Solar Type Research Articles

The Solar Origin of an In Situ Type III Radio Burst Event

Solar type III radio bursts are generated by beams of energetic electrons that travel along open magnetic field lines through the corona and into interplanetary space. However, understanding the source of these electrons and how they escape into interplanetary space remains an outstanding topic. Here we report multi-instrument, multiperspective observations of an interplanetary type III radio burst event shortly after the second perihelion of the Parker Solar Probe (PSP). This event was associated with a solar jet that produced an impulsive microwave burst event recorded by the Expanded Owens Valley Solar Array. The type III burst event also coincided with the detection of enhanced in situ energetic electrons recorded by both PSP at 0.37 au and WIND at 1 au, which were located very closely on the Parker spiral longitudinally. The close timing association and magnetic connectivity suggest that the in situ energetic electrons originated from the jet’s magnetic reconnection region. Intriguingly, microwave imaging spectroscopy results suggest that the escaping energetic electrons were injected into a large opening angle of about 90°, which is at least nine times broader than the apparent width of the jet spire. Our findings provide an interpretation for the previously reported, longitudinally broad spatial distribution of flare locations associated with prompt energetic electron events and have important implications for understanding the origin and distribution of energetic electrons in interplanetary space.

Morphology of Solar Type II Bursts Caused by Shock Propagation through Turbulent and Inhomogeneous Coronal Plasma

Type II solar bursts are radio signatures of shock waves in the solar corona driven by solar flares or coronal mass ejections (CMEs). Therefore, these bursts present complex spectral morphologies in solar dynamic spectra. Here, we report meter–decameter radio observations of a type II burst on 2014 July 25 made with the Ukrainian radio telescopes UTR-2 (8.25–33 MHz) and GURT (8.25–78 MHz). The burst demonstrates fundamental and harmonic components, band splitting, a herringbone structure, and a spectral break. These specific spectral features, observed jointly in a single type II burst, are rarely detected. To contribute to our understanding of such puzzling type II events, we carried out a detailed analysis of the recorded type II dynamic spectrum. In particular, the herringbone pattern has been exploited to study electron density turbulence in the solar corona. We calculated the power spectral densities of the flux variations in selected herringbones. The spectral index is in the range of α = −1.69 to −2.00 with an average value of −1.897, which is slightly higher than the Kolmogorov spectral index of −5/3 for fully developed turbulence. We also recognized that the second type II burst consists of three drifting lanes. The lane onset times coincide with the spectral break in the first type II burst. We regard that the CME/shock passage through a streamer caused the spectral break and triggered the multilane type II radio emission. Thus, we support one of the proposed scenarios for type II burst occurrence as being the result of CME/shock–streamer interaction.

The Activity of a Solar-Type Star TOI-1422 and Mass Loss of the Atmosphere of the Planet TOI-1422b

The results of the analysis of the activity of a solar type star G2V TOI-1422 are presented and estimates of the loss of atmospheric matter of the planet TOI-1422b are made. The planet can be attributed to the type of hot Neptunes. Compared to other exoplanets of a similar mass range, it is expected that the planet has an extensive gas envelope. According to the long-term photometric survey of Kamogata Wide-field Survey (KWS) the TOI-1422 activity was analyzed and the existence of possible activity cycles of 1650–1680 days and 2450 days was suggested. The probable value of the rotation period P of the star lies in the range of 27 (+19, –8) days, observations of the KWS survey in the V filter indicate the most possible value for the period P = 32 days. Mass loss of the planet’s atmosphere is determined using an approximation formula corresponding to the model of atmospheric loss with an energy restriction. To estimate the flux of XUV photons analytical dependences were used linking the flux values and the parameter log R_{{{text{HK}}}}^{'}. Calculations have shown that the atmosphere matter loss of TOI-1422b is dot {M} = 9.4 times {{10}^{8}} g/s; considering the existing errors in determining the parameters of the atmosphere it lies in the range from 6.8 times {{10}^{8}} to 1.4 times {{10}^{9}} g/s, and considering the uncertainty in the value of the chromospheric activity index—from 8.3 times {{10}^{8}} to 1.1 times {{10}^{9}} g/s.

