MM/DD 14:45--16:15 Name
Abstract
05/19 14:45--16:15 Yuki Sato
Neptune is the eighth planet of the solar system. It's mainly compoesed of hydrogen and helium. Previous study shows that storms occur at both northen and southern mid latitude. (15-60N, 15-60S) [Imke de Pater et al., 2014]. Storms rotate at a certain speed in the longitude direction. The speed of storms is correlated with the zonal winds measured by Voyager 2. On June 26 and July 2 2017, a large-scale storm (the diameter is 9,000 km) waseobserved by the Keck Observatory. Some scientists say that this is probably because of seasonal change. In this study, we developped the technique to estimate the drift rate and intensity of storms by observing a whole spectrum of Neptune. By using this technique, when seeing is bad, it's possible to observe Neptune in short time span for a long term. In this seminar, we estimated the lifetime, intensity, drift rate of storms in 2017, 2018 and 2019. We use methane absorption band in this study. Methane absorbs 890 nm flux strongly. When we observe the aspect with a storm at 890 nm, 890 nm flux becomes stronger compared to the aspect without a storm. This is because the altitude of storm is higher than that of other areas. And the appearent area of storms changes by the rotation of Neptune, so 890 nm flux changes. We calculate the theoretical value of 890 nm changing by the rotation. We take the ratio of 890 nm flux and flux of 855 nm to correct the efect of the Earth atmosphere, and fit the theoretical line with the observed values in the least squares method. In addition to estimation of drift rate and intensity, we are trying to estimate the latitude of storms. In this presentation, I'll show the results of my observation.
05/26 14:45--16:15 Shunsuke Niwa
Tropical cyclones (TCs) causes serious damage to human society every year. For reduction of its risk, TC forecast is important but prediction of TC intensity is a big problem. TCs are intensified by strong updraft and lightning is an good indicator of updraft intensity so lightning can be use to monitoring TC intensity. Previous studies suggested that lightning actvity in TC can be a predictor of TC intensity. Although relationship between lightning frequency and TC intensity have been investigated in numerous studies, relationships of electrical properties of lightning (EPs) with TC intensity have not been researched except for Atlantic. In this study, we will investigate the relationships of EPs of lightning and TCs over the Western North Pacific. We obtained best track data of TCs from Joint Typhoon Warning Center (JTWC) and lightning data from World Wide Lightning Network (WWLLN) and Two stations of Global ELF Observation Network (GEON), Syowa (69.0S, 39.5E) and Kuju(33.1N, 131.2E). The relationship between maximum sustained wind of 5 TCs over Western North Pacific and EPs such as Peak Current (Ip), Charge moment change (Qdl) and Charge amount (Q) of lightning in the inner core and rainband respectively. It is found that EPs of the inner core lightning of strong TC are correlated to TC intensity. In addition, Ip and Q of lightning in rainband of weak TCs tend to peak 1~2 days before TC intensity change.
06/02 14:45--16:15 Purwadi
During the Understanding of Lightning and Thunderstorm (ULAT ) Project and e-Asia Joint research Project, 2017 to 2019 FSY, some VLF receiver with sampling frequencies 100 µs was deployed to cover cloud to ground (CG) lightning in Asian countries such as Northwest Pacific and southeast (AVON). Moreover, VLF receiver with sampling frequencies 10 µs was deployed in the Philippines to cover lightning observation in that country (Nationwide Network). Both of VLF receiver is manufactured by Meisei Company-Japan and developed together with Hokkaido University. It can be and mostly combined with automatic weather stations (POint TEnki KAnsoku = POTEKA), so it is called V-POTEKA. During the research period, the instrument was tested and operated, showing the ability to detect the lightning phenomena in the target area. The comparison of the lightning geolocation estimate by the V-POTEKA lightning detection networks and Blitzortung shows the relative distance 35km and 37 km for the V-POTEKA with sampling frequency 10µs and 100 µs, respectively. The absolute different time of detection between both types of V-POTEKA and Blitzortung for the same lightning is estimated to be 1 second and 823µs for the V-POTEKA with sampling frequency 10µs and 100µs, respectively. The relationship between lightning and other thunderstorm cloud characteristics such as cloud top temperature (CTT), cloud top height (CTH), and precipitation has been conducted using AVON lightning data and static grid method. The result of this work is agreed with the previous work, which mentions that the total lightning is an exponential function of CTH. Using the grid 0.5ºx0.5º lightning density detected by AVON, we could draw the daily thunderstorm activities over Kalimantan and its adjacent sea. The lightning mostly occurs in the afternoon and evening along the coast island. Moreover, in the central region of Kalimantan island and the sea adjacent to the coast, the lightning mostly occurs at night and early morning over the plains. Generally, the result agrees with the diurnal rainfall pattern of TRMM precipitation standard V7. During the operation, the V-POTEKA Nationwide Network in the Philippines detects the lightning produce by Taal Volcano eruption the cloud ash on January 12th, 2020. The evolution of development Taal Volcano eruption the cloud ash is detected using Himawari 8 band 15 (12µm) and performed in 2D and 3D. Based on the news in online media, the big explosion of Taal Volcano is around 15:00LT (07:00 UTC). The cloud ash's temporal evolution shows that the maximum cloud growth speed is ~50 m/s at around 07:00 to 07:10 UTC, which is closed to the big explosion time. The first CG lightning detected by V-POTEKA Nationwide Network occurs at 07:47:25.15725 UTC. 34 CG lightning is detected by V-POTEKA Nationwide Network during the Taal Volcano eruption on January 12th, 2020. Moreover, we try to estimate the energy input of the typhoon. The lightning is assumed proportional to the energy and the wind to be the carrier of the energy. We did the back-tracing of the 60 points in radius 100 km to the typhoon eye. The speed and direction are taken from the ERA5 reanalysis at the pressure level 1000 Mb to 400Mb with spatial resolution 0.25x0.25. We calculate a new point with interval time 30 minutes with the speed and direction updated to be the closest place and data. The lightning data detected by Blitzortung is counted using the backtracking point windows with interval time 6 hours. The result of this study shows, the wind in level 900 Mb is to be the most reasonable path to carry the energy to the typhoon Trami from place with the distance-time 36 hours to 48 hours from the typhoon Trami eye. The lag time in the maximum cross-correlation value between reaching center time and increasing maximum wind speed is 6-12 hours, which is assumed to be the conversion time of energy from latent heat to the kinetics energy.
