Table of contents

International Symposium on Sun, Earth, and Life

June 3-4, 2016, East Hall - ITB

Steering Committee

1. Hendra Gunawan (ITB and AIPI, Indonesia)

2. Thomas Djamaluddin (LAPAN, Indonesia)

3. Edy Tri Baskoro (ITB, Indonesia)

4. Premana W. Premadi (ITB, Indonesia)

5. Budi Dermawan (ITB, Indonesia)

6. Nat Gopalswamy (Goddard Space Flight Center, NASA, USA)

7. J. N. Goswami (Physical Research Laboratory, India)

Scientific Committee

1. Ikbal Arifyanto (ITB, Indonesia)

2. Lucky Puspitarini (ITB, Indonesia)

3. Hendra Gunawan (ITB and AIPI, Indonesia)

4. Premana W. Premadi (ITB, Indonesia)

5. Taufiq Hidayat (ITB, Indonesia)

6. Budi Dermawan (ITB, Indonesia)

7. Mahasena Putra (ITB, Indonesia)

8. Dhani Herdiwijaya (ITB, Indonesia)

9. E. Sungging Mumpuni (LAPAN, Indonesia)

10. Clara Y. Yatini (LAPAN, Indonesia)

11. Nat Gopalswamy (Goddard Space Flight Center, NASA, USA)

12. J. N. Goswami (Physical Research Laboratory, India)

13. Thierry Fouchet (Observatoire de Paris, Paris)

Organizing Committee

1. Dhani Herdiwijaya (ITB, Indonesia) - Chair

2. Lucky Puspitarini (ITB, Indonesia)

3. Anny Sulaswatty (AIPI, Indonesia)

4. Indra Noviandri (ITB, Indonesia)

5. Clara Y. Yatini (LAPAN, Indonesia)

6. Abdul Waris (ITB, Indonesia)

7. Mahasena Putra (ITB, Indonesia)

8. Evan Irawan Akbar (ITB, Indonesia)

9. Ikbal Arifyanto (ITB, Indonesia)

10. Aprillia (ITB, Indonesia)

11. E. Sungging Mumpuni (LAPAN, Indonesia)

12. M. Zamzam Nurzaman (LAPAN, Indonesia)

13. Dede Enan (ITB, Indonesia)

International Symposium on Sun, Earth, and Life

June 3-4, 2016, East Hall - ITB

Keynote Speakers

1. Prof. Bambang Hidayat (Indonesian Academy of Sciences)

"A Recollection of Research Merit "

2. Prof. Nat Gopalswamy (Goddard Space Flight Center, NASA, USA)

"The Coronal Connection to Space Weather"

3. Prof. J. M. Pasachoff (Williams College, USA) via Skype

"Coronal Science and Outreach at Recent and Future Solar Eclipses"

4. Prof. J. N. Goswami (Physical Research Laboratory, India)

"Water on the Surface and in the Interior of the Moon"

5. Prof. Thomas Djamaluddin (National Institute of Aeronautics and Space)

"New Timau National Observatory: Accelerating Development of Space Science and Technology in Indonesia"

6. Prof. Taufiq Hidayat (Institut Teknologi Bandung)

"Nitrile Compounds on Titan as Observed by ALMA"

All papers published in this volume of Journal of Physics: Conference Series have been peer reviewed through processes administered by the proceedings Editors. Reviews were conducted by expert referees to the professional and scientific standards expected of a proceedings journal published by IOP Publishing.

Maurice Allais reported anomalous behavior of pendulums, during solar eclipses in 1954 and 1959. This effect, which is then known as the Allais effect, has been searched for by a number of other researchers. Both positive and negative results had been reported. In this paper we report our pendulum experiment during total eclipse on 9 March 2016, over Indonesia. Apparatus set up and method of measurement are described, and we discuss some points which may contribute to uncertainties of the results.

