tailieunhanh - Astrophysics and Space Science Proceedings Phần 10

Ooty IPS hình ảnh hiển thị vị trí bảng hiện tại (trên cùng bên trái), lệch CME lỗ hào quang (trên bên phải), nén CME của gió mặt trời (phía dưới bên trái), và tuyên truyền CME (dưới cùng bên phải). | Interplanetary Consequences of a Large CME 491 22 00 21 00 23 00 20 00 SCET rau 21 Hours 30 22 1 25 20 - 15 - 10 - 5 0 u Fig-2 Radio spectra from the WAVES and Cassini missions. Cassini was located at AU Flux log 1000 100 10 104 6d00h 12h 12h 12h 5d00h 7d00h 4d12h Day and Time UT Fig-3 Particle profiles in different energy bands 492 M. Lahkar et al. 7 8 I-. . Nov2003 Date Fig. 5 1-AU and Ulysses hourly averages of solar wind parameters Fig. 4 Ooty IPS images showing the current sheet location top left CME deflection by the coronal hole top right CME compression of the solar wind bottom left and CME propagation bottom right . The Sun is located at the center of each image. The two images at top right represent solar-wind speed the others represent density As Ulysses was favorably located in the CME propagation direction it could record the nose part of the CME and its shock as indicated by a speed value of over 900 km s-1 at 5 AU. At Earth the shock speed was below 600 km s-1 suggesting that the eastern tail swept the Earth. From these measurements we infer a speed profile V R a to Earth. However the deceleration V R 2 out to 5 AU near Ulysses implies gradual decline in speed along the CME propagation direction which is in good agreement with the IPS measurements. Interplanetary Consequences of a Large CME 493 3 Conclusion Our study shows the characteristics of a fast-moving CME and its interactions with transient and solar-wind structures at different distances from the Sun with good consistency between diverse diagnostics. The enhancement in radio emission and production of high-energy particles suggest that the magnetic field associated with the CME was strong. The gradual decline in CME speed suggests that the internal magnetic energy of the CME supported its propagation including expansion in overcoming the aerodynamical drag imposed by the ambient solar wind . Manoharan 2006 . Acknowledgment We thank the Cassini GOES SOHO