1. 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 Center, Lebedev Physical Institute

2. ABSTRACT The results are presented of radio sounding observations probing the inner solar wind near the minimum of solar activity cycle using polarized pulsar pulses from PRS B0525+21 and PSR B0531+21 received when the lines of sight toward these pulsars was close to the Sun. The observations were obtained in June 2005 and June 2007 on the Large Phased Array of Lebedev Physical Institute at 111 MHz. An upper limit for the scattering of giant pulses from PSR B0531+21 due to their passage through the turbulent solar wind plasma is determined. The arrival-time delays for pulses from PSR B0531+21 are used to derive the radial dependence of the mean density of the circumsolar plasma. The resulting density distribution indicates that the acceleration of fast high latitude solar wind outflows continues to heliocentric distances of 5-10 R S, where R S is the solar radius. The mean plasma density at heliocentric distances of about 5 R S is 1.4  10 4 cm -3, substantially lower than at solar activity maximum. This is associated with the presence of polar coronal holes. The Faraday rotation measure at heliocentric distances of 6-7 R S is estimated. Deviation of the spatial distribution of the magnetic field from spherical symmetry are comparatively modest in the studied range of heliocentric distances.

3. Propagation effects of pulsed signals in the solar wind Dispersion delay of pulses Scattering of pulses on electron density fluctuations Faraday rotation of polarization plane

4. Dispersion delay of pulses  t = A  2  DM, A = const DM =  N dz

5. Scattering of pulses on electron density fluctuations Structure function of radio wave phase fluctuations D S (  ) =2  ( r e ) 2 (  /l) 2 l  R eff l – turbulence inner scale Wave field coherence scale  0 D S (  0 ) = 1 Scattering angle  sc  sc = / 2   0 Pulse broadening by scattering  sc = z  sc 2 / 2 c

6. Scattering of pulses on electron density fluctuations t I(t) = I 0  exp ( - t 2 /  0 2 ) exp [( t - t) /  sc ] dt -  I(t) = I 0 exp (  0 2 /4  sc 2 – t/  sc ) [ 1 -  (  0 /2  sc – t/  0 ) ] Max. at t   0

7. Faraday rotation of polarization plane  = C  2  RM, C = const RM =  N B z dz

8. Observations Radio telescope BSA LPI : geometric area 70 000 м 2, operation frequency 111 МHz Receiver: 96 channels  20 кГц, whole bandwidth 1.92 МHz, integration time 2.68 мs Pulsar В 0525+21: period 3,74 s, two components, polarization degree 40-50 %; yy 2005, 2007. Pulsar in the Crab nebula В 0531+21: period 33 мs, giant pulses, polarization degree10 % ; y 2007.

9. Antenna BSA LPI

11. Pulsars coronal occultation

12. Example of pulsar В 0525 record

13. Dispersion delay for pulsar PSR В 0525, 2005, 2007

14. Pulse delay and ambient plasma density Dispersion delay upper estimate :  t < 2 ms  DM < 2  10 16 cm -2  N (5.5 R  ) < 2  10 4 cm -3 (2005)  t < 4 ms  DM < 4  10 16 cm -2  N (5.5 R  ) < 4  10 4 cm -3 (2007) Counselman & Rankin, 1969-1970 observations, 111-430 Мгц :  t  5 ms, N (10 R  )  7  10 3 cm -3, N (5.5 R  )  6  10 4 cm -3

15. Dispersion delay for PRS B 0531, 2007

16. Density dependence on the distance from the Sun, PSR B 0531, 2007

17. Giant pulses of PSR В 0531

18. PSR В 0531scattering

19. Scattering and density fluctuations Upper estimate of pulse broadening (B 0531):  sc < 2 ms  scattering angle  sc < 3 10 -3 rad  10 Counselman & Rankin, 1969-1970 observations, 111-430 МHz :  sc  6 ms

20. PSR В 0525 Faraday rotation

21. Rotation measure radial profile В 0525

22. Rotation measure Rotation measure upper estimate at R = 7 R  : RM < 6 rad/m 2 (2005 y.) RM < 3 rad/m 2 (2007 y.) Bird et al., observations 1978-1979 y.: RM < 10 rad/m 2

23. Conclusions Our estimates of  t,  sc show, that in the years 2005-2007 mean density, as well density fluctuations were several times (2-3) lower, than in observations 1969-1970 г. (Counselman & Rankin). During period of closest approach solar offset point of radio path was located at high heliolatitudes, about 80 о. Possible explanation: polar coronal hole with low plasma density at solar activity minimum. Our estimates of rotation measure are in agreement with the results of Bird et al., (1978-1979г.). The deviations in spatial magnetic field distribution from spherically symmetric are modest: B ns 2  10 -2 G. Radial density profile ( B 0531, 2007) show that the acceleration of fast solar wind continues up to the distances about 5 – 10 R S.