Munetoshi Tokumaru (ISEE, Nagoya University)

Slides:



Advertisements
Similar presentations
K. Fujiki, H. Ito, M. Tokumaru Solar-Terrestrial Environment Laboratory (STELab), Nagoya University. SOLAR WIND FORECAST BY USING INTERPLANETARY SCINTILLATION.
Advertisements

The Johns Hopkins University Applied Physics Laboratory SHINE 2005, July 11-15, 2005 Transient Shocks and Associated Energetic Particle Events Observed.
Olga Khabarova & Vladimir obridko Heliophysical Laboratory, Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS (IZMIRAN), Moscow,
Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.
Using a DPS as a Coherent Scatter HF Radar Lindsay Magnus Lee-Anne McKinnell Hermanus Magnetic Observatory Hermanus, South Africa.
THE AUSTRALIAN NATIONAL UNIVERSITY Infrasound Technology Workshop, November 2007, Tokyo, Japan OPTIMUM ARRAY DESIGN FOR THE DETECTION OF DISTANT.
Valentina Abramenko Big Bear Solar Observatory of NJIT Multi-fractality of Solar Magnetic Fields: New Progress with HMI Abstract. The SDO/HMI instrument.
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.
SSL UC Berkeley 2010 June ACE/SOHO/STEREO/Wind Workshop Interplanetary Propagation of Solar Impulsive Energetic Electrons Linghua Wang, Bob Lin and S ä.
Abstract For a while it seemed like a simple fluid-like, self-similar, Kolmogoroff cascade was the easy explanation for the nature and evolution of the.
EISCAT Tromsø. Progress in Interplanetary Scintillation Bill Coles, University of California at San Diego A. The Solar Wind: B. Radio Scattering: C. Observations:
What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory,
SHINE 2008 June, 2008 Utah, USA Visit our Websites:
1 C. “Nick” Arge Space Vehicles Directorate/Air Force Research Laboratory SHINE Workshop Aug. 2, 2007 Comparing the Observed and Modeled Global Heliospheric.
Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)
Intermittency beyond the ecliptic plane Anna Wawrzaszek, Marius Echim, Wiesław M. Macek, Roberto Bruno Mamaia, 6-13 September 2015 (1) Space Research Centre.
2011-Aug-11/AOGS 2011 Global Observations of the Solar Wind with STEL IPS Array M. Tokumaru, K. Fujiki, T. Iju, M. Hirota, M. Noda, and M. Kojima (STEL,
Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Mejía-Ambriz.
1 / 10 Comparison between Microwave and Hard X-ray Spectral Indices of Temporally and Spatially Resolved Non-Thermal Sources Kiyohara, J., Takasaki, H.,
Interplanetary Scintillation Observations of the Solar Wind Using SWIFT and Upgraded STEL Multi-station System M. Tokumaru, K. Fujiki, and T. Iju (STEL,
Signatures of Intermittent Turbulence in Hinode Quiet Sun Photosphere Valentina Abramenko, Big Bear Solar Observatory, USA, Plasma.
Observations of Intra-Hour Variable Quasars Hayley Bignall (JIVE) Dave Jauncey, Jim Lovell, Tasso Tzioumis (ATNF) Jean-Pierre Macquart (NRAO/Caltech) Lucyna.
Upgrade of STEL Multi-Station Interplanetary Scintillation System and Recent Observations of the Solar Wind Munetoshi Tokumaru, Masayoshi Kojima, Ken ’
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)
CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego,
The investigations of the solar wind with the large decametric radio telescopes of Ukraine Falkovych I.S. 1, Konovalenko A.A 1, Kalinichenko N.N. 1, Olyak.
TO THE POSSIBILITY OF STUDY OF THE EXTERNAL SOLAR WIND THIN STRUCTURE IN DECAMETER RADIO WAVES Marina Olyak Institute of Radio Astronomy, 4 Chervonopraporna,
Solar System Physics Group IPS Using EISCAT and MERLIN: Extremely-Long Baseline Observations at Multiple Frequencies R.A.Fallows, A.R.Breen, M.M.Bisi,
Intrinsic Short Term Variability in W3-OH and W49N Hydroxyl Masers W.M. Goss National Radio Astronomy Observatory Socorro, New Mexico, USA A.A. Deshpande,
Steven R. Spangler, Department of Physics and Astronomy
Scintillation in Extragalactic Radio Sources Marco Bondi Istituto di Radioastronomia CNR Bologna, Italy.
InterPlanetary Scintillation IPS induced Pluripotent Stem cell iPS.
Composition and spectral properties of the 1 AU quiet- time suprathermal ion population during solar cycle23 M Al-Dayeh, M I Desai, J R Dwyer, H K Rassoul,
