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.

Slides:

Advertisements

Similar presentations

Pulsar radio wave dispersion, intermittency, and kinetic Alfvén wave turbulence Paul Terry Stas Boldyrev.

Advertisements

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.

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

Which describes a variation of wave frequency ω(t) in a geometric-optic approximation [4]. Here n(ω) is the refractive index of the medium, is the vector.

1 Signal Propagation (Seeber, 2.3).. 2 Ch. 3 Clock definition.

1 Signal Propagation (Seeber, 2.3).. 2 Ch. 3 Clock definition.

Hamburg, September Observation of Carbon Radio Recombination Lines Towards Dust Cloud L1407 at decameter wavelengths. S. V. Stepkin, A. A.

SWG-17Pasadena, CA B A Direction Finding and Triangulation from STEREO & Wind M. J. Reiner.

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

Interplanetary Scintillations and the Acceleration of the Solar Wind Steven R. Spangler …. University of Iowa.

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)

Incoherent Scattering

Theory of Solar Radar Experiments: Combination Scattering by Anisotropic Langmuir Turbulence November 8, Uppsala, Sweeden Licentiate seminar by Mykola.

Stuart D. BaleFIELDS iPDR – Science Requirements Solar Probe Plus FIELDS Instrument PDR Science and Instrument Overview Science Requirements Stuart D.

Solar System Physics Group Heliospheric physics with LOFAR Andy Breen, Richard Fallows Solar System Physics Group Aberystwyth University Mario Bisi Center.

Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Mejía-Ambriz.

Solar System Physics Group Heliospheric studies with LOFAR and EISCAT-3D Andy Breen, Mario Bisi & Richard Fallows Aberystwyth University.

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego,

Diagnostics of solar wind streams N.A.Lotova, K.V.Vladimirsky, and V.N.Obridko IZMIRAN.

(1) Institute of Radio Astronomy, Kharkov, Ukraine (2) Space Research Institute, Graz, Austria Decameter Type IV bursts: Properties of Fiber Bursts V.N.

Single Pulse Investigations at the Decameter Range O.M. Ulyanov 1, V.V. Zakharenko 1, V.S. Nikolaenko 1, A. Deshpande 2, M.V. Popov 3, V.A. Soglasnov 3,

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.

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

Voyager 2 Observations of Magnetic Waves due to Interstellar Pickup Ions Colin J. Joyce Charles W. Smith, Phillip A. Isenberg, Nathan A. Schwadron, Neil.

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,

Investigation of different types radio sources by IPS method at 111MHz S.A.Tyul’bashev Pushchino Radio Astronomy Observatory, Astro Space Center of P.N.Lebedev.

M.Nechaeva, Radiophysical Research Institute, Nizhni Novgorod, Russia Radio interferometer signal at raying of the solar wind plasma.

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.

SUBDIFFUSION OF BEAMS THROUGH INTERPLANETARY AND INTERSTELLAR MEDIA Aleksander Stanislavsky Institute of Radio Astronomy, 4 Chervonopraporna St., Kharkov.

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

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.

Coronal scattering under strong regular refraction Alexander Afanasiev Institute of Solar-Terrestrial Physics Irkutsk, Russia.

Interstellar turbulent plasma spectrum from multi-frequency pulsar observations Smirnova T. V. Pushchino Radio Astronomy Observatory Astro Space Center.

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.

-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.

The Suprathermal Tail Properties are not well understood; known contributors Heated solar wind Interstellar and inner source pickup ions Prior solar and.

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

Simulations of turbulent plasma heating by powerful electron beams Timofeev I.V., Terekhov A.V.

Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

Reflection distance,, and the change in the electron number density,, at the reflecting plasma boundary: We searched for but found no echo in simultaneously.

Sixth European Space Weather Week Conference Site Oud Sint-Jan, Bruges, Belgium November 2009 Space-time Localization of Inner Heliospheric Plasma.

Observations of reflected ions downstream of shocks in the heliosphere John Richardson M.I.T. (Voyager plasma experiment) 10 – 5950 eV/q.

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.

How can we measure turbulent microscales in the Interstellar Medium? Steven R. Spangler, University of Iowa.

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,

Solar System Physics Group Heliospheric physics with LOFAR Andy Breen, Richard Fallows Solar System Physics Group Aberystwyth University Mario Bisi Center.

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.