06/09 14:45--16:15 Haruki Sugiyama
Uranus is the seventh planet of the solar system, and time-varying structures such as methane clouds have been discovered by the close-range exploration by Voyager 2 in 1986 and observation by a large-scale telescope on the ground. It is thought to be a cloud of methane ice. The time scale of this cloud change is wide, ranging from a few days to a few years, but large telescopes and space telescopes often observe only a few days once a year, and the time scale of the change is not well understood. The goal of this research is to make continuous observations of Uranus by making full use of the abundant machine time of the Pirka Telescope, and to clarify the existence of bright clouds and the time change of their size on a scale of weeks and months. If there are clouds on Uranus' surface, the overall flux of Uranus in the methane band will vary with cloud area. However, fluxes other than the methane band are not affected by the presence of clouds. By utilizing this fact, the existence of clouds is estimated by comparing the fluxes at the wavelengths other than the methane band. In this presentation, we will introduce the analysis results of 11/12 observation data to the present.
06/16 14:45--16:15 Tatsuharu Ono
The lightning flashes observation is useful as a way to understand the atmospheric large structure and the chemical reaction constituting the atmosphere. The lightning flashes have been observed in the Earth and Jupiter. It is suggested that there is a relationship between the zonal jet and the cumulonimbus with lightning in Jupiter (Gierasch et al.,2000, Ingersol et al., 2000). It is difficult to know the vertical convection covered by the dense clouds by using multi-wavelength observation. However, the lightning flashes observation can use for monitoring the atmosphere dynamics like the vertical convection covered by dense clouds. And one hypothesis suggests that some components of the Jovian atmosphere are created by lightning flashes. It is important to know the lightning to understand the formation mechanism of the atmosphere. In Venus, it is considered that there are lightning generated by the charge separation by the ice particle like the Earth or cloud particles of sulfuric acid. However, the existence of Venusian lightning is controversial for over 20 years. In the previous study, there are radio wave observations and optical observations by CCD. There is no robust evidence of existence the lightning because it is difficult to distinguish between the lightning signal and the electrical noise or other plasma waves, the observation area is limited, and the CCD's sensitivity is not enough for lightning flashes. If we can confirm the existence of Venusian lightning like the Jovian, it leads to an understanding of the Venusian atmosphere dynamics and atmospheric components. In this study, we observe the planetary lightning with the photomultiplier tube. For Venus, we observe more than tens of hours to obtain the lightnings light curve, occurrence frequency, and distribution. We would reveal the relationship between lightning and atmosphere dynamics by comparing the obtained lightning data and wind velocity and cloud distribution. The Planetary Lightning Detector (PLD) we developed is designed for Venusian and Jovian lightning flashes' observation. From the previous study, the dominant wavelength of the lightning flashes could be 777 nm in Venus (Borucki et al.,1996). PLD equips narrowband filter (FWHM = 1nm) of 777 nm. PLD observes the light by using a Photomultiplier tube. The minimum exposure time is 50 microseconds. The maximum time resolution is about 2x10^4 points/s. PLDs FOV can be changed to 5, 10, 30, 60 pinhole, and 2x11 slit by using field stops. Slit and Pinhole are used for Venuss night-side observation. To obtain the lightnings light curve, we operate the bandpass filter to remove noise and large time scale variation by the atmosphere. And then, we search the large count value over 4-sigma. We have observed Venus by using PLD. For Venuss data, we have obtained a few events whose count value is over the 4-sigma. These energies are estimated. The energy is about 10^7 to 10^8 J. However, the rate of the flash event is similar to the rate estimated by the noise sample. From this result, its considered we only observed the cosmic ray or noise in this observation time. The observation time is not enough to reveal the lightning occurrence frequency for Venus. In the future, we increase the total observation time by using shorter exposure time. In this seminar, we introduce the PLD and discuss the result observed from May 2020.
06/23 14:45--16:15 AHMAD SHAQEER MOHAMED THAHEER
Water pollution has become a serious issue in Malaysia due to its major threat to the ecosystem and reduces water production and supply to the houses. The traditional approach of finding and monitoring wetland using in situ measurement methods is found to be infeasible given the cost and time requirements and difficulties in accessing the required area. Thus, remote sensing-based methods using multispectral are much more favored. Even still, the methods have shortcomings such as it has a specific spatial resolution, dependent on weather conditions, besides with water bodies have low spectral reflectance, and a certain type of wetlands share the same spectral characteristics with water, thus, increasing the difficulty in distinguishing both features. The multiple pointing satellite system is required to combat the problems yet it requires new measurement techniques and databases. Therefore, this study focuses on the bidirectional reflectance factor (BRF) measurement of polluted water. BRF measurement helps in visualizing the reflectance with respect to the changing of the angles i.e. azimuth, zenith, light incidence, camera reflected, and polarization angles. Furthermore, polarization helps in separating the polarized and unpolarized effect of the light reflected by the surface. This phenomenon will help in obtaining the information on the water near-surface condition. Even so, the method has to be tested as ideal and real conditions are different due to several factors. This seminar attempted to show the preliminary analysis results of polluted water near Klang Estuary including the Klang River which was rated as polluted by the Department of Environmental Malaysia in 2018. This study uses Landsat-8 data and the SpectrumCatcher developed by Hokkaido University to measure the water reflectance.
06/30 14:45--16:15 Torabi Kambiz
Linkage between the 11-year solar activity based on sunspot number and climate change of the Earth has been suggested by monthly or yearly averaged data, even though short periodic variation could modulate longer periodic phenomena. In previous study, 27-day variation of Outgoing Longwave Radiation (OLR) during solar maximum year was found by Takahashi et al. (2010). Moreover, anti-phase relation between lightning around Marine Continent and OLR around Western Pacific Warm Pool region was found by Sanmiya et al. (2013). Motivation of this study is that clarifying the phase relation of about one-month periodic variation of OLR in Western Pacific Warm Pool and the Equator. We have chosen one main data from OLR in WPWP, OLR in the Equator, cosmic rays and F10.7, then selected spikes and data from -15 to +15 day from each spike, also plied up those data. We calculated time range as all duration, solar maximum year and solar minimum year respectively. Western Pacific Warm Pool is known as correlating negatively with lightning around the Marine Continent and typhoon-rich area. The equator is known as correlating positively with lightning around the Marine Continent and typhoon-pool area. We will discuss characteristics of variation of phase relation from 1974 to 2018 which includes 21st to 24th of solar cycle.
