REGISTRATION
PERSONAL INFORMATION
| Submission Time: | 2017-07-10 03:28:41 UTC |
| Email: | zucca@astron.nl |
| First Name: | Pietro |
| Middle Name: | |
| Last Name: | Zucca |
| Name as it appears on badge : | Pietro Zucca |
| Affiliation: | ASTRON - Netherlands Institute for Radio Astronomy |
| Nationality: | Italian |
| Degree: | Dr. |
| Preferred Working Group 1st Choice: | WG 6 (Solar Energetic Particles) |
| Preferred Working Group 2nd Choice: | WG 1 (Data) |
PRESENTATION
| Title : | Shock location and CME 3D reconstruction of the first spatial resolved solar type II radio burst with LOFAR. |
| Abstract | |
| Type II radio bursts are evidence of shocks in the solar atmosphere emitting radio waves ranging from metric to kilometric lengths. These shocks may be associated with coronal mass ejections (CMEs) reaching super-Alfvénic speeds. Radio imaging of the decametre wavelengths (90–20 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window to study coronal radio shocks leaving the inner solar corona and entering the interplanetary medium and understand their association with CMEs. Here, we study a coronal shock associated with a CME and type II radio burst to determine the location where the shock is triggered in relation to the propagating CME, the ambient medium Alfvén speed and the orientation of the coronal magnetic field. The type II shock imaging and spectra were obtained using 91 simultaneous tied-array beams of LOFAR while the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments onboard the Solar Terrestrial Relation Observatory (STEREO). Coronal magnetic fields were obtained from the heliospheric imager (HMI) onboard the Solar Dynamic Observatory (SDO). The radio emission associated with the type II shock was found to be located at the flank of the CME in a region where the mach number is between 1.4 to 1.8 and the shock geometry is quasi-parallel with θ ∼ 70 degrees. Using the tied array beam observing mode of LOFAR we were able to locate the type II radio shock position between 50 and 70 MHz and relate it to the expanding flank of a CME leaving the inner corona. We were also able to show that the type II radio emission originated in a region were the expanding flank reaches super Alfvénic speeds and encounters a quasi-perpendicular geometry of the magnetic field. |
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LUNCH
Sep. 18, Sep. 19, Sep. 20, Sep. 21, Sep. 22
List
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