Valentina Abramenko 1, Vasyl Yurchyshyn 1, Philip R. Goode 1, Vincenzo Carbone 2, Robert Stein Big Bear Solar Observatory of NJIT, USA; 2 – Univ.
Evidence for Anisotropy and Intermittency in the Turbulent Interstellar Plasma Bill Coles, University of California, San Diego 1. It had been thought that.
OH maser sources in W49N: probing differential anisotropic scattering with Zeeman pairs desh Raman Research Institute, Bangalore + Miller Goss, Eduardo.
Intermittency Analysis and Spatial Dependence of Magnetic Field Disturbances in the Fast Solar Wind Sunny W. Y. Tam 1 and Ya-Hui Yang 2 1 Institute of.
-1- Solar wind turbulence from radio occultation data Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering.
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.
ORIGIN OF THE SLOW SOLAR WIND K. Fujiki , T. Ohmi, M. Kojima, M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University and K. Hakamada Department.
The Suprathermal Tail Properties are not well understood; known contributors Heated solar wind Interstellar and inner source pickup ions Prior solar and.
Inherent Length Scales and Apparent Frequencies of Periodic Solar Wind Number Density Structures Nicholeen Viall 1, Larry Kepko 2 and Harlan Spence 1 1.
Probing Turbulence At and Near CME-driven shocks Using Energetic Particle Spectra Living with a Star Team meeting Sep 18th, 2008 Pasadena, CA Gang Li From.
Turbulence in the Solar Wind
CASS/UCSD Dusan_CCMC_2013 Heliospheric Solar Wind Forecasting Using IPS Slides For A Possible CCMC Presentation 2013 Introduction:
1 Pruning of Ensemble CME modeling using Interplanetary Scintillation and Heliospheric Imager Observations A. Taktakishvili, M. L. Mays, L. Rastaetter,
Diffraction scintillation at 1.4 and 4.85GHz V.M.Malofeev, O.I.Malov, S.A.Tyul’bashev PRAO, Russia W.Sieber Hochschule Nederrhein, Germany A.Jessner, R.Wielebinski.
IPS tomography IPS-MHD tomography. Since Hewish et al. reported the discovery of the interplanetary scintillation (IPS) phenomena in 1964, the IPS method.
IPS Observations Using the Big Scanning Array of the Lebedev Physical Institute: Recent Results and Future Prospects I.V.Chashei, V.I.Shishov, S.A.Tyul’bashev,
CME rate: 1/3 (4) day -1 at solar min (max) [LASCO CME catalogue. Yahsiro et al., 2005] |B| at 1 AU: 5 (8) nT at solar min (max) [OMNI data] D (fraction.
Generation of anisotropic turbulence in drifting proton-alpha plasmas Yana Maneva, S. Poedts CmPA, KU Leuven In collaboration with: A. Viñas and L. Ofman.
B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington,
B.V. Jackson, H.-S. Yu, P.P. Hick, and A. Buffington,
Driving 3D-MHD codes Using the UCSD Tomography
Institute for Space-Earth Environmental Research (ISEE),
Interplanetary scintillation of strong sources during the descending phase near the minimum of 23 solar activity cycle Chashei I1., Glubokova1,2 S., Glyantsev1,2.
ICME in the Solar Wind from STEL IPS Observations
George C. Ho1, David Lario1, Robert B. Decker1, Mihir I. Desai2,
IPS g-value Measurements
Diagnosing kappa distribution in the solar corona with the polarized microwave gyroresonance radiation Alexey A. Kuznetsov1, Gregory D. Fleishman2 1Institute.
WITH LOW FREQUENCY UKRAINIAN RADIO TELESCOPES UTR-2, URAN and GURT
Exploration of Solar Magnetic Fields from Propagating GONG Magnetograms Using the CSSS Model and UCSD Time-Dependent Tomography H.-S. Yu1, B. V. Jackson1,
Coupled ion acceleration and
Third-Moment Descriptions of the Interplanetary Turbulent Cascade, Intermittency, and Back Transfer Bernard J. Vasquez1, Jesse T. Coburn1,2, Miriam A.
D. Odstrcil1,2, V.J. Pizzo2, C.N. Arge3, B.V.Jackson4, P.P. Hick4
Effects of Dipole Tilt Angle on Geomagnetic Activities
Steven R. Spangler University of Iowa
Investigation of Heliospheric Faraday Rotation Due to a Coronal Mass Ejection (CME) Using the LOw Frequency ARray (LOFAR) and Space-Based Imaging Techniques.
ESS 261 Topics in magnetospheric physics Space weather forecast models ____ the prediction of solar wind speed April 23, 2008.
What is the scattering screen in front of quasar PKS B ?
Presentation transcript:

