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

Slides:

Advertisements

Similar presentations

Observations of turbulence in the magneto-ionized ISM on subparsec scales Marijke Haverkorn.

Advertisements

Probing cosmic plasma with Giant Radio Pulses June 22, 2006 “Scattering and Scintillation in Radio Astronomy’’ Vladislav Kondratiev, Michael Popov, Vladimir.

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 Extreme Dimension: Time-Variability and The Smallest ISM Scales Dan Stinebring Oberlin College.

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.

Diffuse Gamma-Ray Emission Su Yang Telescopes Examples Our work.

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.

YERAC On the structure of radio pulsar magnetospheres On the structure of radio pulsar magnetospheres Igor F. Malov, Еlena Nikitina Pushchino Radio.

Microstructure in the Ionized ISM from radio scattering observations. Barney Rickett UC San Diego O’Dell Symposium Lake Geneva WI April 2007.

Radio Diagnostics of Turbulence in the Interstellar & Intergalactic media J. M. Cordes, Cornell University URSI 20 August 2002.

The Transient Universe: AY 250 Spring 2007 Existing Transient Surveys: Radio II: Interferometric Surveys Geoff Bower.

New observations of three AXPs at low radio frequencies Daria Teplykh & V.M. Malofeev, A.E. Rodin, S.V. Logvinenko. Pushchino Radio Astronomy Observatory.

THE SEARCH OF GIANT RADIO GALAXIES AT DECLINATIONS FROM 3 TO 12 DEGREES Pushchino Radio Astronomy Observatory of Astro Space Center Tyul’bashev S.A., Gliantsev.

1/9/2007Bilkent University, Physics Department1 Supercontinuum Light Generation in Nano- and Micro-Structured Fibers Mustafa Yorulmaz Bilkent University.

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 ~ pc (3 x Km)

Long-term monitoring of RRAT J HU HuiDong Urumqi Observatory, NAOC July 27, 2009 Rotating Radio Transients Observation.

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 Sternberg Astronomical.

Observations of Intra-Hour Variable Quasars Hayley Bignall (JIVE) Dave Jauncey, Jim Lovell, Tasso Tzioumis (ATNF) Jean-Pierre Macquart (NRAO/Caltech) Lucyna.

Interstellar Scattering Joseph Lazio (Naval Research Laboratory) J. Cordes, A. Fey, S. Spangler, B. Dennison, B. Rickett, M. Goss, E. Waltman, M. Claussen,

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,

What do Scintillations tell us about the Ionized ISM ? Barney Rickett UC San Diego SINS Socorro May 2006.

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

Pulsar Studies at Urumqi Na Wang Urumqi Observatory, NAOC.

Pulsar study using SKA Osamu KAMEYA （ NAOJ, Mizusawa VLBI Observatory ）

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,

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.

RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing,

Gravitational Wave and Pulsar Timing Xiaopeng You, Jinlin Han, Dick Manchester National Astronomical Observatories, Chinese Academy of Sciences.

Aristeidis Noutsos University of Manchester. Pulsar Polarization Pulsar radiation is elliptically polarised with a high degree of linear polarization.

Steven R. Spangler, Department of Physics and Astronomy

Scintillation in Extragalactic Radio Sources Marco Bondi Istituto di Radioastronomia CNR Bologna, Italy.

Methods for describing the field of ionospheric waves and spatial signal processing in the diagnosis of inhomogeneous ionosphere Mikhail V. Tinin Irkutsk.

A Non-Radial Oscillation Model for Radio Pulsars In collaboration with Dr. J. Christopher Clemens University of North Carolina at Chapel Hill.

Pulsar Data analysis Desh, Anish RRI MWA Meeting Canberra, January

Scuola nazionale de Astrofisica Radio Pulsars 2: Timing and ISM

Pulsar Scintillation Arcs and the ISM Dan Stinebring Oberlin College Scattering and Scintillation In Radioastronomy Pushchino 19–23 June 2006.

Low frequency observation of both pulsar wind and magnetodipole radiation from switch on-off pulsars Ya.N. Istomin P.N. Lebedev Physical Institute, Moscow,

Scintillation from VERY Small-Scale HI Carl Gwinn (UCSB), John Reynolds (CSIRO), Warwick Wilson (CSIRO) Theory: CG, ApJ 2001 See also:

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

OH maser sources in W49N: probing differential anisotropic scattering with Zeeman pairs desh Raman Research Institute, Bangalore + Miller Goss, Eduardo.

Scattering and Scintillation in Radio Astronomy 1 The dual-frequency calibration of ionosphere influence in VLBA data processing Andrey Chuprikov.

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.

Detection of giant component from pulsar PSR J V.M. Malofeev, D.A. Teplykh, O.I. Malov and S.V. Logvinenko Pushchino Radio Astronomy Observatory.

-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 Power Spectra and Point Distribution Functions of Density Fields in Isothermal, HD Turbulent Flows Korea Astronomy and Space Science Institute Jongsoo.

What Goes into a Pulsar Timing Model? David Nice Physics Department, Princeton University Pulsar Timing Array: A Nanohertz Gravitational Wave Telescope.

Project P2445 – Four-Frequency High Precision Timing of a Millisecond Pulsar Ryan Shannon (PI, Graduate Student, Cornell University), with Jim Cordes,

Low Frequency Observations of the ISM and Pulsar Timing Joris Verbiest Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF)

Spectrum and small-scale structures in MHD turbulence Joanne Mason, CMSO/University of Chicago Stanislav Boldyrev, CMSO/University of Madison at Wisconsin.