This study was conducted to determine the Earth's surface gravitational acceleration (g) prior to, during, and after a partial solar eclipse. Data was collected in Basic Physics Laboratory Universitas Pendidikan Indonesia, Bandung with coordinates S 6°51'48", E 107°35'40" for three days on March 8 – 10, 2016, in time interval measurement from 6 a.m. to 9 a.m. This research used a standard pendulum, Kater's reversible pendulum, which deviated less than 3° so that the motion can be regarded harmonics oscillation. The period of pendulum oscillation motion is measured by a light sensor (photogate sensor) with accuracy until 10^-13 seconds. The data analysis shows that there is small difference value of gravity acceleration at the Earth's surface from three days of observation, i.e. in the order of 10^-3 ms^-2. It means, there is a changes in the Earth's surface gravitational acceleration (g) due to the partial solar eclipse but not significant.

Since 1950s, several authors have reported the so-called anomalous gravity during the total solar eclipses through various experiments. To address this issue, in the moment of the total solar eclipse of 9 March 2016 passing most regions in Indonesia, we undertook microgravity measurements using two precise gravimeters. The measurements were made at two locations: (1) Poso (central Sulawesi), a location close to the centre passage of the total eclipse and (2) Lembang (West Java), the site of Bosscha Observatory, where the partial solar eclipse occurred. The two sites are selected to measure the possible different influence of the eclipse on aligning the three objects. The measurements were recorded three days before and one day after the eclipse at various intervals from 30 seconds to a short time at 5 seconds. The finer recording was performed several hours before and after the total eclipse. This measurement allowed detailed analysis, not only in time but also in frequency range. A detailed analysis is presented in this paper. We consider all possible geophysical as well as atmospheric effects. The residual data show that the shielding effect, usually thought as responsible factor on anomalous gravity, is not significant.

Spectroscopy observation of solar corona has been carried out from 9th March 2016 Total Solar Eclipse expedition in Maba, East Halmahera. Due to limitation by the weather condition during the observation, the obtained data were not favorable. Because of the low signal to noise ratio, the wavelength calibration was not straightforward. To obtain the optimum results, steps for data reduction were performed as the following: selecting the finest data, extracting the 1D spectrum from 2D spectrum, and calibrating spectrum wavelength (including careful interpolation). In this preliminary result, we discuss the instrumentation, the data under investigation, the extraction process of spectrum, and the polynomial interpolation that has been used for extracting information from our data.

Ludendorff coronal flattening index of the Total Solar Eclipse (TSE) on March 9, 2016, was calculated at various distances in solar radius. As a result, we obtained the coronal flattening index ( = a + b) at a distance of 2 solar radii is 0.16. The 24^th solar cycle phase based on the 2016 TSE event obtained -0.64 which showed the corona is pre-minimum type. Resulted coronal flattening index value gives a predicted maximum amplitude of the monthly sunspot number (W_max) for the 25^th solar cycle to be 70 ± 65. Therefore, the solar activity for 25^th solar cycle predicted to be lower than the current solar cycle, which has a maximum sunspot number value of 146 in February 2014

The March 9^th 2016 total solar eclipse observation was carried out at Universitas Palangkaraya, Central Kalimantan. Time-resolved imaging of the Sun has been conducted before, after, and during totality of eclipse while optical spectroscopic observation has been carried out only at the totality. The imaging observation in white light was done to take high resolution images of solar corona. The images were taken with a DSLR camera that is attached to a refractor telescope (d=66 mm, f/5.9). Despite cloudy weather during the eclipse moments, we managed to obtain the images with lower signal-to-noise ratio, including identifiable diamond ring, prominence and coronal structure. The images were processed using standard reduction procedure to increase the signal-to-noise ratio and to enhance the corona. Then, the coronal structure is determined and compared with ultraviolet data from SOHO to analyze the correlation between visual and ultraviolet corona. The spectroscopic observation was conducted using a slit-less spectrograph and a DSLR camera to obtain solar flash spectra. The flash spectra taken during the eclipse show emissions of H 4861 Å, He I 5876 Å, and H 6563 Å. The Fe XIV 5303 Å and Fe X 6374 Å lines are hardly detected due to low signal-to-noise ratio. Spectral reduction and analysis are conducted to derive the emission lines intensity relative to continuum intensity. We use the measured parameters to determine the temperature of solar chromosphere.