THE ACTIVITY OF A SOLAR-TYPE STAR TOI-1422 AND MASS LOSS OF THE ATMOSPHERE OF THE PLANET TOI-1422b

The results of the analysis of the activity of a solar type star G2V TOI-1422 are presented and estimates of the loss of atmospheric matter of the planet TOI-1422b are made. The planet can be attributed to the type of hot neptunes. Compared to other exoplanets of a similar mass range it is expected that the planet has an extensive gas envelope. According to the long-term photometric survey of Kamogata Wide-field Survey (KWS) the TOI-1422 activity was analyzed and the existence of possible activity cycles of 1650-1680 days and 2450 days was suggested. The probable value of the rotation period P of the star lies in the range of 27 (+19, –8) days, observations of the KWS survey in the V filter indicate the most possible value for P = 32 days. Mass loss of the planet’s atmosphere is determined using an approximation formula corresponding to the model of atmospheric loss with an energy restriction. To estimate the flux of XUV photons analytical dependences were used linking the flux values and the parameter \(\log R_{{{\text{HK}}}}^{'}\). Calculations have shown that the mass loss of TOI-1422b is \(\dot {M} = 9.4 \times \) 108 g/s and taking into account the existing errors in determining the parameters of the atmosphere it lies in the range from 6.8 × 108 g/s to 1.4 × 109 g/s.

Investigating noble gases and nitrogen in Zag (H3-6) and ALH 77216 (L3.7–3.9): The ordinary chondrites with solar type neon and argon

Concentrations and isotopic compositions of noble gases (He, Ne, Ar, Kr, and Xe) and nitrogen in two ordinary chondrites (OCs), Zag (H3-6) and ALH 77216 (L3.7–3.9), are presented. The aim of the study is to examine the cosmic ray exposure history, radiogenic ages and isotopic signatures of trapped gases in them. The results of stepwise heating analyses indicate that light noble gases (He and Ne) are mixture of trapped and cosmic ray produced components. Neon isotopes are enriched from solar wind (SW), while shows a trend towards galactic cosmic ray (GCR) region in both the meteorites. Phase-Q neon is not observed in any of the meteorite. The heavy noble gases Ar, Kr and Xe indicate mixture of Q-HL-SW and cosmogenic. Elemental ratios of trapped 36Ar, 84Kr and 132Xe indicate that noble gases in Zag and ALH 77216 are mixtures of the three components Q, HL and SW. The cosmic-ray exposure (CRE) ages calculated from neon for Zag and ALH 77216 are 5.6 ± 0.3 Ma and 28.5 ± 0.4 Ma, respectively. These ages are within the range typically observed for the respective meteorite types of OCs. Nitrogen isotopes indicate presence of multiple components in both the chondrites. Isotopic signature of trapped nitrogen in both the chondrites is distinct from that of SW, Q and HL, indicating additional source of nitrogen in the meteorites.

Performance Test of Solar Power Plant as a Source of Electricity in Mini Greenhouse

The potential of solar energy in an area is very dependent on the position between the sun and the position of the region on the earth’s surface. Greenhouse is house plant with environment plant that can controlled through devices electronics. The power electricity is needed for lights, water pumps, and another electronic component. This study aims to test the performance of solar panels as a source of electricity in a mini greenhouse and to determine how long it takes to charge the battery. This research was conducted at the Laboratory of Agricultural Equipment and Machinery Production Management, Faculty of Agricultural Technology, Andalas University. The result of this result is system mini greenhouse that consist of 2 solar panels type monocrystalline 100 Wp, Solar Charge Controller MPPT type, Inverter, Accu VRLA, cable, switch. Power generation results Sun this produce 2 outputs or output, i.e. tension and strength current. Tension and strong generated current fluctuate. This thing caused no stable intensity the sun at the moment testing field done. From use burden lamp of 20 watts obtained voltage Accu starting 12.87 V. From testing charging Accu who have conducted needed 8 hours for charging with voltage 13V.

Design, optimization and economic viability of an industrial low temperature hot water production system in Algeria: A case study

Solar energy has a great potential in many areas of industrial activity in Algeria. This is because most of Algeria has high levels of sustainable solar insulation. Unfortunately, few industries use solar energy for hot water generation, but some industrial processes require hot water at temperatures that can be easily obtained from solar thermal panels. This paper presents a case study to investigate the technical and financial feasibility of a solar-powered industrial agro-processing system in Algiers. Based on the solar collectors connection type for which the economic feasibility study was carried out, an appropriate design of the system was determined. The latter was actually done by analyzing the levelized cost of energy savings. The design of the thermo-solar process is carried out based on F-chart method with a new approach by integrating the incidence angle modifier and of using real and experimental data requirements to determine realistic achievable performance of the solar process. The results showed that, in comparison to the currently used electrical system, the electrical energy savings achieved by the solar-powered system make it an economically viable option with a solar coverage rate of 80%. The investment depreciation balance shows that the use of such a thermal solar energy system will be more competitive than fossil fuels system if the price of electricity in the country increases from 0.048 to 0.075 €/kWh.

