An explosion of type IV radius decimetric related to the Bengal induced by the X2 radiation of the emission of electron cyclotron master by LV et al. – European astronomer radio community

Decimetric broadband radio explosions have been observed (with frequencies from hundreds of MHz to a few GHz) from the sun and other flame stars. In the solar case, such explosions have been classified as decimetric explosions of type IV (T-IVDM). Its spectra often contain substantial fine structures, such as pulsations, peaks and various absorption structures. This makes them different from their metric and centimeter counterparts.

Due to the lack of image data in decimetric wavelengths, previous studies determined the orientation of the field of origin based on the leaders of leaders of sunspots (Aschwanden 1986; Zlobec et al. 1987). This leads to contradictory conclusions about the mechanism of T-IVDM explosions. During the last eight decades of solar astronomy radio, only solar peaks that are highly transitory, highly polarized and extremely bright are widely attributed to the emission of Master of Electron Cyclotron (ECME), while several other types of consistent solar bursts, such as type-i, II and III, have been attributed to the emission of plasma.

We analyze a T-IVDM outbreak induced by the Bengal in 20110924 with medium polarization levels and sources near a sunscreen. The event was observed by NRH at several image frequencies and by SDO/AIA in EUV Pass Bands. The purpose is to identify the underlying radiation mechanism.

Figure 1: General description of the T-IVDM radio on September 24, 2011. (b) The dynamic spectra that combine the data of the San Vito Observatory (100-175 MHz), the Bleien Observatory (175-870 MHz) and the Onderejov Observatory (870-2000 MHz). Explosions I and II are two components of the T-IVDM event. (c) The temporary profiles of maximum t_B and the degree of polarization (D) with a cadence of 10 SA eight frequencies of NRH.

The event consists of two main subcurses (bursts I and II), each duration of ∼20 minutes. The observations reveal three characteristics: (1) Both explosion components are highly intermittent, with a higher and lower frequency cutting to ∼1–2 GHz and 200–300 MHz, respectively. (2) The maximum brightness temperature (T_B) is ∼2 × 10¹¹ K for explosion I and ∼4 × 10¹⁰ K for explosion II. (3) Polarization is left -handed with levels
Reach ∼70%–100%, with a general increased general trend. According to these observations, we conclude that the emission is consistent since the incoherent turning radiation of sun shoots cannot produce such intermittency with high T_B > 10¹¹ K and strong polarization at such frequencies (for example, Dulk 1985).

Figure 2: The AIA and HMI data of the event. In_B
at eight frequencies (228–445 MHz) for representative moments of explosions I and II. (d) and (h) the HMI magnetogram superimposed by extrapolated nlfff
Field lines The colored sections of the field lines correspond to the field forces that increase from ∼40.7 a ∼79.5 gy the corresponding 2 Ω_frowning Increase from 228 to 445 MHz. Colored circles show 95% contours at 13:04:17 (D) and 13:45:07 UT (H). The yellow sphere that crosses the cyan field line marks the location where
Energy electrons are injected for particle transport simulation.

NRH sources moved systematically during the explosion, exhibiting at least two jumps that indicate the beginning of explosions I and II. Around 13:00 UT, the sources moved to the region above the pounced loops, already ∼13: 20 UT, jumped towards the western leg of the loops, just above the most right sun spot with a negative polarity. Throughout the process, NRH sources aligned well each other, and the most frequency sources are closer to the album.

We draw two main conclusions: (1) NRH sources of both explosions (I and II) are found along the field lines that point to the sunny stain with a strong left -hand polarization (Figure 1 (d)), so both explosions are x, y (2) the sources align well with
The color 2 Ω_frowning section. Therefore, the most likely radiation mechanism is the harmonic mode x (x2) through ECME since the alternative process of coherent plasma emission would produce the mode or for the fundamental branch or the weak polarization for the
harmonic branch (for example, Chen et al. 2022).

In addition, we model the transport of transmission electrons down along a coronal circuit. We discover that most electrons are reflected in the convergent sunspots within the altitude range of 20-100 mm. This agrees with the well -defined spectral ranges of such explosions. Energy electrons based on ECME exhibit a speed distribution function similar to cover (VDF) instead of the alleged distribution of loss concessions generally.

This study provides essential evidence that the T-IVDM explosion induced by the Bengalia is ECME induced in harmonic mode X, and largely expands the ECME application on the solar astronomy radio and provides solar samples for similar bursts of other slapped stars.

Based on the recent article by LV M., Zhong Z., Kong X., NO, H., Yu, F., Wang B., Tan B., Victor, M., Alexey, K., Song, H., Zheng R., Chen and. ,,, A decimetric type IV radius explosion related to the Bengal induced by the X2 radiation of the emission of electron cyclotron masler, APJL, 989, L24, DOI: https://doi.org/10.3847/2041-8213/adf5c6

References

Aschwanden, M.: 1986, Soph, 104, 57

Zlobec, P., Messerotti, M., Li, H. et al.: 1987, Soph, 114, 375

Dulk, G.: 1985, ARA & A, 23, 169

Chen, Y., Zhang, Z., Ni, S., et al.: 2022, APJL, 924, L34