Prominence is a hot gas that consists of electrically charged particles, which is propelled outward Solar surface. It can happen when the activity of sunspot rising up. Ground- based observation of prominence is rather difficult due to the brightness of the Sun, which it needs appropriate method. During total solar eclipse (TSE), prominence is easier to observe. In Ternate, Maluku islands (0°4632.0"N 127°2305.7"E), we observed solar prominence in visual and infrared spectra performed by using regular-DSLR camera for visual wavelength and modified-DSLR (IR-cut filter removal) for infrared wavelength, respectively. Next, we calculated the length of prominence from TSE images, and found that the real minimum length of prominence in red is 1.05 times longer than green and blue ones. And, the real maximum length of prominence is 1.08 times longer than blue and 1.04 times longer than green. The intensity of red is brighter 1.37 times to green and 1.23 times to blue. The causes of the results due to the different temperatures of the prominences and the radiation from H-alpha emission. We succeeded to observe directly the prominence with simple cameras and measured its length and brightness.

We observed the white-light corona during the total solar eclipse of 2016 March 9 from Corong Beach, East Borneo. The solar corona is nearly circular with exception on the southern part of the Sun. Coronal structures are clearly seen. Based on the data, we obtained the Ludendorff flattening index, Nikolsky geometric flattening index, and phases of solar activity (Φ and P) are 0.129, 1.32, -0.716, and 0.573 respectively. Relation between Ludendorff and Nikolsky index, sunspot number, and phases of solar activity were discussed. We also predicted the amplitude of solar cycle 25 to be 196 ± 52 (based on 13-month smoothed monthly data) and 130 ± 42 (based on monthly sunspot number data).

Air temperature, pressure, and wind speed measurements on the surface taken during the Total Solar Eclipse (TSE) of March 9, 2016, are made. They were taken in Terentang Beach, Bangka Island, Indonesia. In this paper, we propose to analyze them by using time series clustering. The following steps are conducted: data collecting, splitting, smoothing, distance calculation, and clustering. The final results show cluster memberships of the three parameters on 3 time frames: one day before, the TSE day, and one day after. After doing some simulations, it can be seen that the profiles of temperature and pressure on the TSE day are on the same cluster while the wind-speed profile on the TSE day is the same as on the one day after.

Observations of the meteorological variables have been conducted in Terentang coastal area, Central Bangka which is located in totality path of Total Solar Eclipse on March 9, 2016. These measurements were made before, during, and after the solar eclipse using a portable automatic weather station with 1 Hz data recording to investigate the influence of total solar eclipse on the incoming solar radiation and other weather variables. Due to the cloudiness at the first phase of the eclipse, the reduction of the radiation was not proportional to the percentage of the solar obscuration. Along with the disappearance of thick clouds, solar radiation changes reach the lowest value from 123 W/m2 to zero point at 5 minutes before the maximum phase. In contrast to the radiation decrement, decreasing air temperature was not comparable to the solar obscuration because it was not only determined by radiation, but also surrounding environment. High relative humidity, on average 89%, was discovered as an effect of the low atmospheric pressure which was affected by the insolation decline. The effect of total solar eclipse can be seen more clearly with spectrum analysis using Fourier transformation to identify periodogram patterns of each meteorology variable. This transformation produced a spectrum's peak totality which is higher than before and after the event on the insolation. The spectrum represents that total solar eclipse has considerable effect to the incoming solar radiation and others which is indicated by the change of the amplitude.

Of all mesoscale phenomena, sea and land breezes have been the most studied, both observationally and theoretically. During the total solar eclipse (TSE), some parameters vary anomalously in response to the occurrence of TSE on 9th March 2016 in Bangka, Indonesia. As it occurred during morning hours, it is considered to be much more significant because of its effect in sea and land breezes pattern, especially in term of lag time. We use Portlog Rainwise Automatic Weather Station which is able to measure data in 1 Hz accuracy. Comparison of hourly observations during first contact until final contact result a slow cooling temperature reduction of 0.1°C until totality phase. A significant weakening in wind speed of about 2.5 ms-1 was observed clearly from the instrument. Unfortunately, the reduction is not coincided with the change of wind direction until the third contact. A near constancy in temperature and the wind's behaviour during TSE result delay time in sea and land breezes pattern after the totality. The lag time occurred in three days measurement data, especially sea breeze onset on the next morning day. The lag time in sea breeze was about one hour retardation. The effect of eclipse on the onset timing of sea and land breeze may be attributed to the proportion of heat accumulation due to the obscuration.