Statistical study of type III bursts and associated HXR emissions

Context. Flare-accelerated electrons may produce closely temporarily related hard X-ray (HXR) emission while interacting with the dense solar atmosphere and radio type III bursts when propagating from the low corona to the interplanetary medium. The link between these emissions has been studied in previous studies. We present here new results on the correlation between the number and spectrum of HXR-producing electrons and the type III characteristics (flux, starting frequency). Aims. The aim of this study is to extend the results from previous statistical studies of radio type III bursts and associated HXR emissions: in particular, to determine what kind of correlation, if any, exists between the HXR-emitting electron numbers and the radio flux, as well as whether any correlations between the electron numbers or energy spectra are deduced from associated HXR emissions and type III starting (stopping) frequencies. Methods. This study is based on thirteen years of data between 2002 and 2014. We shortlisted ≃200 events with a close temporal association between HXR emissions and radio type III bursts in the 450–150 MHz range. We used X-ray flare observations from RHESSI and Fermi/GBM to calculate the number of electrons giving rise to the observed X-ray flux and observations from the Nançay Radioheliograph to calculate the peak radio flux at different frequencies in the 450–150 MHz range. Under the assumption of thick-target emissions, the number of HXR-producing electrons and their energy spectra were computed. The correlation between electron numbers, power-law indices, and the peak radio fluxes at different frequencies were analysed as well as potential correlations between the electron numbers and starting frequency of the radio burst. Bootstrap analysis for the correlation coefficients was performed to quantify the statistical significance of the fit. Results. The correlation between the number of HXR electrons and the peak flux of the type III emission decreases with increasing frequency. This correlation is larger when considering the electron number above 20 keV rather than the electron number above 10 keV. A weak anti-correlation is also found between the absolute value of the electron spectral index and the peak radio flux at 228 MHz. A rough correlation is found between the HXR-producing electron number above 20 keV and the type III starting frequency. This correlation is smaller if the electron number above 10 keV is considered. All the results are discussed in the framework of results from previous studies and in the context of numerical simulations of bump-in-tail instabilities and subsequent radio emissions.

The influence of coconut endosperm composition based on the maturity levels against the quality of pliek-u

Pliek-u is Acehnese’s food heritage that has potential as functional food due to its high protein and lactic acid contents. The study aimed to investigate the effect of coconut endosperm composition based on the maturity levels against the quality of pliek-u. Two levels of Tall Coconut maturities used i.e., over mature (u-riek) and mature (u-pateun). About 2kg of grated coconut endosperm was fermented in a plastic box for 7 days at 3 compositions i.e., 30% over mature and 70% mature (P1), 50% over mature and 50% mature (P2), and 70% over mature and 30% mature (P3). Each treatment had been conducted in 3 replications. Then, the coconut was dried by using solar tunnel dryer type Hohenheim Aceh for 2 days. To produce pliek-u, soon after the drying process, the warm coconut was pressed by using a hydraulic press. The parameters observed to evaluate the quality of pliek-u were moisture, fat, protein, and acidity. The consumer preferences were evaluated from 30 panellists on 4 criteria i.e., aroma, color, texture and taste by using hedonic scale from 1 to 5. Results showed that the composition of coconut endosperm at different maturity levels had influenced the quality of pliek-u significantly. The best moisture was obtained from pliek-u produced by treatment P2, while the lowest fat content, the highest protein content and the most acid taste were identified from pliek-u produced by treatment P3. However, according to consumer’s preferences, the best overall acceptance was pliek-u produced by treatment P1 and P2 at score 4.2 (like). Therefore, this study recommended the best composition of coconut endosperm in pliek-u processing at 50% over mature and 50% mature (P2).

