Low-Frequency Observations of Drifting, Non-Thermal Continuum Radio Emission Associated With the Solar Coronal Mass Ejections

Ramesh, R.; Kishore, P.; Mulay, Sargam M.; Barve, Indrajit V.; Kathiravan, C.; Wang, T. J.

doi:10.1088/0004-637x/778/1/30

Cited by 21 publications

(16 citation statements)

References 55 publications

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“…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.…”

Section: Discussionmentioning

confidence: 99%

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

et al. 2017

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Section: Discussionmentioning

confidence: 99%

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

et al. 2017

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“…Solar observations with the help of Gauribidanur Radio Heliograph at 80 MHz supplemented by spectral data records within 35-85 MHz belong to more modern researches on the lowfrequency type IV radiation. However, the moving type IV bursts were only taken into account in a few studies (Ramesh et al 2013;Sasikumar Raja et al 2014).…”

Section: Introductionmentioning

confidence: 99%

“…To explore the outer corona, a number of groundbased radio telescopes developing in recent years has been involved. The low-frequency antenna arrays focus on imaging and spectral measurements, implemented by the LOw Frequency ARray (LOFAR; van Haarlem et al 2013), the Murchison Widefield Array (MWA; Tingay et al 2013), and upgraded Indian facilities in the Gauribidanur Radio Observatory (Ramesh et al 2013). Also, the solar-dedicated Nançay Radio Heliograph produces valuable solar images in meter-decimeter range.…”

Section: Introductionmentioning

confidence: 99%

A Decameter Stationary Type Iv Burst in Imaging Observations on 2014 September 6

Koval

Stanislavsky

Chen

et al. 2016

ApJ

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First-of-its-kind radio imaging of decameter solar stationary type IV radio burst has been presented in this paper. On 6 September 2014 the observations of type IV burst radio emission have been carried out with the two-dimensional heliograph based on the Ukrainian T-shaped radio telescope (UTR-2) together with other telescope arrays. Starting at ∼09:55 UT and throughout ∼3 hours, the radio emission was kept within the observational session of UTR-2. The interesting observation covered the full evolution of this burst, "from birth to death". During the event lifetime, two Cclass solar X-ray flares with peak times 11:29 UT and 12:24 UT took place. The time profile of this burst in radio has a double-humped shape that can be explained by injection of energetic electrons, accelerated by the two flares, into the burst source. According to the heliographic observations we suggest the burst source was confined within a high coronal loop, which was a part of a relatively slow coronal mass ejection. The latter has been developed for several hours before the onset of the event. Through analyzing about 1.5 × 10 6 of heliograms (3700 temporal frames with 4096 images in each frame that correspond to the number of frequency channels) the radio burst source imaging shows a fascinating dynamical evolution. Both space-based (GOES, SDO, SOHO, STEREO) data and various ground-based instrumentation (ORFEES, NDA, RSTO, NRH) records have been used for this study.

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“…The density structure of the corona strongly affects the propagation of CMEs (Odstrčil and Pizzo, 1999;Riley, Linker, and Mikić, 2001;Odstrčil et al, 2002;Manchester et al, 2004). The density is also important for estimates of the Alfvén Mach number and compression rate of CME-driven shocks (Reames, 1999;Sokolov et al, 2004;Manchester et al, 2005), and for the interpretation of solar radio emission such as type II and type IV radio bursts produced by coronal eruptions (Caroubalos et al, 2004;Cho et al, 2007;Shen et al, 2013;Ramesh et al, 2013;Zucca et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

Validation of Spherically Symmetric Inversion by Use of a Tomographically Reconstructed Three-Dimensional Electron Density of the Solar Corona

Wang¹,

Davila²

2014

Sol Phys

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Determination of the coronal electron density by the inversion of white-light polarized brightness (pB) measurements by coronagraphs is a classic problem in solar physics. An inversion technique based on the spherically symmetric geometry (Spherically Symmetric Inversion, SSI) was developed in the 1950s, and has been widely applied to interpret various observations. However, to date there is no study about uncertainty estimation of this method. In this study we present the detailed assessment of this method using a three-dimensional (3D) electron density in the corona from 1.5 to 4 R ⊙ as a model, which is reconstructed by tomography method from STEREO/COR1 observations during solar minimum in February 2008 (Carrington rotation, CR 2066). We first show in theory and observation that the spherically symmetric polynomial approximation (SSPA) method and the Van de Hulst inversion technique are equivalent. Then we assess the SSPA method using synthesized pB images from the 3D density model, and find that the SSPA density values are close to the model inputs for the streamer core near the plane of the sky (POS) with differences generally less than a factor of two or so; the former has the lower peak but more spread in both longitudinal and latitudinal directions than the latter. We estimate that the SSPA method may resolve the coronal density structure near the POS with angular resolution in longitude of about 50• . Our results confirm the suggestion that the SSI method is applicable to the solar minimum streamer (belt) as stated in some previous studies. In addition, we demonstrate that the SSPA method can be used to reconstruct the 3D coronal density, roughly in agreement with that by tomography for a period of low solar activity (CR 2066). We suggest that the SSI method is complementary to the 3D tomographic technique in some cases, given that the development of the latter is still an ongoing research effort.

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Low-Frequency Observations of Drifting, Non-Thermal Continuum Radio Emission Associated With the Solar Coronal Mass Ejections

Cited by 21 publications

References 55 publications

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

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

A Decameter Stationary Type Iv Burst in Imaging Observations on 2014 September 6

Validation of Spherically Symmetric Inversion by Use of a Tomographically Reconstructed Three-Dimensional Electron Density of the Solar Corona

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