07/07 14:45--16:15 Meryl Regine Algodon
The Asia-Pacific region's extreme weather comprises mostly of typhoons and tropical cyclones.These cause deaths and damaged properties to several countries. Consequently, it is important to analyze this meteorological phenomenon to allow researchers to understand its behavior, and properly mitigate the hazards that go with it. A standard mode of visualization of typhoons involves the use of three-dimensional representations of a typhoon cloud top. Creating a three-dimensional model requires visible distinct features or landmarks in the clouds stereo images. This is difficult as clouds do not normally have rigid structures like points and corners to serve as landmarks. In this study, an experiment under the ULAT project (ULAT: Understanding Lightning and Thunderstorm) was conducted where images of Typhoon Trami were taken from an aircraft and by DIWATA-1 satellite last September 26, 2018. A 3D model of Typhoon Tramis cloud top was reconstructed from the images using a commercially available software. Aircraft or low-altitude satellite images provide closer views of the typhoon cloud top than that of geostationary satellite images making it easier to reconstruct a 3D model. This allows for the manual adjustment of the camera to capture images ideal for 3D reconstructions. From the result, an estimate of the cloud top dimension was derived and validated by mapping Himawari Thermal Infrared bands with cloud-top height measured by dropsonde data.
07/21 14:45--16:15 Yokota Shuntaro
Polarimetric observation is an effective method for determining the particle properties of the planet's surface and atmosphere. From this reason, many polarimetric observations of Jovian atmosphere have been performed so far. Although previous studies show the difference in the polarization degree depending on the Jovian latitude [McLean et al., 2017, Schmid et al., 2011], there are few observations tracking the regional differences of the polarization degree in a short term period, such as a few hours or a few days. Thus, the data volume is insufficient enough to discuss the temporal variations of particle characteristics. The purpose of this study is to observe the motion of the polar upper layer in the Jovian atmosphere and the temporal variations of the particle characteristics from the polarimetric and multispectral imaging using the 1.6 m Pirka telescope operated by Hokkaido University and to clarify the convection mechanism of the Jovian atmosphere by comparing the multispectral imaging data to polarimetric imaging data. In this presentation, we introduce the results derived from the spectral imaging observations and the polarimetric imaging observations using the Multi Spectral Imager (MSI) (pixel scale = 0.39/ pix) with the band-pass filters of 650 nm, 727 nm, and 889 nm, which is mounted on the Pirka telescope. We conducted the MSI observations from May to August 2019. The images at the methane absorption wavelength of 727 nm and 889 nm show bright clouds and haze layers in Jovian atmosphere due to the higher ratio of scattered light. Liquid Crystal Variable Filter (LCTF) installed in the MSI can be used for the polarimetric observations with the linear polarizer. We obtained the polarimetric data of May 22, 2019 (observed longitudinal range was 120 270 deg) and June 24, 2019 (0 180 deg). The latitudinal variations of the stokes parameter are comparable with the results reported by the previous studies. In order to monitor the temporal variations of the cloud/haze structure and their polarimetric characteristics, it is necessary to simultaneously obtain the multispectral and polarimetric data with the time resolution of 1 day. At the presentation, we will show the initial results derived from the image analysis and will show the future observation plan more in detail.
07/28 14:45--16:15 Garid Zorigoo
A smartphone spectrometer is a handy tool to get the spectrum of an object such as leaf or soil, designed for anyone ranging from farmers to scientists. When the light enters the narrow slit in front of the spectrometer, it gets diffracted and imaged by the monochromatic camera. Then, with the help of a smartphone, this monochromatic image of the spectrum gets processed. The working principle is simple, yet it gives more spectral-data accessibility to anyone. Combined with a controllable gimbal, a smartphone spectrometer can measure the spectrum on any azimuth and elevation angle. The sensors built-in inside of the smartphones (accelerometer, magnetic, GPS) is convenient for such a measurement. In consequence, we can measure the spectral data of the entire cropland. This study is to make fundamental techniques and libraries of codes for processing data collected by the device. The output of this work will be used in multiple ongoing projects and other future studies.
08/04 14:45--16:15 Loren Joy Estrebillo
Hazards linked with climate change pose increasing risks as frequency and intensity of extreme weather events increase. Flooding, landslides, and storm surges brought about by tropical cyclones (TCs) cause the greatest loss in lives and destruction to properties and infrastructure, yet accurate forecast of the timing, location, and intensity of TCs remain an ongoing challenge. Located along the typhoon belt in the western North Pacific (WNP), the Philippines experiences an average of 20 typhoons each year, about 8 or 9 cross and/or make landfall on the Philippine landmass. There has been a significant development in the accuracy of TC track forecast within the Philippine Area of Responsibility (PAR) over the years with the use of ground-based synoptic observations, automatic weather stations, weather radars, and meteorological satellites. Lightning activity is the indicator of the dynamics and microphysics in thunderstorms. Recent studies suggest that lightning activity in tropical cyclones can give predictive information about its intensity development. Thus, a ground-based lightning observation system (V-POTEKA) has been developed, and it has been installed at four stations in the Philippines, Guam, Palau and Okinawa, Japan. The V-POTEKA system uses the event-trigger method and can detect radio wave pulses from lightning discharges in the very low frequency (VLF) range of 1-50 kHz. It also consists of the automatic weather station (AWS), the VLF sensors, and the automatic data-processing unit. The V-POTEKA system analyzes lightning data, extracts pertinent information, i.e., peak amplitude and time of the triggered waveform, and transmits data to the data server in Japan and the Philippine through 3G communication. Lightning locations from the V-POTEKA data are calculated using the difference in time-of-arrival (TOA) method. In this seminar, I will present the results of the cross-correlation analysis of lightning activity in TCs along the WNP region using V-POTEKA and Blitz lightning datasets. Select TCs in 2019 were examined best track data from the Japan Meteorological Agency and Joint Typhoon Warning Center, and ocean surface winds from NASA Cyclone Global Navigation Satellite System (CYGNSS). Highest correlations were calculated for optimal lags among lightning and TC intensity (maximum sustained winds and minimum central pressure) were calculated having mean correlation values of 0.6-0.7 with peak winds occurring at approximately 30 hours before the lightning peak.