Properties of Flare Events on M Stars from LAMOST Spectral Survey Based on Kepler and TESS Light Curves

A catalog of M stars has been published from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope data release 7 (LAMOST DR7). We cross-matched the LAMOST M catalog with Kepler, Kepler 2 (K2) and Transiting Exoplanet Survey Satellite (TESS) surveys. We obtained the light curves from the Kepler and TESS surveys. We detected 20,047 flare events from 4053 M stars and calculated their durations, amplitudes, and energies. We analyzed the distribution of the flare durations and energies. The distributions of flare duration for Kepler, K2 and TESS peak are at 3–3.5 hr, 4–6 hr and 1–1.5 hr, respectively. This may be the result of the different cadences for the three data sets. The highest regions of the flare energies of Kepler, K2 and TESS are 32–32.5, 32–32.5 and 31–31.5 erg in Log format, respectively. A linear relationship between flare duration and energy emerges from our analysis. The ratio of flare duration to total observational time is approximately 0.2%–0.3% for the Kepler, K2 and TESS surveys. The occurrence rate of a star with a flare event increases from the M0 to M4 subtypes. We also determined the spatial distribution of the flare rate of M stars in the Milky Way. It seems that the flare rate decreases as the vertical height increases. The power index of the flare energies is in the region of 1.53–2.32, which is similar to previous result for solar type star (2.0). Further, we examined the relationship between the flare amplitude and chromospheric intensity. The flare activity increases rapidly with the increase in the Hα EW at the lower values (less approximately 2 Å) and it increases slowly at the higher values.

An experimental case study on development the design and the performance of indirect solar dryer type for drying bananas

Due to the shortages of fossil fuels and higher prices, as well as to reduce the causes of climate change and the fuel consumption utilized in the drying procedure, more emphasis is placed on resources of solar energy, due to it is easily accessible. For these aims, the indirect solar dryer thermal performance for drying of the banana samples was experimentally investigated. Two indirect solar dryers; chimney-type and fan-type, consisting of the collector and dryer sections, were designed and fabricated. The lowest value of the banana piece moisture content was obtained in the case of the chimney-type as 10.59 %, which shows 81 % improvement in the drying procedure in comparison with the open sun solar dryer. In addition, the average collector thermal efficiencies obtained for the chimney and fan were 34.14 % and 29.54 %, respectively; thus, using the chimney with a solar collector offers the best thermal efficiency. Moreover, the average dryer thermal efficiencies obtained for the chimney and fan were 14.45 % and 12.76 %, respectively. Therefore, the experimental results illustrate that the chimney-type solar dryer performs better than the fan-type and open sun solar dryers.

SOLAR PHOTOVOLTAIC DAN PENERAPANNYA MENJADI POWER BANK 10000 MAH

Consumers of mobile devices expect manufacturers to produce devices that will be an efficient source of electrical energy. The battery currently used in the smartphone allows the device to operate for several hours. PowerBank extends the operating time of the device without the need to charge it through a charger that is connected to the mains and the most important feature that determines the quality of a power bank is its capacity. This paper first analyzes the effect of the number of solar cells on the application of a 10000 mAh PowerBank. It has been shown in this study that the capacity of the 10000 mAh PowerBank can charge a series of 2, 4, and 8 solar cells. What has also been investigated is Then testing it for several types of mobile devices. The results show that using a 2, 4, and 8 solar cell circuit type can only charge handheld cell phones with a battery capacity of 2000 mAh.

Solar Radio Spikes and Type IIIb Striae Manifestations of Subsecond Electron Acceleration Triggered by a Coronal Mass Ejection

Understanding electron acceleration associated with magnetic energy release at subsecond scales presents major challenges in solar physics. Solar radio spikes observed as subsecond, narrow-bandwidth bursts with Δf/f ∼ 10−3–10−2 are indicative of a subsecond evolution of the electron distribution. We present a statistical analysis of frequency- and time-resolved imaging of individual spikes and Type IIIb striae associated with a coronal mass ejection (CME). LOFAR imaging reveals that the cotemporal (<2 s) spike and striae intensity contours almost completely overlap. On average, both burst types have a similar source size with a fast expansion at millisecond scales. The radio source centroid velocities are often superluminal and independent of frequency over 30–45 MHz. The CME perturbs the field geometry, leading to increased spike emission likely due to frequent magnetic reconnection. As the field restores itself toward the prior configuration, the observed sky-plane emission locations drift to increased heights over tens of minutes. Combined with previous observations above 1 GHz, the average decay time and source size estimates follow a ∼1/f dependence over three decades in frequency, similar to radio-wave scattering predictions. Both time and spatial characteristics of the bursts between 30 and 70 MHz are consistent with radio-wave scattering with a strong anisotropy of the density fluctuation spectrum. Consequently, the site of the radio-wave emission does not correspond to the observed burst locations and implies acceleration and emission near the CME flank. The bandwidths suggest intrinsic emission source sizes <1″ at 30 MHz and magnetic field strengths a factor of two larger than average in events that produce decameter spikes.

