Simultaneous Near-Sun Observations of a Moving Type IV Radio Burst and the Associated White-Light Coronal Mass Ejection

Variation in Coronal Activity from Solar Cycle 24 Minimum to Maximum Using Three-Dimensional Reconstructions of the Coronal Electron Density from STEREO/COR1

“…This suggests that our SSPA 3D coronal density models reconstructed for 100 CRs (with a cadence of about two weeks) may be used for the interpretation of radio bursts (such as type II and moving type IV produced by CMEs) as observed from the Earth direction (e.g. Cho et al, 2007;Ramesh et al, 2013;Shen et al, 2013;Sasikumar Raja et al, 2014;Hariharan et al, 2016;Lee et al, 2016), in particular, when LASCO/C2 pB data are not available. We estimate the total mass (or electron content) contained in the coronal region observed with COR1 and its evolution with solar cycle.…”

Strength of the Solar Coronal Magnetic Field – A Comparison of Independent Estimates Using Contemporaneous Radio and White-Light Observations

“…Stokes I, alone (Smerd, Sheridan, and Stewart, 1975;Gopalswamy and Kundu, 1990;Bastian et al, 2001;Vršnak et al, 2002;Mancuso et al, 2003;Cho et al, 2007;Kishore et al, 2016) or both the total and circularly polarized intensities, i.e. Stokes I and V (Dulk and Suzuki, 1980;Gary et al, 1985;Ramesh et al, 2010a;Ramesh, Kathiravan, and Narayanan, 2011;Tun and Vourlidas, 2013;Sasikumar Raja and Ramesh, 2013;Hariharan et al, 2014;2016b;Anshu et al, 2017). Note that we have mentioned only Stokes I and V emission here since differential Faraday rotation of the plane of polarization in the solar corona and Earth's ionosphere makes it impossible to observe the linear polarization (represented by Stokes Q and U ) within the typical observing bandwidths of ≈ 100 kHz (see for example Grognard and McLean, 1973.)…”

Solar physics with the Square Kilometre Array

“…The stationary type IV bursts emanate from electrons trapped in post-eruption arcades behind CMEs while the moving ones correspond to CME-related outward-moving material. Stationary type IV bursts should arise from plasma emission mechanism, while plasma emission (e.g Duncan, 1981;Stewart et al, 1982;Gopalswamy & Kundu, 1989;Klein & Mouradian, 2002;Ramesh et al, 2013;Hariharan et al, 2016), and more rarely gyrosynchrotron emission from nonthermal electrons (Gopalswamy & Kundu, 1987;Bastian et al, 2001;Maia et al, 2007;Tun & Vourlidas, 2013;Bain et al, 2014;Carley et al, 2017) have beeen invoked for the interpretation of the properties of moving type IV bursts. The detection of gyrosynchrotron emission from some CMEs (see Figure 7 for an example), is important because, if combined with modeling (see Section 8.3), it could provide estimates about the CME magnetic field; in the publications cited above, CME magnetic fields from 15 to 0.1 G have been reported at heights from 1.3R ⊙ to 2.8R ⊙ .…”