Secchirh

14 Aug 2010 : Radio emission

Renaud Romagnan — 2018-07-13T08:50:03Z

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28 October 2003 On the Disk Halpha and Radio Observations of the Flare and Coronal Mass Ejection Event

Renaud Romagnan — 2018-07-13T08:44:45Z

The spectrum includes an interplanetary type III burst which starts, in the low corona at decimeter wave length, a type II burst and a complex continuum.

The Halo CME seen (SOHO/LASCO)

NRH 164 MHz

NRH image at 410 MHz (11:04 UT) with the position of the Moreton wave (11:05 UT) superposed.

The evolution of the Halpha and radio emissions seen by the Meudon H ? telescope and the NRH are associated with a X17.2 flare and a halo CME. At 164 MHz, radio images show that the emission covers the whole disk of the Sun and extends as far as 1.8 Rs from the sunÕs center in a few minutes. The radio emissions, the Moreton wave seen in H ?, and the CME all show a similar temporal and spatial development and the three phenomena are likely to be related.

(Pick et al., The Astrophysical Journal, Volume 631, Issue 1, pp. L97-L100, 2005)

20 february 2002 Comparisons of hard X-ray (HXR) sources and radio emission sources

Renaud Romagnan — 2018-07-13T08:42:56Z

The event analysed shows a close correspondence between the changes in the HXR 25-40 keV sources and the decimetric radio sources at 410 MHz, on the time scale of a few seconds. This close correspondence suggests common acceleration/injection sites for HXR and decimetric radio emitting electrons. The radio observations from NRH are shown in white contours, and the HXR observations from RHESSI are shown in black contours.

(Vilmer et al., Solar Physics, v. 210, Issue 1, p. 261-272, 2002)

14 July 2000 The on-disk Bastille event : Angular expansion of the Halo CME

Renaud Romagnan — 2018-07-13T08:35:54Z

The analysis of multi-wavelength, high-cadence images obtained from the NRH shows the on-disk signatures of the initiation of the CME at low-coronal heights, <=2 Rs The formation of the CME inferred from the radio data indicates a nearly developed halo at the low corona.

(Maia et al., Solar Physics, 204, Issue 1/2, p. 197-212, 2001)

20 April 1998 Radio CME and CME driven shock

Renaud Romagnan — 2018-07-13T08:34:04Z

Panel b shows an ensemble of expanding loops which closely looks like the white light CME imaged in Panels a and c. These loops, so-called radio CME, are detected up to 3Rs behind the CME front. The white lines in b indicate the position of the leading edge of the CME at the times shown in a and c.
(Bastian et al., The Astrophysical Journal, Volume, 558, L65, 2001)

NRH images showing the outward progression of a weak type II radio source(indicated by the arrows at two different frequencies. The source in the northern quadrant is a stationary noise storm.
(Maia et al. The Astrophysical Journal, 528, L49, 2000)

02 May 1998 Halo CME associated with on-disk electromagnetic disturbances

Renaud Romagnan — 2018-07-13T08:33:00Z

Complex radio event which includes type III and type II bursts and various continua.

Artemis IV radio spectrum : the type II burst includes successive spectral drifting components M1, M2 and M3

Panel a : A LASCO/SOHO image showing the halo CME. Panel d : Running difference of Kanzelhohe H ? images showing the moving H ? wave front (marked by an arrow in the first difference image).
Panel c : The radio type II-like burst sources seen by the NRH (labelled M1, M2, and M3 are located near the wave fronts.
Panel b : EUV dimming region shown in an EIT/SOHO image. A 236 MHz image is over plotted in contours. At the time of the EIT image, this ascending moving radio source had already left.

(Pohjolainen et al., The Astrophysical Journal, Volume, 556, Issue 1, pp. 421-431, 2001)

View survey

06 Nov 1997 : Expansion in latitude of the Coronal Mass Ejection

Renaud Romagnan — 2018-07-13T08:24:29Z

Upper panel : Radio images at distinct frequencies which show the complexity of the emitting region ; the emission expands toward the northern hemisphere.

Lower panel : Composite image of a SOHO/LASCO C2 image with a NRH image at 164 MHz showing that there is a close correspondence between the extent in latitude of the white light CME and the sites of the radio emission

(Maia et al., JGR, 104, 12507, 1999)