08/11 14:45--16:15 Ishida Yurino
Global food insecurity has increased in recent years, and increasing food production is one of the critical goals to address the situation. Food production can be increased by closing the current yield gap. Soil nutrient deficiency is a well-known constraint to crop production. However, our findings from a recent soil survey conducted in Kenya and Indonesia showed that excess soil nutrients could also be a major constraint to crop production. It could be due to differences in fertilizer management strategies among farmers, which underpins the importance of performing soil diagnosis and the use of appropriate fertilizer management strategies. Currently, soil diagnosis takes too long to manage the amount of fertilizer. For prompt fertilizer management, we developed a simple soil diagnosis method that can easily be performed by a person at the field in our graduate thesis. This study focused on developing simple soil diagnosis methods for (i) available phosphate, a parameter shown to vary widely in farmers fields due to differences in fertilizer management, and (ii) soil pH, a parameter affected by soil base materials and fertilizer management. This method is beneficial for small fields and can increase food production. However, this method is still a time-consuming job using vast fields. Therefore, it is necessary to develop a new method of prediction of soil nutrients that can easily be performed by a person, even in the huge fields. Our future work focused on developing simple soil diagnosis that predicts soil nutrients by the spectrum of the plants that took by the Spectrum Catcher. In this seminar, we introduce our graduate thesis and research plan.
08/18 14:45--16:15 Watabe Narumi
Rainfall by thunderstorms and typhoons causes a large-scale disaster mainly in Southeast Asia. Damage from disasters must be minimized by monitoring them in real-time and forecasting them. It is known that the typhoon shows the maximum wind speed after 1-2 days when the frequency of thunder is high. There is a strong correlation between lightning activity and guerrilla rainfall, as the frequency of lightning and the intensity of typhoons change over time. However, lightning is an electric phenomenon, and the magnitude of its energy is represented by voltage and current. Among them, it is impossible to directly measure the voltage of lightning, so only the current can be accurately measured. Also, the energy of lightning cannot be calculated because there is no means for measuring the resistance of lightning. It is necessary to develop new methods for estimating lighting energy. So we focused on infrasound. Infrasound refers to sound waves below the lower limit of human hearing (20Hz). The wavelength of infrasound is on the scale of kilometers, so it can occur only when something huge moves. The sources of infrasound are mainly natural phenomena of geophysics including lightning in addition to artificial explosions. The remote detection of information such as the scale of the natural phenomenon is expected to contribute to disaster prevention and mitigation. The infrasound sensor developed by the Kochi University of Technology adopted a method that converts minute changes in sound pressure into electrical signals. Using this sensor, we aimed to estimate the energy of lightning, which is difficult to observe with electromagnetic waves and to establish a method to improve the detection accuracy of the lightning location. We experimented to calibrate whether the infrasound sensor developed by the Kochi University of Technology could be used for lightning. The experiment was conducted using fireworks, which is a type of artificial explosion that can calculate the explosion energy. In this seminar, we introduce our research plans.
09/01 14:45--16:15 Noda Akira
The traditional numerical methods are limited in forecasting nonlinear rainfall such as guerrilla rain or linear precipitation zone. Recently, machine learning methods receive big attention as a new forecasting method and show great potential for prediction of these rainfalls in many studies. I`m going to introduce one of them and finally I`ll show my study plan. If we can predict them correctly, it must be very useful for water disaster prevention.
09/08 14:45--16:15 Hamada Kizuku
Galileo satellite are Jupiters satellite. One of them is Europa. Europa is covered ice crust. It is thought that there is liquid ocean under the surface. Liquid water is one of the most important material for life, and the potential habitability of the ocean depends on its chemical composition. Previous study shows that Europa have geyser. If in Europa subsurface ocean plume to the surface, knowing the composition of the surface lead to understand that of subsurface ocean. In this seminar Ill show you that my observation of NaCl on the surface using Pirka telescope.
09/15 14:45--16:15 Arikawa Kana
Mercury has a slight atmosphere.Its origin has not yet been elucidated.Previous studies have reported seasonal changes in the Mercury Na atmosphere.In order to understand the time variation of the Na atmosphere, it is necessary to start from the development of equipment to obtain observational data.Because Mercury is the closest planet to the Sun, it is difficult to observe.This time, I will talk about the observation method of the Mercury Na atmosphere and the development schedule of the observation equipment necessary for that purpose.If the observation device is completed and more time fluctuation data can be obtained, it should be useful for understanding the time fluctuation mechanism of the Na atmosphere in the future.
09/15 14:45--16:15 Hirobe Takumi
Compared to forests, which occupy more than half of Japan's land area, the number of forests that need to be cut down is increasing year by year. In addition, the forestry industry is small, there are many micro businesses, the aging rate is high, and price competitiveness with overseas is lost.Therefore, modern forestry is required to have high productivity and management ability, and ICT technology is attracting attention.In this study, we show that it brings high efficiency to forestry by exploring the possibility of remote sensing of tree species by spectral analysis using drones as ICT technology.
10/28 13:00--14:30 Ono Tatsuharu
Lightning is useful to monitor the atmosphere dynamics. We have found lightning on Jupiter by spacecraft nightside observations (Little et al.,2000, Becker et al., 2020). There are lightning around the cumulonimbus on Jupiter. The vertical convection creates this cumulonimbus. There would be a relationship between the vertical convection and the zonal jet. The previous study suggests that vertical convection supplies the energy to form the zonal jet by coupling the multi small-scale eddies (Gierasch et al.,2000, Ingersol et al., 2000). The vertical convection causes material mixing. The vertical convection transport the ammonium from the lower layer (Guillot et al., 2020). This mixing affects Jupiter's vertical structure. The observations of the vertical convection are difficult by using multi-wavelength because the convection is covered by the dense clouds. We can expect to obtain the information of vertical convection by monitoring the lightning if it is assumed that lightning occurs when cumulonimbus clouds form. Although the existence of Venusian lightning is controversial for over 30 years, it is considered that there are lightning generated by the charge separation by the ice particle like the Earth or cloud particles of sulfuric acid. In the previous study, there are radio wave observations and optical observations by CCD. There is no robust evidence of the existence of lightning because it is difficult to distinguish between the lightning signal and the electrical noise or other plasma waves, the observation area is limited, and the CCD's sensitivity is not enough for lightning flashes. If we can confirm the existence of Venusian lightning like the Jovian, it leads to an understanding of the Venusian atmosphere dynamics and atmospheric components. In this study, we develop a measurement technique to observe the planetary lightning with the photomultiplier tube using a ground-based telescope. We use the ground-based telescope to increase the observation time and area. we observe more than tens of hours to obtain the lightnings light curve, occurrence frequency, and distribution. The previous studys observation time is from a few hours to a few days in a few years. We would reveal the relationship between lightning and atmosphere dynamics by comparing the obtained lightning data and wind velocity and cloud distribution. The Planetary Lightning Detector (PLD) we developed is designed for Venusian and Jovian lightning flashes' observation. From the previous study, the dominant wavelength of the lightning flashes could be 777 nm in Venus, 656 nm in Jupiter (Borucki et al.,1996). PLD equips narrowband filter (FWHM = 1nm) of 777 nm and 656 nm. PLD observes the light by using a Photomultiplier tube. The minimum exposure time is 50 microseconds. The maximum time resolution is about 2x10^4 points/s. PLDs FOV can be changed to 5, 10, 30, 60 pinhole, and 2x11 slit by using field stops. To obtain the lightnings light curve, we operate the bandpass filter to remove noise and large time scale variation by the atmosphere. And then, we search the large count value over 4-sigma. We have observed Venus by using PLD. We found a total of 47 candidate events for Jupiters data. The number of events caused by light variations would be about 20. The observed area is about 5.3x10^3 km^2. The total observed time is about 5.0 hours. The event rate is 2.45x10^-13 s^-1km^-2. The event rate estimated by the previous study is 1.3x10^-10 s^-1km^-2 (Little et al.,2000) or 1.9x10^-9 s^-1km^-2 (Becker et al.,2020). Our results are about 50 times or about 700 times smaller than previous results. It would be because we detected only the large energy lightning in which optical energy is larger than 10^10 J. We havent considered the blurring Jupiter image at this time. In the future, we have to improve the technique to remove the noise and dayside variation to distinguish the flash event. In this seminar, we introduce the PLD and discuss Jupiters result observed from July 2020.
