# On the Source Position and Duration of a Solar Type III Radio Burst Observed by LOFAR by P. Zhang et al.*

Type III radio bursts are generated by non-thermal electron beams propagating through the solar corona and interplanetary space. In dynamic spectra, the flux of solar type III radio bursts have a time profile of rising and decay phases at a given frequency, which has been actively studied since the 1970s. There are several factors that may contribute to the observed duration of a type III radio burst: 1) The velocity dispersion of the electron beam exciter; 2) The fluctuation of background electron density (Roelof & Pick, 1989); 3) The propagation effect due to wave scattering and refraction; 4) The intrinsic emission process of the radio wave. However, which one is the dominant factor is still an open question.

#### Observation

The LOw-Frequency Array (LOFAR) is an advanced radio antenna array with the capability of producing dynamic spectra and radio images at the same time with high resolution (van Haarlem et al., 2013). Figure 1(a) shows the dynamic spectrum of a type III radio burst observed by LOFAR at 11:51 UT on 2015 May 6. It is a single and clear burst with a duration of about 3 second and associated with a small limb flare.

With LOFAR beam-formed mode, we can obtain the source position at different times and frequency channels within the Type III radio burst (Kontar et al., 2017). The centroid source positions of the front edge, the peak, and the tail edge in the dynamic spectrum are shown in Figure 1(b). It is found that the source positions of the front edge, the peak, and the tail edge split with each other spatially. This may indicate that they are generated by electron beams moving in different magnetic ﬂux tubes in the corona. The radial speed of the electrons exciting the front edge, the peak, and the tail edge is 0.42 c, 0.25 c, and 0.16 c, respectively.

Figure 1 – The dynamic spectrum of the type III radio burst and the source position of its front edge, the peak, and the tail edge. The red, green, and black colours represent the front edge, the peak, and the tail edge of the burst, respectively.

#### Results

The contribution of the electron velocity difference to the observed duration can be estimated by statistical survey of the arrival time of the sources at a given height. The level of the coronal density ﬂuctuation at a given height can be measured by a statistically survey of the wave frequency distribution of the sources observed at the same height, so that contribution of the corona density ﬂuctuation to the duration can be estimated (Roelof & Pick, 1989). The results are shown in Table 1. And fortunately, the wave propagation effect can be evaluated by comparison with a few shorter-term bursts from the same region, which took place just at about 50 seconds before the type III burst.

Table 1. The durations of the Type III Burst Observed by LOFAR at a given frequency (Observation at Multiple Frequencies between 34 and 38 MHz are Presented), and the contributions from electron velocity difference and coronal density fluctuation

 $R$(arcsec) $\bar{f}(MHz)$ $\delta N_e/N_e$ $\Delta t_{\delta N_e}$(s) $\Delta t_{\delta v}$(s) $\Delta t_{obs}$(s) 1695 ± 2 38.51 ± 0.07 0.067 0.44 2.21 2.52 1710 ± 2 37.96 ± 0.12 0.071 0.48 2.55 2.52 1725 ± 2 37.03 ± 0.15 0.076 0.52 2.62 2.73 1740 ± 2 36.17 ± 0.13 0.110 0.77 3.68 2.78 1755 ± 2 34.98 ± 0.10 0.195 1.39 3.20 3.09 1770 ± 2 34.01 ± 0.09 0.177 1.29 3.81 3.46

Note: The first and second columns are the source height for surveying and the average frequency of waves observed at the corresponding height. The third column is the density fluctuation level measured at the height. The fourth and fifth columns are the duration contributions from the density fluctuation and the electron velocity difference, respectively. The sixth column is the observed duration in the frequency channel with the frequency in column 2.

The analysis yields that, in the frequency range of 30–41 MHz, the electron velocity dispersion is the dominant factor that determines the time duration of type III radio bursts with long duration, while scattering may play an important role in the duration of short bursts.

Based on recent paper by Peijin Zhang (张沛锦), Sijie Yu (余思捷), Eduard P. Kontar, and ChuanBing Wang (王传兵) “On the Source Position and Duration of a Solar Type III Radio Burst Observed by LOFAR”, ApJ, 885, 140 (2019) DOI: 10.3847/1538-4357/ab458f

#### References

van Haarlem, M. P. et al., A&A, 556, A2 (2013)

Kontar, E. P. et al., Nature Commun, 8, 1515 (2017)

Roelof, E. C.; Pick, M.,  A&A, 210, 417 (1989)

*Full list of authors: Peijin Zhang (张沛锦), Sijie Yu (余思捷), Eduard P. Kontar, and ChuanBing Wang (王传兵)