Munetoshi Tokumaru (ISEE, Nagoya University) Analysis of Solar Wind Density Turbulence using Interplanetary Scintillation Measurements Preliminary Results Munetoshi Tokumaru (ISEE, Nagoya University)

Introduction Spatial spectrum of the solar wind density turbulence is reflected in the high frequency portion of temporal spectrum of interplanetary scintillation (IPS). Flattening by Fresnel filter occurs at the low frequency portion of IPS. Solar wind density fluctuations Frequency Fresnel filter Power

This Study Determine solar wind turbulence parameters by fitting a model to IPS spectra observed at Toyokawa. Observations 2 strong IPS sources: 3C273, 3C48 Period: 2012, 2013(solar maximum) Solar elongation: 0.2 AU < R <1 AU(weak scattering regime for 327 MHz) Model Spatial spectrum of solar wind turbulence:defined by power-law index (α), axial ratio (AR) of anisotropy, level (CN) Use of solar wind speeds V derived from 3-station measurements as a fixed parameter. Usually, V is one of free parameters in the fitting analysis. Investigate the relation between α, AR, and speeds.

Model Weak scattering & thin screen at the point P Free parameters: CN, α, AR Fixed parameter: Solar Wind Speed: V (kF=2πfF/V) Source size θ (kc=1/Zθ) 3C273: 60 mas, 3C48 : 100 mas point-P-Earth distance: Z, wavelength: λ Fresnel frequency Fresnel Filter Finite Source Size Effect

Spectral Fitting Analysis White noise component V=459 km/s, AR=1.07, α= 3.8 Least Squares Fitting: Marquardt Method Fitting in Log-Log Space Weighting Function: 1/N

Correlation between V1 and V3 V1: 4 Free para (Cn, fF(V), AR, α) CC =0.441991 Open: 3C273 Solid: 3C48 N=105, p = 0% V1(km/s)=228.332+/-33.7360 + 0.417804+/-0.835485E-01*V3 (km/s) (Err= 77.4437 km/s) V3(km/s)=209.883+/-37.5834 + 0.467585+/-0.935027E-01*V1(km/s) (Err= 81.9271 km/s)

Histograms of AR and α determined from spectral fitting analysis (Fixed V) In the fitting analysis, V is given from three-station measurements V3. Free parameters are Cn, AR, α. N=105 AR =0.960522 +/- 0.402797 α = 4.08890 +/- 0.562480 Kolmogorov (11/3)

Relation between α and speed V (Fixed V) Open: 3C273 Solid: 3C48 CC = 0.180053 N= 105, p=6.6 % α= 3.64829+/-0.243350 + 0.111965E-02+/-0.602664E-03*V (Err= 0.558628) V = 275.118+/-64.3348 + 28.9584+/-15.5872*α (Err= 89.8399) No correlation or weak positive dependence on V (its significance is poor).

IPS Observations at Ooty and STEL (Manoharan et al., 1994) Power-law index α ← Spectral fitting analysis using Ooty IPS obs. Speed V ← STEL IPS obs. sol. min. sol. max. Three-component model of solar wind density turbulence low freq.:Kolmogorov, intermediate freq:flattening, high freq.:inner scale cutoff The dependence of α on V is ascribed to the selection effect of the frequency range in the spectrum.

Relation between AR and Speed V (Fixed V) Open: 3C273 Solid: 3C48 CC = 0.194379 N= 105, p= 5% AR = 0.619912+/-0.173783 + 0.865533E-03+/-0.430379E-03*V (Err= 0.398932) V = 351.597+/-22.6082 + 43.6532+/-21.7061*AR (Err= 89.5906) Weak positive dependence on V, but Its significance is rather poor.

Radial Variation of AR (left) and α (right)

Radial Dependence of AR (left) and α (right) Microwave IPS measurements in 1994 (Yamauchi et al., 1998) Solid circles: Slow wind, Open triangles: Fast wind Fast wind is associated with larger α for R> 40 Rs (0.2 AU) No difference in AR between fast and slow winds

Relation between AR and α (Fixed V) CC= -0.647138 N=105, p = 0% α = 4.95689+/-0.109257 - 0.903671+/-0.104897*AR (Err= 0.432958) AR = 2.85538+/-0.222027 - 0.463417+/-0.537934E-01*α (Err= 0.310048) Open: 3C273 Solid: 3C48 Significant negative correlation between α and AR This might suggests that AR is strongly coupled with α in the model.

Spectral Fitting Analysis of Kashima IPS Observations at 2,8, and 22 GHz in 1991 Speed Spectral indices α become smaller, and axial ratios AR increase in the near-Sun region, where the solar wind speeds decrease. What is the physical meaning? Axial ratio Spectral index Tokumaru et al., 1992

Comparison between c/a and AR (Fixed V) x’ (radial) y’ The parameter c/a, which represents anisotropy of turbulence, is determined from three-station IPS measurements. Weak positive correlation between AR derived from spectral fit analysis and c/a derived from 3-station measurements? But, its significance is very poor. isotropic: c/a=0 anisotropic: c/a≠0 CC = 0.192489 N= 105, p = 5 % AR= 0.961683+/-0.389509E-01 + 0.294872+/-0.148119*(c/a) (Err= 0.399083) (c/a) = -0.124633+/-0.657414E-01 + 0.125654+/-0.631182E-01*AR (Err= 0.260517) Open: 3C273 Solid: 3C48

Summary We determine solar wind turbulence parameters; α and AR, by fitting a model to IPS spectra observed at Toyokawa Solar wind speeds derived from 3-station measurements are used for this analysis. solar maximum, data for 1AU>R>0.2AU AR ~ 1.0 (isotropic), α~4 (slightly steeper than Kolmogorov=11/3) α, AR: weak dependence on speed? (further study is needed) Negative correlation between AR and α Weak positive correlation between AR and c/a? (further study is needed).