Interstellar Turbulence and the Plasma Environment of the Heliosphere

Solar and heliosheric WG

The Worldwide Interplanetary Scintillation (IPS) Stations (WIPSS) Network Mario M. Bisi [1], J. Americo Gonzalez-Esparza[2][3][4],

Interplanetary scintillation of strong sources during the descending phase near the minimum of 23 solar activity cycle Chashei I1., Glubokova1,2 S., Glyantsev1,2.

CHARACTERISTICS OF TURBULENT PROCESS IN THE SOLAR PHOTOSPHERE

ICME in the Solar Wind from STEL IPS Observations

IPS g-value Measurements

WITH LOW FREQUENCY UKRAINIAN RADIO TELESCOPES UTR-2, URAN and GURT

Radio Remote Sensing of the Solar Corona

Munetoshi Tokumaru （ISEE, Nagoya University）

Steven R. Spangler University of Iowa

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.

In situ particle detection

Presentation transcript:

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. Bubnov Institute of Radio Astronomy, Kharkiv, Ukraine

The solar wind blows a giant bubble with size of about 100 AU called the heliosphere.

The interplanetary scintillations (IPS) technique

Decameter range allows us to observe the interplanetary scintillations at large elongations OR to probe rarefied plasma in the outer heliosphere weakly scattering the high frequencies.

Our investigations of the solar wind in the outer heliosphere briefly consist of: Theoretical investigations and modelling. Theoretical investigations and modelling. Observations. Observations. Fitting the theoretical model to the observed IPS characteristics Fitting the theoretical model to the observed IPS characteristics

Models of the solar wind One flow model with parameters:,, is the distance from the sun Slow-speed stream with parameters and one or two high-speed stream (s) with parameters, = 1АЕ where, is the stream thickness Multi-flow model including:

Spectrum analysis. Spectrum analysis. Dispersion analysis. Dispersion analysis. Methods Scattering of decameter radio waves by the rarefied plasma of the outer heliosphere is well described by methods based on the multiple scattering theory such as Feynman’s path-integral technique.

,,,,,, Spectrum analysis where is the spatial spectrum of electron density fluctuations; is the dispersionof the relative electron density fluctuations are flow thickness, the outer and inner turbulence scales., ; ; The spectrum of the intensity fluctuations in one point. For multi-flow model

Dispersion analysis The cross-correlation between scintillations in two points The cross-spectrum The dispersion dependence whereis the interferometer base r

Observations Radio telescope UTR-2Radio telescope URAN-2 Radio telescopes operate at the frequencies from 9 to 32 MHz.

The scintillation spectra (a) and dispersion curves (b) for radio source 3C196 a b The example of the model fitting

The reconstructedstructure of the solar wind The reconstructed structure of the solar wind

The annual statistics of the velocities of slow(solid line) and fast (dashed line) solar wind streams in the outer heliosphere. The annual statistics of the velocities of slow(solid line) and fast (dashed line) solar wind streams in the outer heliosphere.

The annual statistics of the spectral indices of the electron density fluctuations of slow (solid line) and fast (dashed line) solar wind streams.

Tracking of high-speed solar wind streams in the outer heliosphere The solar wind parameters obtained by Genesis Discovery Mission The solar wind parameters obtained by IPS observations

Harmful effects Ionospheric effects. Ionospheric effects. Radio interference. Radio interference. Angular broadening due to interstellar scattering. Angular broadening due to interstellar scattering. Records of scintillations at decameter wavelengths contain evidences both the interplanetary medium impact and Earth’s ionosphere effects.

LOFAR’s frequency range, from 10 to 250 MHz, will provide an excellent possibility to observe the interplanetary scintillations at all radio source elongations, in other words, to probe the interplanetary plasma in the inner and outer heliosphere, simultaneously. LOFAR’s frequency range, from 10 to 250 MHz, will provide an excellent possibility to observe the interplanetary scintillations at all radio source elongations, in other words, to probe the interplanetary plasma in the inner and outer heliosphere, simultaneously. As for the outer heliosphere, perhaps, the use of the frequencies from 30 to MHz allows us to minimize the harmful effects of the ionosphere and radio interference and to increase the number of the compact radio sources that are suitable for IPS observations with the preservation of the method sensitivity. As for the outer heliosphere, perhaps, the use of the frequencies from 30 to MHz allows us to minimize the harmful effects of the ionosphere and radio interference and to increase the number of the compact radio sources that are suitable for IPS observations with the preservation of the method sensitivity.