Off-Grid Photovoltaic System for a Villa at AVRO City in Duhok

The off-grid solar photovoltaic system is one of the promising technologies for generating friendly electricity. Duhok city suffers from energy shortages in that electricity comes from local generators to support national grid. The aim of the research is to eliminate local generators due to their high costs and noise levels. A photovoltaic (PV) solar system type (off-grid) was proposed for one villa in AVRO city Duhok. A calculation has been done to select size of the system and A PV Syst software was adopted to investigate the design of the proposed system and additionally examined the economic analysis as well as the net profit. The proposed system is used with an average electricity demand of 12.9 kW/day. A typical 3.3 kW PV system was determined to be able to meet the daily power requirements of an entire villa with 8 panels: two in series and four in parallel where each panel has a rating of 415W. The system includes 8 batteries of 12 V,200Ah, and a 5-kW inverter with MPPT tracker. The result shows that yearly average of the energy requirement of villa is 4728.9 kWh and energy available through Solar’s panel is 5999 kWh/year

Panel Segmentation: A Python Package for Automated Solar Array Metadata Extraction Using Satellite Imagery

The National Renewable Energy Laboratory (NREL) Python panel-segmentation package is a toolkit that automates the process of extracting accurate and valuable metadata related to solar array installations, using publicly available Google Maps satellite imagery. Previously published work includes automated azimuth estimation for individual solar installations in satellite images [1]. Our continued research focuses on automated detection and classification of solar installation mounting configuration (tracking or fixed-tilt; rooftop, ground, or carport). Specifically, a faster-region-based convolutional neural network Resnet-50 feature pyramid network model was trained and validated on 862 manually labeled satellite images. This model was used to perform object detection on satellite imagery, locating and classifying individual solar installations' mounting configuration and type. Model results showed a mean average precision score of 77.79%, with the model strongest at detecting fixed-tilt ground mount and fixed-tilt carport installations. The object detection model and its outputs have been incorporated into the panel-segmentation package's automated metadata extraction pipeline, which returns the mounting configuration and azimuth for individual solar arrays in satellite imagery [2]. The complete image dataset with labels has been released on the U.S. Department of Energy (DOE) DuraMAT DataHub, to encourage further research in this area [3].

Solar Coronal Density Turbulence and Magnetic Field Strength at the Source Regions of Two Successive Metric Type II Radio Bursts

We report spectral and polarimeter observations of two weak, low-frequency (≈85–60 MHz) solar coronal type II radio bursts that occurred on 2020 May 29 within a time interval ≈2 minutes. The bursts had fine structures, and were due to harmonic plasma emission. Our analysis indicates that the magnetohydrodynamic shocks responsible for the first and second type II bursts were generated by the leading edge (LE) of an extreme-ultraviolet flux rope/coronal mass ejection (CME) and interaction of its flank with a neighboring coronal structure, respectively. The CME deflected from the radial direction by ≈25° during propagation in the near-Sun corona. The estimated power spectral density and magnetic field strength (B) near the location of the first burst at heliocentric distance r ≈ 1.35 R ⊙ are ≈2 × 10−3 W2m and ≈1.8 G, respectively. The corresponding values for the second burst at the same r are ≈10−3 W2m and ≈0.9 G. The significant spatial scales of the coronal turbulence at the location of the two type II bursts are ≈62–1 Mm. Our conclusions from the present work are that the turbulence and magnetic field strength in the coronal region near the CME LE are higher compared to the corresponding values close to its flank. The derived estimates of the two parameters correspond to the same r for both the CME LE and its flank, with a delay of ≈2 minutes for the latter.

