Presentation is loading. Please wait.

Presentation is loading. Please wait.

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.

Published byCornelia Warren Modified over 8 years ago

Similar presentations

Presentation on theme: "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."— Presentation transcript:

1 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 MPIfR, Germany

2 Introduction Most important characteristic of the turbulent interstellar medium is the three-dimensional spatial spectrum of the electron density fluctuations: a Gaussian or power law. The aim of our project was to obtain the form of turbulence spectrum for different regions of the sky and for pulsars which are at different distances.

3 Observations 100m RT in Effelsberg during 2-12th Sept. 2003 15 pulsars at 1.4GHz and 6 at 4.85GHz Criteria: strong objects with good SNR, pulsars should clearly show scintillation to obtain dynamic spectra the total receiver bandwidht must be much broader then the decorrelation bandwidth of pulsars 1.4GHz: 30chan x 1.33MHz= 40MHz 4.85GHz: 8chan x 60MHz=480MHz two polarization; flux measurements every 30sec; duration of observations 1-10hours

4 PSR 0329+54 (1.41GHz) Example of dynamic spectra in the strong scintillation regime

5 PSR 1929+10 (1.4GHz; 7 Sept.) Example of dynamic spectra in the weak(?) scin.regime

6 PSR 1929+10 (1.4GHz) Scin. data; ACF time function; CCF frequency function; power spectrum; structure function

7 PSR 2020+28 (1.4GHz) 03 Sept. - strong scint; 10 Sept. - lensing effect

8 PSR 2020+28 (1.4GHz) Scint. data; ACF time function; CCF frequency function; power spectrum structure function

9 PSR 1642-03 (4.85GHz) Dynamic spectra in the weak scin. regime

10 PSR 0355+54 (4.85GHz) Dynamic spectra in the strong(?) scin.regime

11 PSR 0355+54 Scint. data; ACF time function CCF frequency function Power spectrum Structure function

12 Number of pulsars

13 Conclusion We have obtained scintillation data for 11 PSR at 1.4GHz and 5 PSR at 4.85GHz: the decorrelation time and bandwidth, power low index for spectra and structure function Possible lensing effect (focal spot effect) have been detected for a few pulsars near the critical frequency

Download ppt "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."

Similar presentations

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

Pulsar radio wave dispersion, intermittency, and kinetic Alfvén wave turbulence Paul Terry Stas Boldyrev.
Primary results of polarization survey of large-SNRs at 6cm Li Xiao, XiaoHui Sun, Chen Wang, WeiBin Shi, Wolfgang Reich, JinLin Han Partner Group of MPIfR.

Primary results of polarization survey of large-SNRs at 6cm Li Xiao, XiaoHui Sun, Chen Wang, WeiBin Shi, Wolfgang Reich, JinLin Han Partner Group of MPIfR.
Probing cosmic plasma with Giant Radio Pulses June 22, 2006 “Scattering and Scintillation in Radio Astronomy’’ Vladislav Kondratiev, Michael Popov, Vladimir.

Probing cosmic plasma with Giant Radio Pulses June 22, 2006 “Scattering and Scintillation in Radio Astronomy’’ Vladislav Kondratiev, Michael Popov, Vladimir.
Preliminary results of giant pulse investigations from Crab pulsar with Radioastron. Rudnitskiy A.G., Popov M.V., Soglasnov V.A. 12 th EVN SYMPOSIUM Cagliari,

Preliminary results of giant pulse investigations from Crab pulsar with Radioastron. Rudnitskiy A.G., Popov M.V., Soglasnov V.A. 12 th EVN SYMPOSIUM Cagliari,
The Highest Time-Resolution Measurements in Radio Astronomy: The Crab Pulsar Giant Pulses Tim Hankins New Mexico Tech and NRAO, Socorro, NM Extreme Astrophysics.

The Highest Time-Resolution Measurements in Radio Astronomy: The Crab Pulsar Giant Pulses Tim Hankins New Mexico Tech and NRAO, Socorro, NM Extreme Astrophysics.
Emmision of the remarkable pulsar B0943+10: Continual changes in the subpulse drift rate and in integrated pulse shape, intensity and polarization at frequencies.

