a Coronal Mass Ejection (CME) Using the LOw Frequency ARray (LOFAR) and Space-Based Imaging Techniques.

Radio Signatures of Coronal Magnetic Fields and Reconnections

Polarization Properties of an Eclipsing Pulsar

Presentation transcript:

-1- Coronal Faraday Rotation of Occulted Radio Signals M. K. Bird Argelander-Institut für Astronomie, Universität Bonn International Colloquium on Scattering and Scintillation in Radio Astronomy Pushchino, Russia Monday, 19 June 2006

-2- Outline  Coronal Faraday Rotation – Definition  Coronal FR using Various Radio Sources –Pulsars –Extended Continuum Sources –Spacecraft (Helios E12: )  FR Variations over Different Time Scales –Background Coronal Magnetic Field –FR Signature of Coronal Mass Ejections –FR Fluctuations: Alfvén Waves & Quasi-harmonic Oscillations  Coronal FR Mapping – the Future?  Summary

-3- Coronal Faraday Rotation - Definition

-4- Faraday Rotation  : Definition radians 2.36∙10 4 in MKS or cgs units radio frequency (Helios: 2.3 GHz) electron density mag field proj. along ray path with

-5- Interplanetary Electron Column Density from Earth “Dispersion Measure” Units: hexems 1 hexem = el/m 2 Earth Sun analogous plot for Faraday Rotation does not exist! I = ∫N e (s) ds

-6- Polarization Angle Measurement Electric Vectors (semi-major axis of polarization ellipse): E 0 = Source (transmitted) E = Measured (received) Angle definitions: q = locally measured polarization angle p = parallactic angle  = Faraday rotation

-7- Rotation Measure RM: A rotation measure of RM = 1 rad m -2 yields:  = 0.97° at 2.3 GHz ( =0.13 m)  = 57.3° at 300 MHz ( =1.0 m)  = 1432° at 60 MHz ( =5.0 m)

-8- Coronal Faraday Rotation Measurement 1.  can be positive or negative (from polarity of interplanetary magnetic field) 2.Angle ambiguity (    ± m·180°) 3.Contributions from electron density and magnetic field cannot be separated without independent measurements 4.Correction for variable ionosphere necessary if solar offset R > 10 R S

-9- Ionospheric Faraday Rotation

-10- Coronal FR using Various Radio Sources

-11- Coronal FR with Pulsars

-12- Pulsars at Conjunction [Bird et al., Nature 283, , 1980]

-13- Pulsar Pulse Profiles: Measurement Technique Pulsar Pulse Profiles: Measurement Technique PSR PSR intrinsic profile modified profile p-angle: intrinsic & modified

-14- Coronal FR of PSR ( )

-15- Solwind Images during 1979 Occultation of PSR

-16- Coronal Magnetic Field from RM & DM: 1979 Coronal Magnetic Field from RM & DM: 1979

-17- Coronal FR with Extended Continuum Sources 3C228 [Spangler, 2005] A B C 1'1'

-18- Coronal FR at VLA: 21 Aug 2003  RM: 62.5 rad/m 2 3C228 R = 7.1…6.2 R S

-19- SOHO/LASCO: 16 AUG C228 Jupiter Venus

-20- Coronal FR with Helios  Helios – 1 –Launch: 10 Dec 1974 –EOM: 15 Mar 1986 –q = 0.31 AU (P = 190 d) –i = 0°, "spin up"  Helios – 2 –Launch: 15 Jan 1976 –EOM: 08 Jan 1981 –q = 0.29 AU (P = 186 d) –i = 0°, "spin down"

-21- Earth-Sun Line Fixed: Helios-1

-22- Coronal Faraday Rotation: Helios Observations = 35.4°  FR = 2.1°

-23- Helios FR: Effelsberg/Goldstone

-24- Coronal FR: Helios-1, Dec  ambiguity

-25- FR Variations over Different Time Scales …Background Coronal Magnetic Field

-26- Ballerina Model of HCS

-27- Radio Ray Path Geometry in the Corona

-28- Coronal Faraday Rotation from Sector Structure

-29- Mean Absolute FR: |  max |  R -4.15

-30- Coronal Electron Density: Radial Profiles

-31- Mean Coronal Magnetic Field R S < R < 10 R S : B r = 7.9 R -2.7 G (17) or B r = 6 R R -2 G (18) [Pätzold et al., Solar Phys. 109, 91, 1987]

-32- FR Variations over Different Time Scales … FR Fluctuations: Alfvén Waves & Quasi-harmonic Oscillations

-33- FR Fluctuations: Standard Deviation vs. Solar Offset

-34- FR Spectra for Various Solar Offset Distances Andreev et al., [1996]

-35- FR Spectral Index vs Solar Offset

-36- Two-Station Coronal Sounding Measurements

-37- Measuring Coronal Velocities

-38- Coronal Velocities from FR Correlations

-39- Two-Station FR Measurements Two-Station FR Measurements

-40- Simultaneous FR Spectra with QHC

-41- Rapid Sequence of FR Spectra QHC comes… … and goes! [Chashei et al., 1999]

-42- FR Variations over Different Time Scales … FR Signature of Coronal Mass Ejections

-43- CME Passing through Helios-2 Ray Path Solwind Coronagraph Images recorded during Helios Solar Occultations In Oct/Nov 1979 [Bird et al., 1985]

-44- CME Height-Time Diagram, 24 Oct 1979

-45- CME Magnetic Field Estimates, 24 Oct 1979 UTSolar Offset (R S )  I (hexems)  (deg) (mG) 08: ±10±2 08: : : : : ±5±1 11:

-46- Coronal FR Mapping – the Future?

-47- One line of sight to a linearly polarized source

-48-

-49- Simulated Coronal FR for CR 1751 [J. Kasper, priv. comm, 2004.]

-50- Transient Simulations: October 2003 CMEs CME not yet detected Large FR in  20 sources CME!

-51- FR Mapping – Conclusions regarding LOFAR  Expected density of suitably polarized sources:  1 deg -2  FR maps could be used to test models of coronal magnetic topology  FR maps of transient flux ropes could be used to predict the geoeffectivity of the ensuing CME impact at Earth

-52- Coronal Faraday Rotation: Summary  Faraday Rotation measurements provide a unique tool for investigating coronal magnetic structure… –Emperical model for the magnitude and radial dependence of the background coronal magnetic field –Evidence for outward (and inward) propagating Alfvén waves –Evidence for dominance of magnetic fluctuations over density fluctuations  FR Mapping of CMEs is a difficult, but not hopeless, task.