Solar observation with the Fourier transform spectrometer I : Preliminary results of the visible and near-infrared solar spectrum

The Fourier transform spectrometer (FTS) is a core instrument for solar observation with high spectral resolution, especially in the infrared. The Infrared System for the Accurate Measurement of Solar Magnetic Field (AIMS), working at 10–13 μm, will use an FTS to observe the solar spectrum. The Bruker IFS-125HR, which meets the spectral resolution requirement of AIMS but simply equips with a point source detector, is employed to carry out preliminary experiment for AIMS. A sun-light feeding experimental system is further developed. Several experiments are taken with them during 2018 and 2019 to observe the solar spectrum in the visible and near infrared wavelength, respectively. We also proposed an inversion method to retrieve the solar spectrum from the observed interferogram and compared it with the standard solar spectrum atlas. Although there is a wavelength limitation due to the present sun-light feeding system, the results in the wavelength band from 0.45–1.0 μm and 1.0–2.2 μm show a good consistency with the solar spectrum atlas, indicating the validity of our observing configuration, the data analysis method and the potential to work in longer wavelength. The work provided valuable experience for the AIMS not only for the operation of an FTS but also for the development of its scientific data processing software.

Statistical Analysis of Radio Frequency Interference (RFI) Caused by Solar Radiation During Wet and Dry

This paper describes a effect of solar radiation and radio signal within ultra-high frequency (UHF), which statistically deduced using Spearman correlation method. The observation was done in several location including Balai Cerap KUSZA (BCK) during dry and wet season. Solar radiation one of meteoparameters that measured simultaneously using a weather station. This data was analysed and compared to power level (radio signal) in dBm during wet and dry seasons. Findings show that telecommunication services occupy the UHF band. Hence, it can be concluded that, there are still some frequencies available for radio astronomical sources including that below 400 MHz. This allocation is suitable for solar observation, Jupiter observation, continuum observation, solar wind observation, as well as pulsar and deuterium observation and VLBI application. Statistical analysis indicate that solar radiation was significantly prominent during peaks of 382.5 MHz, 1800.0 MHz and 2160.0 MHz. It is largely related with a correlation of 0.6252, 0.6769, 0.5965 during the wet season and only small and moderate correlation at all peaks during the dry season. This important information could be a significant contribution for radio astronomers when trying to identify the best allocation for observing radio astronomical sources in the future.

Measurement of Solar Absolute Brightness Temperature Using a Ground-Based Multichannel Microwave Radiometer

Ground-based multichannel microwave radiometers (GMRs) can observe the atmospheric microwave radiation brightness temperature at K-bands and V-bands and provide atmospheric temperature and humidity profiles with a relatively high temporal resolution. Currently, microwave radiometers are operated in many countries to observe the atmospheric temperature and humidity profiles. However, a theoretical analysis showed that a radiometer can be used to observe solar radiation. In this work, we improved the control algorithm and software of the antenna servo control system of the GMR so that it could track and observe the sun and we use this upgraded GMR to observe solar microwave radiation. During the observation, the GMR accurately tracked the sun and responded to the variation in solar radiation. Furthermore, we studied the feasibility for application of the GMR to measure the absolute brightness temperature (TB) of the sun. The results from the solar observation data at 22.235, 26.235, and 30.000 GHz showed that the GMR could accurately measure the TB of the sun. The derived solar TB measurements were 9950 ± 334, 10,351 ± 370, and 9217 ± 375 K at three frequencies. In a comparison with previous studies, we obtained average percentage deviations of 9.1%, 5.3%, and 4.5% at 22.235, 26.235, and 30.0 GHz, respectively. The results demonstrated that the TB of the sun retrieved from the GMR agreed well with the previous results in the literature. In addition, we also found that the GMR responded to the variation in sunspots and a positive relationship existed between the solar TB and the sunspot number. According to these results, it was demonstrated that the solar observation technique can broaden the field usage of GMR.