This paper endeavor to describe sky brightness measurements which was carried out by a team of total solar eclipse observers (TOGEMA) on 9^th March 2016. The observations took place at Tarentang Beach, Bangka Island and it utilized the SQM-LU instrument (Sky Quality Meter- USB Connector) with 1 second time interval data. During total phase that lasted about 1 minute 52 seconds, the instrument recorded the brightness of the sky of 12.88 mag/["]² as the dimmest value. This value is approximately 500 times brighter than the dimmest night sky conditions at the same location, obtained on the previous observation. It was found that the brightest sky that could be measured by SQM-LU during Total Solar Eclipse (TSE) 2016 was 5.91 mag/["]². The activity with digital camera also captured the appearance of Venus and Mercury. The appearance of Venus (-3.71 mag) confirmed naked eye limited magnitude theory. This may explain the inability of observers to perceive Mercury (0.46 mag) using naked eye during the total phase of solar eclipse.

Obscuration of the Sun by the Moon during total solar eclipse generates the changing of the sky brightness. Sky Quality Meter (SQM) was employed to measure the sky brightness during the 2016 total solar eclipse. The sky was still bright at the first contact time. It is shown by the SQM value of zero. Approaching the second contact time, the SQM value is rising up started at the value of 5.92 mpsas. The curvature profile of the SQM measurementvalue is similar to the curvature profile of the SQM measurement at the dawn and dusk. However, the flatness part of the curvature is much shorter than night time value of SQM. The maximum of SQM measurement value is lower than the SQM measurement value during the night in Ternate. It is 12.47 mpsas and happened at the maximum phase of the eclipse. It was confirmed by the fact that at the time of totality, the sky close to the horizon was still bright. There is a discrepancy between the predicted and actual second and third contact and maximum eclipse time. By assigning the maximum of SQM measurement value as the reference value of maximum eclipse time, the actual second and third time can be calculated. The shape of curvature between the actual second and third contact time is symmetry.

The total solar eclipse on 9th March 2016 has given a unique opportunity to assess impacts of the eclipse on various meteorological parameters in Ternate. A weather transmitter, a net radiometer, and a heat flux plate for measuring soil heat flux in bare soil were deployed during this special observation in Madaha, Ternate (0°51'17.5" N, 127°20'56.8" E). The measured meteorological parameters presented here are net radiation, air temperature, relative humidity, and soil heat flux. The results show that those parameters are significantly affected by the eclipse. The percentage of the observed decrease of net radiation during the eclipse was proportional to the obscuration percentage. The air temperature measured at 1.5 m declined around 1.9 °C with approximately 11 minutes lag between the mid-eclipse and minimum temperature during eclipse. Influences from the surrounding environment in the measurement site minimize the temperature response. As a consequence of temperature decrease, relative humidity increased. A drop in soil heat flux was also detected but its response was slower.

Total Solar Eclipse (TSE) is a rare natural event in which the positions of Sun, Moon, and Earth are perfectly aligned. In the past by using this phenomenon, many researches have been done to understand characteristic of the corona. In this paper we carried out the study of TSE which crossed over Indonesia from West to East on 9th March 2016. We observed TSE which occured in Palembang (2.9883° S 104.7513° E), Indonesia. The aim of this research is to understand the effect of moon craters on the appearance of solar corona and identification of solar active regions during TSE. This research was done using Canon SX170 IS camera with ND 5 sun-filter. Although the sky was cloudy during the totality of the phase, coronal video was still taken. Camera also took solar images of partial eclipse phase. Coronal images for every frame were then extracted from the video. Image processing of coronal images was done using RegiStax and PhotoScape freewares. To study solar corona, images from Virtual Moon Atlas, Hinode XRT, and SOHO-LASCO were compared with the result of oriented coronal image. Wider and many more moon craters were found having positive correlation with the brighter effect on solar corona as shown at westward coronal streamer. Those craters are represented by Bel'kovich crater, the biggest one. We also found that only the eastward coronal streamer was correlated with active region, sunspot number 12519, from behind solar limb.