11/11 13:00--14:30 Sato Yuki
Neptune is the eighth planet of the solar system. Its mainly composed of hydrogen and helium. Previous study shows that storms occur at both northernand southern mid latitude. (15－60N, 15－60S)[Imke de Pater et al., 2014]. Storms rotate at a certain speed in the longitude direction. The speed of storms is correlated with the zonal winds measured by Voyager 2. In this study, we developed the technique to estimate the drift rate,intensity and latitude of storms by observing a whole spectrum of Neptune. By using this technique, when seeing is bad, its possible to observe Neptune in short time span for a long term. In this seminar, we estimated the intensity, drift rate and latitude of storms in 2017－2020. we use methane absorption band in this study. Methane absorbs an 890 nm flux strongly. When we observe the aspect with a storm at 890 nm, an 890 nm flux becomes stronger compared to the aspect without a storm. This is because the altitude of storms is higher than that of other areas. And the apparent area of storms changes by the rotation of Neptune, so 890 nm flux changes. We calculate the theoretical line of an 890 nm flux changing by the rotation. The theoretical value also changes with the latitude of storms. The sub-observer latitude during our observation is about 24S, so if a storm is located in the southern hemisphere, the theoretical line becomes broader. If the northern hemisphere, it becomes narrower. We take the ratio of an 890nm flux and an flux of 855 nm to correct the effect of the Earth atmosphere, and fit the theoretical line with the observed values in the least squares method. In this presentation, Ill show the results of my observation.
11/18 13:00--14:30 Meryl Regine Algodon
The Asia-Pacific region's extreme weather comprises mostly of typhoons and tropical cyclones.These cause deaths and damaged properties to several countries. Consequently, it is important to analyze this meteorological phenomenon to allow researchers to understand its behavior, and properly mitigate the hazards that go with it. A standard mode of visualization of typhoons involves the use of three-dimensional representations of a typhoon cloud top. Creating a three-dimensional model requires visible distinct features or landmarks in the clouds stereo images. This is difficult as clouds do not normally have rigid structures like points and corners to serve as landmarks. In this study, an experiment under the ULAT project (ULAT: Understanding Lightning and Thunderstorm) was conducted where images of Typhoon Trami were taken from an aircraft last September 26, 2018. A 3D model of Typhoon Tramis cloud top was reconstructed from the images using a commercially available software. Aircraft or low-altitude satellite images provide closer views of the typhoon cloud top than that of geostationary satellite images making it easier to reconstruct a 3D model. This allows for the manual adjustment of the camera to capture images ideal for 3D reconstructions. The cloud-top altitude was estimated using NOAA sonde data where the cloud altitude was correlated with temperature measurement. This analysis was used to map the cloud altitude with brightness temperature from the Himawari Thermal Infrared bands of Typhoon Trami. An algorithm was also developed to improve the cloud altitude estimation by determining the boundary of the clouds to be analyzed.
11/25 13:00--14:30 Yurino Ishida
Global food insecurity has increased in recent years, and increasing food production is one of the important goals to address the situation. Food production can be increased by closing the current yield gap. For closing the current yield gap, performing soil diagnosis and the use of appropriate fertilizer management strategies are necessary. However, soil diagnosis doesnt function well due to the lack of facilities and the standard procedures of the diagnosis take a too long time to manage the amount of fertilizer. Some soil nutrients strongly relate to soil color. In previous studies, soil organic matter, one of the soil nutrients that play an important role in crop vegetation, was predicted by the reflectance of the soil. However, most soil nutrients couldnt relate to soil color and predict by the reflectance of soil. We try to approach the prediction of soil nutrients from the reflectance of plants by using the Spectrum Catcher. The spectrum Catcher is a handy tool to get the spectrum of an object such as leaf or soil, designed for anyone ranging from farmers to scientists. This system makes it easy to get a spectroscopic image to anyone. The objective of this study is to calibrate and validate the prediction of soil nutrients models by using the image by the Spectrum Catcher. In this seminar, we introduce the method to get the reflectance of plants from spectroscopy images taken by the Spectrum Catcher.
12/02 13:00--14:30 Ahmad Shaqeer
Water pollution has become a serious issue in Malaysia due to its major threat to the ecosystem and reduces water production and supply to the houses. The traditional approach of finding and monitoring wetland using in situ measurement methods is found to be infeasible given the cost and time requirements and difficulties in accessing the required area. Thus, remote sensing-based methods using multispectral are much more favored. Even still, the methods have shortcomings such as it has a specific spatial resolution, dependent on weather conditions, besides with water bodies have low spectral reflectance, and a certain type of wetlands share the same spectral characteristics with water, thus, increasing the difficulty in distinguishing both features. The multiple pointing satellite system is required to combat the problems yet it requires new measurement techniques and databases. Therefore, this study focuses on the bidirectional reflectance factor (BRF) measurement of polluted water. BRF measurement helps in visualizing the reflectance with respect to the changing of the angles i.e. azimuth, zenith, light incidence, camera reflected, and polarization angles. Furthermore, polarization helps in separating the polarized and unpolarized effect of the light reflected by the surface. This phenomenon will help in obtaining the information on the water near-surface condition. Even so, the method has to be tested as ideal and real conditions are different due to several factors. This seminar attempted to show the preliminary analysis results of polluted water near Klang Estuary including the Klang River which was rated as polluted by the Department of Environmental Malaysia in 2019. This seminar also will show the spectral measurement results that were done at Lake Kasumigaura and its correlation results with the collected samples at the lake. This study uses Landsat-8, Sentinel-2, and PlanetScope data and the SpectrumCatcher developed by Hokkaido University to measure the water reflectance.