МАГНІТО-АКТИВНІ ДОВГОТИ НА СОНЦІ І ЗОРЯХ

An overview of studies of long-term increased magnetic activity in two discrete longitudinal intervals observed on the Sun and on the surface of stars of certain types is reviewed. Active longitudes on the Sun were first discovered at the end of the 19th century. Today, as a result of statistical analysis of data observed for more than a century, it has been established that there are two active longitudinal sectors on the solar surface, shifted by approximately 180° relative to each other, which can stably maintain the phase coherence of activity for a long time. At each given moment of time, one of the two longitude intervals are more active (dominant). The occasionally observed “flip-flop” phenomenon, the essence of which consists in a sudden rapid switching of the specified dominance between two active longitudes, is highlighted. The detected phenomenon is regularly repeated, which indicates the existence of stellar magnetic flip-flop cycles. At the same time, solar-type cycles are also characteristic of young analogues of the Sun. On the other hand, based on the study of the evolution of the spot area, a magnetic flip-flop cycle with a duration of about 3.7 years was also detected on the Sun. It is relevant that the ratio of the periods of both types of cycles for young dwarfs and the Sun is the same: the flip-flop cycle is approximately 3–4 times shorter than the cycle of the solar type. That is, the structure and evolution of active longitudes on the Sun is similar to the observed active longitudes on the surface of cold stars that rotate quickly and have outer convective shells. Mechanisms of excitation of magnetically active longitudes proposed by the researchers were analyzed. Dynamo-excitation models of axially asymmetric magnetic harmonics look promising. Our calculations showed that the αΩ-dynamo models with the involvement of helioseismological data on the internal rotation of the Sun ensure the coexistence of dipole and quadrupole harmonics of the global magnetic field, which are necessary for the reproduction of selected longitudinal sectors of increased magnetic activity.

Breakdown of planetary systems in embedded clusters

ABSTRACT We report the first simulations of planetary system dynamics as affected by an embedded cluster environment. Such environments are generally believed to be relevant for the large majority of newborn stars of solar type. Moreover, our cluster model is more realistic than in previous work. We focus on a giant planet system with five members, which represents a likely precursor of our solar system. Our main result is that the perturbing effects of close encounters with cluster stars trigger dynamical chaos leading to breakdown of the system with a significant probability, especially if the natal gas discs are short-lived and the clusters are highly concentrated. When breakdown occurs, all planets except Jupiter suffer a large risk of being ejected from the system or extracted into distant orbits with semimajor axes of hundreds or thousands of astronomical units. This is consistent with recent estimates of a large abundance of low-mass, free-floating planets. We demonstrate a possibility for Jupiter and Saturn to evolve into hot Jupiter orbits by tidal circularization during the chaotic evolution. Even so, the low occurrence rate of this outcome indicates that the real hot Jupiters in general have an origin unrelated to dynamical evolution in birth clusters.

Uji Performansi Alat Pengering Tipe Terowongan Hohenheim Aceh Dengan Aplikasi Proportional Integral Derivative Controller Untuk Kipas Outlet

The purpose of this study was to evaluate the performance of Hohenheim Aceh type solar tunnel dryer with the application of proportional integral derivative (PID) controller for outlet fans . The instrumentations used were solar tunnel dryer type Hohenheim Aceh, HTC-meter, anemometer, pyranometer, and other supporting equipment s . The results showed that during the drying process solar irradiation had fluctuat ed , where the average solar irradiation was 649 W/m 2 . The average temperature in the drying chamber is 40.6°C while the average temperature in the environment is 32.9°C. Conditions in the drying chamber were suitable for drying because the temperature inside the dryer was relatively higher than the ambient temperature. The average relative humidity ( RH ) in the drying chamber was 36% and the average RH in the environment was about 40% . T he relationship between temperature and RH value was negative and strong indicated bu r-value of 0.7379 . On the other hand, t he relationship between solar irradiation and temperature was positive and also strong indicating that the energy source for this dryer was from solar irradiation with an R -square of 86.02 % and r-value of 0.92747 . The application of PID controller had improved the performance of Hohenheim Aceh type solar tunnel dryer by preventing the incident of unproper drying temperature. However, the airflow in the drying chamber was too low thus the further engineering design is needed to improve the drying system.

A comparison of Solar Cycle 23rd and 24th for Solar type II radio bursts associated with coronal mass ejection in relation to interplanetary features

A comparison of Solar Cycle 23rd and 24th for Solar type II radio bursts associated with coronal mass ejection in relation to interplanetary features