Feasibility for Operationally Monitoring Ground-Based Multichannel Microwave Radiometer by Using Solar Observations

Ground-based multichannel microwave radiometers can observe the atmospheric microwave radiation brightness temperature and continuously provide temperature and humidity profiles of the troposphere. At present, microwave radiometers are operated in many countries for monitoring climate and meteorological phenomena, and there have been many microwave radiometers of this kind presently implemented in China, but they lack a unified monitor for their operational condition, which is necessary if they are taken as a network. For this reason, a real-time monitoring receiving system of radiometer is fundamental and important. In order to check the system stability and the antenna performances, this paper studied the feasibility of applying the solar signals to monitor the antenna alignment, antenna pattern and stability of a radiometer system in working for operational field applications. An experiment was performed and the results from the analysis of the annual variation features with long-term solar observation data at four frequencies, 22.235, 26.235, 30.000 and 51.250 GHz, show that an antenna pattern retrieved from solar observations agrees well with that retrieved from the traditional method. In addition, a daily analysis of the solar signals in online data of a radiometer can be used for monitoring the alignment of the antenna and the stability of the ground-based microwave radiometer system.

Operational solar flare prediction model using Deep Flare Net

We developed an operational solar flare prediction model using deep neural networks, named Deep Flare Net (DeFN). DeFN can issue probabilistic forecasts of solar flares in two categories, such as ≥ M-class and < M-class events or ≥ C-class and < C-class events, occurring in the next 24 h after observations and the maximum class of flares occurring in the next 24 h. DeFN is set to run every 6 h and has been operated since January 2019. The input database of solar observation images taken by the Solar Dynamic Observatory (SDO) is downloaded from the data archive operated by the Joint Science Operations Center (JSOC) of Stanford University. Active regions are automatically detected from magnetograms, and 79 features are extracted from each region nearly in real time using multiwavelength observation data. Flare labels are attached to the feature database, and then, the database is standardized and input into DeFN for prediction. DeFN was pretrained using the datasets obtained from 2010 to 2015. The model was evaluated with the skill score of the true skill statistics (TSS) and achieved predictions with TSS = 0.80 for ≥ M-class flares and TSS = 0.63 for ≥ C-class flares. For comparison, we evaluated the operationally forecast results from January 2019 to June 2020. We found that operational DeFN forecasts achieved TSS = 0.70 (0.84) for ≥ C-class flares with the probability threshold of 50 (40)%, although there were very few M-class flares during this period and we should continue monitoring the results for a longer time. Here, we adopted a chronological split to divide the database into two for training and testing. The chronological split appears suitable for evaluating operational models. Furthermore, we proposed the use of time-series cross-validation. The procedure achieved TSS = 0.70 for ≥ M-class flares and 0.59 for ≥ C-class flares using the datasets obtained from 2010 to 2017. Finally, we discuss the standard evaluation methods for operational forecasting models, such as the preparation of observation, training, and testing datasets, and the selection of verification metrics.

Ground-based Multichannel Microwave Radiometer Antenna Pattern Measurement using Solar Observations

Ground-based multichannel microwave radiometers (MWRs) can provide continuous temperature and humidity profiles of the troposphere. MWR antenna pattern measurements are important for reliable and accurate antenna temperature measurement and are usually carried out in a microwave anechoic chamber. Measurement using an anechoic chamber is complex and expensive because the conventional measurement procedure requires a special situation and professional instruments. More importantly, the construction of the anechoic chamber and the installation method of the absorbing material can directly influence the performance of the anechoic chamber and the result of the antenna measurement. This paper proposes a new method of MWR antenna measurement by observing the sun, and this method can be used to measure other radar antenna patterns. During the measurement, the MWR observes the microwave radiation brightness temperature (TB) to measure the antenna pattern by high-resolution raster scanning of the azimuth and elevation of the sun under a clear sky in Xi'an, China. Analysis of the TB scanning data of the sun at four frequencies, 22.235, 26.235, 30.000 and 51.250 GHz, showed that the microwave radiation TB of the sun is strong enough to be observed by the MWR. Furthermore, the antenna pattern was illustrated and analyzed based on these data, which fully proves that the sun can be used to measure the antenna pattern. Finally, the antenna pattern derived from the solar observation was compared with the result of the far-field measurement with a point source in the microwave anechoic chamber at 30 GHz, the maximum error of the beamwidth is less than 0.1°, which showed that this pattern matched well to the pattern measurement using a point source in the microwave anechoic chamber. Therefore, the antenna pattern of the MWR can be measured by scanning the sun without a point source in the microwave anechoic chamber, and this method can be used for convenient MWR antenna measurements and can reduce the measurement complexity and cost.