12/09 13:00--14:30 Kambiz Torabi
Linkage between the 11-year solar activity based on sunspot number and climate change of the Earth has been suggested by monthly or yearly averaged data even though intraseasonal variation is existing such as Madden-Julian oscillation. Madden-Julian oscillation is one of the well known tropical atmospheric phenomenon. However, it is not reproduced by simulation not because of modeling but because of lack of fundamental understanding of the tropical atmosphere. Motivation of this study is that clarifying the phase relations of about one-month periodic variation of OLR in Western Pacific Warm Pool (WPWP), highest Sea Surface Temperature and important area for both El Nino/La Nina and Madden-Julian oscillation, and OLR in Equator, area integrated the area for half the equator. Moreover, we would suggest that importance for considering solar parameter not only Cosmic ray or F10.7 but also Dst index or Kp index from our results.
12/16 13:00--14:30 Yokota Shuntaro
Polarimetric observation is an effective method for determining the particle properties of the planet's surface and atmosphere. Polarimetric imaging provides information on the intensity of scattered light, which can be combined with model calculations to constrain particle properties. From this reason, many polarimetric observations of Jovian atmosphere have been performed so far. Previous studies have shown the distribution of polarization with Jupiter's latitude, confirming the effects of stripe structure and high-altitude haze [McLean et al., 2017, Schmid et al., 2011]. Polarimetric imaging at high polarization with methane absorption wavelengths is suitable for elucidating the variation of particle characteristics corresponding to cloud structure. For spectroscopic imaging observations, methane absorption wavelength have sensitivity at specific altitudes from the upper troposphere to the stratosphere due to the optical path difference of the reflected light [Karkoschka et al., 1994], and the vertical structure of Jupiter's atmosphere has been elucidated using multiple methane absorption wavelengths in ground-based telescopes and spacecraft observations. Previous studies have only observed polarization only a few times a year, and the temporal variation of particle characteristics has not been clarified. The temporal variability of particle properties in the upper troposphere and stratosphere, focusing on the spatiotemporal variability of clouds, has not been sufficiently discussed. The purpose of this study is to observe the motion of the polar upper layer in the Jovian atmosphere and the temporal variations of the particle characteristics from the polarimetric and multispectral imaging using the 1.6 m Pirka telescope operated by Hokkaido University and to clarify the convection mechanism of the Jovian atmosphere by comparing the multispectral imaging data to polarimetric imaging data. In this presentation, we introduce the results derived from the spectral imaging observations and the polarimetric imaging observations using the Multi Spectral Imager (MSI) (pixel scale = 0.39 / pix) with the band-pass filters of 619 nm, 727 nm, 756 nm, and 889 nm, which is mounted on the Pirka telescope. We conducted the MSI observations from May 2019 to October 2020. For this observation, we have conducted 27 nights observation and the typical seeing size was 4 arcseconds. In order to monitor the temporal variations of the cloud/haze structure and their polarimetric characteristics, it is necessary to simultaneously obtain the multispectral and polarimetric data with every few days interval. The images at the methane absorption wavelength of 619 nm, 727 nm and 889 nm show bright clouds and haze layers in Jovian atmosphere due to the higher ratio of scattered light. The deepest methane absorption at 889 nm shows the strongest polar polarization and strong latitudinal dependence consistent with the results of Schmid et al.,[2011]. There is a correlation between the polarization and the flux intensity corrected for peripheral attenuation in the 727 nm and 889 nm imaging. This relationship is strong in the latitudinal direction and it is reflected by the zone and band structure. We can also see variation of polarization in the longitude direction, and it is possible to be reflected by the differences in cloud top height and particle composition within each structure. For the observations up to 2020, we obtained data for several consecutive days and data with intervals of more than one week. In this presentation, Ill show the results of my observation.
12/23 13:00--14:30 Niwa Shunsuke
Prediction of the Tropical Cyclone (TC) intensity such as maximum sustained wind and minimum sea surface pressure is an important issue for a long time. Previous studies suggested that lightning activity in TCs has a possibility to improve the accuracy of intensity prediction. Although relations between lightning frequency and TC intensity have been investigated in the previous studies, relations of electrical properties(EPs) of lightning with TC intensity have not been studied. In this study, we investigated the relations of EPs of lightning (peak current (Ip), charge moment change (Qdl) and charge amount (Q)) every 6 hours during the lifetime of 28 TCs over the Western North Pacific in 2013. We used the best track data of TCs provided by Joint Typhoon Warning Center (JTWC), time and location of lightning data provided by World Wide Lightning Network (WWLLN) and Extremely Low Frequency (ELF) magnetic field data obtained at two stations of Global ELF Observation Network (GEON), Syowa (69.0S, 39.5E) and Kuju(33.1N, 131.2E) for calculating EPs. ELF magnetic waveforms at Syowa station were used for calculating Ip and Qdl, Kuju for calculating Q. For the case of Ip and Qdl, we set two thretholds of the magnetic field at Syowa, 20 pT and 10 pT. The events exceeding 20 pT can be used to derive Ip and Qdl, but the events with 10~20 pT can be used for derive only Qdl. In order to compare TC intensity with lightning parameters, median values of EPs of lightning in the inner core region (100 km from the center of TC, 200 km for large TCs) and in the rainband region ( 100 km ~ 500 km from the center, 200 km ~ 1000 km for large TCs) every 6 hours and maximum values of the cross-correlation coefficients and lag time were calculated. We find that the inner core of weak TCs (category 1,2) with strong lightning activity (more than 50 lightning events with B > 20 pT at Syowa) and violent TCs (category 5) tend to have better correlation of EPs with maximum sustained wind than that of lightning frequency. When TCs are devided into two track type, westward and northward, TCs moving westward have better correlation between EPs of lightning and TC intensity than TCs moving northward. We also found that the inner core of TCs with more than 50 intense lightning ( B > 20 pT at Syowa ) have stronger relation between EPs and TC intensity than the case of less intense lightning. In the inner core with many intense lightning, the correlation coefficients of EPs are higher than that of lightning frequency detected by WWLLN. Therefore, the inner core of TCs with intense lightning have more possibility to improve intensity prediction than lightning frequency.