Emmision of the remarkable pulsar B : Continual changes in the subpulse drift rate and in integrated pulse shape, intensity and polarization at frequencies.
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.

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.
ITER reflectometry diagnostics operation limitations caused by strong back and small angle scattering E.Gusakov 1, S. Heuraux 2, A. Popov 1 1 Ioffe Institute,

ITER reflectometry diagnostics operation limitations caused by strong back and small angle scattering E.Gusakov 1, S. Heuraux 2, A. Popov 1 1 Ioffe Institute,
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.

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.
VSOP-2 Observations of Pulsars Carl Gwinn * With D.L. Jauncey 2, S. Dougherty 3, H. Hirabayashi 4, J.E. Reynolds 2, A. K. Tzioumis 2, E.A. King 2, B. Carlson.

VSOP-2 Observations of Pulsars Carl Gwinn * With D.L. Jauncey 2, S. Dougherty 3, H. Hirabayashi 4, J.E. Reynolds 2, A. K. Tzioumis 2, E.A. King 2, B. Carlson.
Contour statistics, depolarization canals and interstellar turbulence Anvar Shukurov School of Mathematics and Statistics, Newcastle, U.K.

Contour statistics, depolarization canals and interstellar turbulence Anvar Shukurov School of Mathematics and Statistics, Newcastle, U.K.
Pulsar broadening measurements at low frequencies with LOFAR Kimon Zagkouris University of Oxford In collaboration with the LOFAR Pulsar Working Group.

Pulsar broadening measurements at low frequencies with LOFAR Kimon Zagkouris University of Oxford In collaboration with the LOFAR Pulsar Working Group.
Detection of Giant pulses from pulsar PSR B0950+08 Smirnova T.V. Pushchino Radio Astronomy Observatory of ASC FIAN Pushchino Radio Astronomy.

Detection of Giant pulses from pulsar PSR B Smirnova T.V. Pushchino Radio Astronomy Observatory of ASC FIAN Pushchino Radio Astronomy.
Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ 100-1000 pc (3 x 10 16 Km)

Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)
Mean pulse profiles and spectra at the low frequencies Malov O.I., Malofeev V.M. Malov O.I., Malofeev V.M. Pushchino Radio Astronomy Observatory.

Mean pulse profiles and spectra at the low frequencies Malov O.I., Malofeev V.M. Malov O.I., Malofeev V.M. Pushchino Radio Astronomy Observatory.
Variability of the Flux Densities of Radio Sources on Timescales Shorter than a Month A.G. Gorshkov 1, V.K.Konnikova 1 M. Mingaliev 2 1 - Sternberg Astronomical.

Variability of the Flux Densities of Radio Sources on Timescales Shorter than a Month A.G. Gorshkov 1, V.K.Konnikova 1 M. Mingaliev Sternberg Astronomical.
Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Mejía-Ambriz.

Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Remote Sensing of Solar Wind Velocity Applying IPS Technique using MEXART Mejía-Ambriz.
8 th EVN Symposium: Exploring the universe with the real-time VLBI. 26 – 29 September 2006.Giuseppe Cimò – JIVE Interstellar Scintillation and IDV Twinkle,

8 th EVN Symposium: Exploring the universe with the real-time VLBI. 26 – 29 September 2006.Giuseppe Cimò – JIVE Interstellar Scintillation and IDV Twinkle,
Simultaneous monitoring observations of solar active regions at millimeter wavelengths at radio telescopes RT-7.5 BMSTU (Russia) and RT-14 Metsahovi radio.

Simultaneous monitoring observations of solar active regions at millimeter wavelengths at radio telescopes RT-7.5 BMSTU (Russia) and RT-14 Metsahovi radio.
First Result of Urumqi 6cm Polarization Observations: Xiaohui Sun, Wolfgang Reich JinLin Han, Patricia Reich, Richard Wielebinski Partner Group of MPIfR.

First Result of Urumqi 6cm Polarization Observations: Xiaohui Sun, Wolfgang Reich JinLin Han, Patricia Reich, Richard Wielebinski Partner Group of MPIfR.

Similar presentations

Ads by Google