Tidal elevation is generating primary by the gravitational forces between earth with moon and solar. Since the sun plays an important role on generating the tidal sea level then the effect of total solar eclipse (TSE) March 9, 2016 on surface water level has been analysed from real time one-minute tide gauge station from Geospatial Information Agency. Two stations was selected to observe the impact of TSE i.e. in coastal of Bangka Island where totally path of TSE was detected and the other is in the coastal Belitung Island, located near to Bangka Island. We compare the observed sea level with the predicted sea level from 9 constituents using Tidal Model Driver (TMD). The result shows that during the TSE in Bangka Island, the observed tidal phase is shifted and observed sea level is higher compare with the prediction one. But in Belitung Island, there is no pattern change of tidal phase and with small increasing sea level compare with the prediction.

The total solar eclipse is an interesting phenomenon because the sun is covered by the moon. This phenomenon is like a night deception for animals, humans, and plants. One of the animals is Bekantan (Nasalis larvatus (Wurmb.)). Nasalis larvatus change its activity when this phenomenon occurs. The aims of the present study are (1) daily activity of Nasalis larvatus on total solar eclipse on March 9^th, 2016 and (2) the effect of total solar eclipse on its activity in Mangrove Center, Kariangau, East Kalimantan. The adlibitum method was used in this study on Bekantan's adult female. The result shows that the total solar eclipse has considerable effect on the daily activity of Bekantan. During total solar eclipse, the activity of Bekantan significantly stopped. When the total solar eclipse finished, Bekantan started its daily activity, and it was indicated by feeding activity which was led by alfa-male.

Our research has been looking for astronomical aspects in Buginese-Makassarese culture from historical to ethnographical sources. We found from history that astronomy had been used by Buginese - Makassar society long before Islam came to South Sulawesi at early 17th century and had their own first telescope at the time of Gowa's Prime Minister, Karaeng Pattingaloang. Meanwhile from ethnographical source, utilization of astronomy penetrated not only at Islamic calendar and worship time, but also at agriculture, sailing navigation, and weather prediction. Some of our literature were taken from Lontaraq (ancient manuscript) which now the experts are not many and old, especially in the field of astronomy. It was found that Lontaraq was using lunar period to characterize local weather [called: Pananrang]. Therefore, we need to excavate immediately more about this matter before the experts reduced in number.

Javanese calendar has several cycles, i.e. 5 days (pasaran), 6 days (paringkelan), 7 days (week), 8 days (padangon and padewan), 30 days (month), and 365 days (year). There is another 210- day cycle caled pawukon which divided into 30 part caled wuku. This cycle originated from an incest tale about a king named Prabu Watugunung which married his mother named Dewi Sinta and his aunt named Dewi Landep. In this marriage they had 27 sons and all of them are called wukus. In this tale it was told that this incestuous relationship caused some havoc in the world and the gods decided to kill this family. After some struggle, all of them are killed and then the gods brought them up to paradise one by one starting from Dewi Sinta and ended with Prabu Watugunung. This ascencion needs 30 weeks (210 days) because to be ascended one wuku had to wait for 7 days, and after one cycle is finished the cycle starts all over again. The establishment of a cycle of pawukon is regarded as an effort to create a cosmos out of chaos (incestuous relationship), and furthermore pawukon is used as a kind of horoscope to determine one"s fate in the future. It is because the cosmos is regarded as a clockwork in which each element of this clockwork works in a predetermined fashion.

The Assembled Solar Eclipse Package (ASEP) is not only an integrated apparatus constructed to obtain imaging data during solar eclipse, but also it involved sky brightness and live streaming requirement. Main four parts of ASEP are composed by two imaging data recorders, one high definition video streaming camera, and a sky quality meter instrument (SQM) linked by a personal computer and motorized mounting. The parts are common instruments which are used for education or personal use. The first part is used to capture corona and prominence image during totality. For the second part, video is powerful data in order to educate public through web streaming lively. The last part, SQM is used to confirm our imaging data during obscuration. The perfect prominence picture was obtained by one of the data capture using William-Optics F=388mm with Nikon DSLR D3100. In addition, the diamond ring and corona were recorded by the second imaging tool using Sky Watcher F=910mm with Canon DSLR 60D. The third instrument is the Sony HXR MC5 streaming set to be able to broadcast to public domain area via official website. From the SQM, the value of the darkness during totality is quiet similar as a dawn condition. Finally, ASEP was entirely successful and be able to fulfil our competency as educational researcher in university.