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 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,

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.

p no Bhaswati Bhattacharyya On behalf of GHRSS team

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

Long-Term Timing of Globular Cluster Pulsars

A Turbulent Local Environment

Steven R. Spangler University of Iowa

Ten Years of Millisecond Pulsar Timing at Kalyazin

Steven R. Spangler University of Iowa

Extrasolar planet detection: a view from the trenches

Polarization Properties of an Eclipsing Pulsar

Instructor: Gregory Fleishman

GALACTIC ASTRONOMY (II): PULSARS

Presentation transcript:

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

1. Relations of pulsar observations to the turbulent plasma spectrum 2. Construction of the structure function from multi-frequency observations 3. Measurements of the ISM spectrum in the directions to PSR , , , , Conclusions

Diffractive scintillation Inhomogeneities of size s d = /2  sc ~ 10 7  cm Time scale t d = s d /V ~ sec  min Frequency scale f d = c/(  R  sc 2 ) ~ KHz  MHz Modulation index, m  1 Refractive scintillation Inhomogeneities of size s r = R  sc ~  cm Time scale T ref = s r /V ~ weeks  months s r s d ~ R (Frenel scale) 2 Dispersive arrival times, angular broading, time of arrival fluctuations, pulse broading

Electron density irregularities in the plasma cause random phase perturbations of the wavefront. These are characterized by the phase structure function: D s (  ) = S = const  (f 0 /f)  DM For a power-law spectrum  Ne (q) = C Ne 2  q  -n, 2  /l i  q  2  /l out n = 11/3 for Kolmogorov spectrum D s (  ) =const  2 C Ne 2 (  ) n-2, q = 1/  Diffractive scintillation Correlation function of flux variations I(t) is described by the equation B I (t) = 2 exp[- D S (t)]. If t 0 is the characteristic scale of intensity variations we have D S (t 0 ) = 1 D S (t)  [B I (0) – B I (t)]/ 2  (1/2) D I (t)/ 2, t << t 0 D S (t)  D S (  ) by  = Vt

In frequency domain: D S (  f)  (n-2) [B I (0) – B I (  f)]/ 2 To reduce D S (  f) to frequency f 0 : D S (  f, f 0 ) = (f/f 0 ) 2 D S (  f,f)  f(f 0 ) = (f 0 /f) 2  f(f) For the case of strong angular refraction,  ref >>  dif :  f(f 0 ) = (f 0 /f) 3  f(f),  ref = 3Vf/R  (  t/  f) The slope of D S (  f ) is the same as D S (  t)

Refractive scintillation For homogeneous medium D s (  ) = m ref 2 /(6(4-n))  (T ref /t dif ) 2  = VT ref Variations of DM D DM (  ) = A (f 0 / f) 2, A = 6, pc -2 cm 6 Pulsar timing D s (t) = (2  f) 2 2  τ 2

dash line: n = 3.5 straight line: n = 11/3

Interstellar plasma spectrum in the direction to PSR , Shishov, Smirnova, Siber et al., 2003 R = 1 kpc, V = 95 km/s (parallax) Data: f = 102, 610, 4860 MHz Flux variations, T ref =17 days, m=0.37 at 610 MHz (Stinebring et al., 2000) Timing during 30 years, residuals  t = 0.7 ms at 103 MHz (Shabanova, 1995) Reference frequency f 0 = 1000 MHz

 = 1.47

straight line: 1.5 dash line: 1.67

Interstellar plasma spectrum in the direction to PSR , Smirnova, Shishov, Siber et al., A&A, Data: f = 102, 340, 610, 800, 4860 MHz  = 30 mas/year (Brisken et al., 2003), R – 160 pc ? R = 160 pc, V = 22 km/s; R = 2.9 kpc, V = 400 km/s  sc = 6.8 mas at 326 MHz (Gwinn et al., 1993) Flux variations, T ref = 0.9 days, m = 0.46 at 610 MHz (Stinebring et al., 2000) Timing during 8.5 years, residuals  t = 1 ms at 103 MHz (Shabanova et al, 2001)

Interstellar plasma spectrum in the direction to PSR (Smirnova, Gwinn, Shishov, A&A, 2006 R = 150 pc, V = 100 km/s (parallax) Data: f = 152, 327, 436 MHz fdif = 16 MHz, tdif = 17 min at 328 MHz (Gwinn et al. 2006)

PSR R = 433 pc, V = 102 km/s (Brisken et al. 2002) Observations: f = 41, 62.43, and MHz December - January 2001, 2003, 2004 DKR: time duration 35.3 min BSA: T = 12 min Time resolution 2.56 ms or 5.12 ms B = 128  20 KHz and 128  1.25 KHz at 41 MHz Time averaging 19.4 s (15 P1) at 113 MHz, 39 s at 88 MHz, 62 and 41 MHz

PSR R = 262 pc, V = 36.6 km/s (Brisken et al. 2002) Observations: f = 41, 62.43, and MHz December - January 2001, 2003, 2004 DKR: time duration min BSA: T = 3.2 min Time resolution 2.56 ms or 5.12 ms B = 128  20 KHz and 128  1.25 KHz at 41 MHz Time averaging 15.2 s (60 P1) at 113 MHz, s at 88 MHz, 62 and 41 MHz

Conclusions 1.Multi-frequency observations of pulsar interstellar scintillation give us new and more accurate information about the shape of turbulent spectrum in the definite directions of the sky. 2. Interstellar plasma spectrum for 4 from 5 pulsars is well described by a power law with n from 3 to 3.5 for scales from 10 7 to cm which is different from Kolmogorov one. 3. We detected strong angular refraction of radiation in the direction to 3 pulsars: , and The spectrum in the direction to PSR has a changing of slope from n = 3.3 for scales less than 10 9 cm to n = 3.7 for scales from 10 9 to cm (Kolmogorov spectrum).