01/06 13:00--14:30 Futamura Yuki
The stratosphere in the polar region of Jupiter has denser haze than other latitudinal regions of stratosphere. It is known that the polar haze has a cap-like feature. However, their dynamics have not been investigated in detail. Polarimetric observation is effective for investigating physical parameters such as haze particle size and optical thickness, but there are only a few examples of observation for the structure in the longitudinal direction. In this study, we conducted polarimetric imaging observation of Jupiter at Syowa Station in Antarctica, where you can see Jupiter at high altitude (10 or more in elevation) for a period exceeding Jupiter's rotation cycle (about 10 hours), every 5 months during the winter season in Antarctica in 2019. As a result, the longest continuous observation per observation was 14 hours. Polar haze was observed in the wavelength range of 8905 nm using a bandpass filter including the methane absorption wavelength range. As an initial analysis, the Jupiter image was magnified and adjusted in position, the peripheral extinction was corrected, the haze region was determined from the latitude distribution of brightness, and the polarization degree of that region was obtained. We concluded that the degree of polarization is not uniform as a function of longitude and its variation has a correlation with magnetic field.
01/27 13:00--14:30 Noda Akira
It is difficult to predict the occurrence and rain volume of torrential rainfalls, such as guerrilla rain, rain band with typhoon and linear precipitation zone. As heavy rain area is spatially localized and the parent thunderstorm tends to develop within a short time, it makes difficult to accurately predict the occurrence location/time and rain volume. Recently, the machine learning technique is remarkably developed with the improved processing speed of computers and with a huge amount of the data. In addition to this, the application of the machine learning methods to the meteorological fields is intensively tried in the world. Since 2017, we started installing the automatic weather observation system (AWS) named as P-POTEKA in Metro Manila, the Philippines, which is one of the cities suffering from the torrential rainfall and related flood. So far, we installed 35-P-POTEKAs in Metro Manila and continue the weather observations (rain volume, temperature, air pressure, humidity, wind speed, wind direction and solar radiation) with the time resolution of 1 min. In this study, we used both P-POTEKA rain volume data and machine learning model (ConvLSTM: Convolutional Long-Short Term Memory) in order to predict the near future (< 1hour) rain volume and distribution. At the presentation, we will show the results derived from the machine learning prediction of the rain volume and distribution more in detail.
01/27 13:00--14:30 Hamada Kizuku
Galileo satellite are Jovian satellite. One of them is Europa. Europa is covered ice crust. It is thought that there is liquid ocean under the surface. Liquid water is one of the most important material for life, and the potential habitability of the ocean depends on its chemical composition. Previous study shows that Europa have geyser. If in Europa subsurface ocean plume to the surface, knowing the composition of the surface lead to understand that of subsurface ocean. Furthermore, it is thought that NaCl on the surface creates vacancy in the crystal strucuture that absorb specific wavelengths due to the strong radiation belt of Jupiter, and it has been confirmed by HST observations. In this seminar Ill show you that my observation of NaCl on the surface using Pirka telescope.
02/03 13:00--14:30 Arikawa Kana
Mercury is the innermost planet in the solar system.Mercury is known to have a dilute atmosphere.Previous studies have shown seasonal fluctuations in the Mercury Na atmosphere due to collisions with interplanetary dust and temporal fluctuations in the Mercury Ca atmosphere due to collisions between interplanetary dust and comet Encke dust.The ultimate goal of this study is to observe the time variation of the atmosphere of Mercury Na using the Pirka telescope, investigate the relationship with Comet Encke, and elucidate the origin of the atmosphere.In this seminar, we will show that the first stage, the observability of the Mercury Na atmosphere, was examined using the Pirka telescope.
02/03 13:00--14:30 Hirobe Takumi
Tree species identification using remote sensing has been proposed as a way to improve the efficiency of forestry in Japan. So far, image (RGB) analysis using satellites and drones and analysis using reflection spectra have been conducted. However, while the analysis is highly accurate, it often requires expensive measurement equipment and is time-consuming, making it practically difficult to implement in forestry. The ultimate goal of this research is to reveal inexpensive and accurate tree species identification by drones using estimation by reflection spectra. As a first step of this research, we will discuss the possibility of making measurements in the Uryu Research Forest in Hokkaido, Japan on September 17, 2020.
02/10 13:00--14:30 Garid Zorigoo
Plants have a waxy-cuticle outer layer on their leaves to protect from dehydration. Different plant species have different waxy-cuticle layer thickness and surface roughness. The previous study suggests that one can estimate this waxy-cuticle layer property (mainly thickness part) with the mirror reflection measurement with polarizer. Not only that, but also we have some findings which suggest that within a same-species, outer cuticle-layer differs from the different environmental stresses. With adequate enough dataset or measurements consisting various different-species, diverse environmental-stresses, we could find a method to detect those environmental conditions just from the optical measurement. This kind of optical measurement and detection method is quite crucial to place where late-detection of plant-disease or nutrition-deficiency affects hugely to the harvest (in some cases like banana-plant, there is no cure from the disease once it shows symptoms to naked eye). To create this enormous dataset, a lot of manual work and scheduled measurements are needed. To overcome this issue, we are developing a fully autonomous goniometer measurement device at FMI center. In this presentation, I will introduce you to this device, what kind of measurement it can do, and finally discuss some measurements it already done.
02/17 13:00--14:30 Watabe Narumi
Rainfall by thunderstorms and typhoons causes a large-scale disaster, especially in Southeast Asia and other tropical regions. Damage caused by disasters could be minimized by monitoring and predicting in real-time. It is known that typhoon shows the maximum wind speed 1-2 days after the peak of lightning frequency. There is a strong correlation between lightning activity and torrential rainfall. If we could monitor the lightning activity quantitatively, it must be useful to monitor and predict strong rainfall. Lightning is an electrical phenomenon, and the magnitude of its significance is usually represented by its peak current and charge moment change before and after the stroke. However, the energy dissipation by lightning, which might be a good indicator of atmospheric convection, cannot be estimated only from the electromagnetic field measurement since it is impossible to measure the conductivity in the discharge path. Here we focus on infrasound below 20 Hz, which may be a good proxy of energy dissipation caused by lightning stroke. In order to estimate the dissipated energy by lightning stroke, we need to know the quantitative relationship between the dissipated energy and the intensity of infrasound in another way. In the present research, we try to calibrate the quantitative relationship between infrasound intensity measured at a known distance and dissipated energy in the atmosphere, using two kinds of fireworks displays. At a building of Hokkaido University, we measured the infrasound pressure of fireworks for some cases which occurred at the range of 5 km. We also carried out similar measurement in the lakeside of Lake Toya in Hokkaido in distance range of 0.3 - 4 km. The maximum dissipated energies of the fireworks are in ~10^6 J, which is approximately 1,000-5,000 times smaller than that of typical lightning, namely. Based on these measurements, we determined the constant to calculate the dissipated energy from infrasound pressure measurement. On the other hand, this constant is not very stable for different cases probably due to the variations in sound spectrum, the height of explosion, the temperature profile of the atmosphere near surface. We need to consider such conditions when we estimate the dissipated energy of lightning, adding to the effect of line source of the sound in lightning path while the fireworks have a point source.
02/24 13:00--14:30 Hamamoto Ko
Venus is covered by thick sulfuric acid clouds extending from 50 to 70 km in altitude, which reflect about 80% of the incident sunlight, but in the ultraviolet wavelength range, various patterns are observed due to absorption by SO2 and an unknown absorber. The unknown absorber contributes to about half of the solar heating in the Venusian atmosphere. The distribution and temporal variability of the unknown absorber are important basic information for understanding the Venusian climate system. Long-term observations in the UV wavelength range by spacecraft including the Venus Climate Orbiter AKATSUKI and Venus Express, as well as space telescopes, have revealed that the albedo at 365 nm, where the absorption of the unknown absorber has been observed, fluctuates between 0.2-0.4 at low latitudes and 0.3-0.6 at high latitudes from 2006 to 2017[Lee et al., 2019]. However, the mechanism of this albedo variability has not been clairfied, and continuous observations are important to understand the characteristics of this variability. This study aims to use observational data to elucidate the long-term changes in albedo in the UV wavelength range and the mechanism of UV pattern formation by unidentified absorbers, which are important for understanding the Venusian climate system. The Venus Climate Orbiter AKATSUKI is a meteorological satellite that has continuously observed atmospheric motion and cloud distribution at multiple altitudes at multiple wavelengths from UV to mid-infrared wavelengths. In this study, UV patterns will be classified by shape, scale, and observed phase angle, and analyze the temporal variation of their albedo, based mainly on the observation data of UVI, which can observe at 283 nm and 365 nm, and the past observation data of Venus Express, in addition to the UV spectral observation by ground-based telescope.
03/03 13:00--14:30 Hline Htet Win
The presentation discusses the integration and testing of Hardware-In- the-Loop simulation so called HIL System LAB using a commercial Flight Simulation software package and a custom design Flight Control System. The Flight Control System for AeroMas UAV is developed and validated using HIL System LAB before flight test. The ability and potential of simulation system are increased significantly when the simulation system is linked directly to the actual flight hardware. The aerodynamic model for AeroMas UAV is built with the help of Plane-Maker program bundled with X-Plane Flight Simulator. X-Plane uses actual flow calculations many times per second to figure out how the given aircraft flies in the simulated environment. By accessing X-Plane state variables through plug-in, the real time avionics sensors data are emulated like an actual way. The X-Planes plug-in communicates with the onboard flight computer throuth USB serial communication. The avionics sensor input data of Flight Control Computer that should be produced by X-Plane are position data of Latitude, Longitude, Altitude, Speed and attitude data of Roll, Pitch, Yaw. The internal design parameters of Flight Control Algorithm can be analyzed and optimized to reduce time and cost effectively during the design phase. Although robust and mature control is not possible, traditional PID control method is used as Flight Control Algorithm to simplify design process and minimize required hardware resource. Monitoring of hardware resource can be possible to observe whether it can response to avionics sensors data efficiently. The development of HIL lab aims to check and refine the hardware implementation through UAV autopilot in long run reliability test. Due to the nature of simplicity and fidelity the HIL System LAB can be deployed as a test platform to assist in the studying of flight control systems at Myanmar Aerospace Engineering University. Over all, the results obtain in this research shown that the effectiveness of HIL System LAB as a Simulated Flight Testing Environment and Educational design tool.
03/10 13:00--14:30 San Lin Phyo
This research focuses on implementation of aerial photo mapping process by using autonomous quad copter. But only how to implement quad copter and aerial photo taking process will be presented in this seminar. The purpose of this research is to apply the autopilot system of quad copter in aerial photography process. Photogrammetry is the science of obtaining reliable information about the properties of surfaces and objects without physical contact with the objects, and of measuring and interpreting this information. The goal of aerial photogrammetry is to obtain the aerial imagery using aircraft, helicopter, hot air balloon, kite or parachute. In this research, quad copter is used as a platform to take aerial photos. At first, quad copter is constructed according to reference design.The type of reference quad copter is STEDIDRONE Q4DX, cross type quad copter. And then, flight test and autopilot test for the constructed quad copter is implemented. After these tests have been implemented and the obtaining results are acceptable, aerial photo taking process is continued. Canon G-15 power shoot camera is used to shoot aerial photos. To get required extra functions for this camera, script program is written. Before writing script program, CHDK firmware is installed on SD card. After installing it, script program is added on CHDK and runs it. APM 2.6 mega board on quad copter is connected with camera by modified USB cable. APM 2.6 mega is released USB (relay) output to camera wherever waypoint which defined to shoot photo. Whenever USB (relay) output is triggered to camera, camera shoots photo. By this way, the desired photos to do mapping are obtained. These photos are composed by using composition software and produced as a map. This research is intended to produce 2-D mapping. In future, 3-D mapping process and image analysis can be continued and extended based on this research.
03/17 13:00--14:30 Ye Min Htay
As the population of the world is increasing, the food supply to customer is more demanding than usual. For this reason, scientist and farmers use precision agriculture to improve the efficiency of the field producing high yields while the inputs is minimizing. Unmanned Aerial Vehicle is trending in precision agriculture field as it reduce the time for scouting the fields and get better accuracy. In this presentation, DJI Phantom 4 Pro is used as a platform to mount the multispectral camera (Micasense-RedgeM). Five Band Camera performs great achievement for crop monitoring in estimation of Leaf chlorophyll, Normalized Difference Vegetation Index (NDVI) and Digital Elevation Model (DEM). From the ground truth, the Near Infrared Band can perform high prediction than visual inspection. Some plants can be seen as green but they tend to weak when the multispectral camera is taken. From the result, we can export the data to farmer or other farm equipment and then, Spraying crops, feeding fertilizers and ground leveling can be done at right place with right time. As a result, we can minimize the environmental pollution such as deteriorating the nitrogen and others gases to the atmosphere and soil erosion.