Tutulemma which stands for tutulma (eclipse) and analemma is a Turkish name to describe analemma which contains solar eclipse. The photographs of analemma which looks like a figure 8 pattern of the solar path in the sky throughout a year is very common. However, this observation is rarely done in low latitude countries, especially tutulemma's plot. Related to the eclipse event on 9 March 2016, we built the first tutulemma in Indonesia which cointains partial solar eclipse observed from the rooftop of LAPAN Bandung office. The purpose of this endeavor is also to understand how the sun moves in one year, particularly at low latitude region based on observation data. We took the picture of the Sun every week at the same time of the day (the time of the eclipse). In this observation, we used a tripod and DSLR camera with a variable ND filter to take the data. To obtain the pattern, the weekly data were combined by image stacking using the same foreground. Finally, we got a figure 8 shaped pattern tutulemma which a bit different from high latitude country ones.

On March 9^th 2016, some regions in Indonesia witnessed the Total Solar Eclipse (TSE). At that time, Indonesia was the only mainland in the world that could observe TSE. This moment is extraordinary because its probability of being observed at the same point happens every 350 years. On a purpose of raising public awareness and engaging more participations, UNAWE Indonesia developed a handy material and sent the so called educational packages which provided essential information about eclipse, especially TSE. Each package contains of modul of TSE study and materials for simple TSE activity so people who received the package could observe TSE safely. In the delivery of this program, we established a collaboration partner, whom are teachers, as an 'eclipse ambassador'. The local partners were responsible for socializing the information for school or their community. We encouraged them to conduct an observation activity and ask them to fill an evaluation report. As a result, 48 out of 59 partners or equal to 81.3% of all partners has sent the evaluation of the package and documentation of the activity during TSE. They responded positively as it was easy to understand, functional, and convenient.

MAGIC (Ma Chung Galactic Club) of Ma Chung University, Malang, is one of the amateur astronomers club who did public outreach and education during the Total Solar Eclipse March 9, 2016. The motivation for doing this was the bad experience during Total Solar Eclipse 1983. At that time the Indonesian government forbid the people to observe the Total Solar Eclipse in a way to avoid blindness. We try to fix this misunderstanding by educating people the safe way to enjoy the partial and total solar eclipse. MAGIC team was divided into two teams, one team went to Palu and did the solar eclipse related education in six high schools before and during the eclipse. The other team did the observation on Ma Chung University campus, Malang, to accompany people who want to see the partial solar eclipse through filtered telescopes. The sky during the solar eclipse was clear both in Malang and Palu. People were very excited and satisfied with the solar eclipse, and their interest to astronomy is increased.

Sorong is located outside the narrow path of total solar eclipse on March 9^th, 2016. The predicted obscuration of the sun was 94.2%. The public outreach to anticipate the solar eclipse was intended to educate students in junior and senior high school in Sorong Regency. Some of them are located in the remote area where the educational materials are difficult to find. The public outreach is unique, since it was run by the local person who is student of physics education. The student has both the ability to explain the solar eclipse phenomenon and able to adapt to knowledge level of students. The materials that were given to the schools are brochure and the eclipse glasses. Beside solar eclipse lectures in class, the pinhole workshop and observation practice were held. The limited materials and resources were faced during the public outreach. However, the enthusiasm was shown by the students and teachers. At least one of the schools held the solar eclipse observation on the day of the eclipse.

Recent developments in personal computing platforms have been revolutionary. With the advent of the Raspberry Pi series and the Arduino series, sub USD 100 computing platforms have changed the playing field altogether. It used to be that you would need a PC or an FPGA platform costing thousands of USD to create a dedicated device for a a dedicated task. Combining a PiCam with the Raspberry Pi allows for smaller budgets to be able to stream live images to the internet and to the public in general. This paper traces our path in designing and adapting the PiCam to a common sized eyepiece and telescope in preparation for the TSE in Indonesia this past March.

The Total Solar Eclipse (TSE) on the 9^th March 2016 received a huge attention from the mass media. Some of them intensively write articles about it even months before the TSE day. As we know media plays strategic role not only in raising public awareness but also interest. The aim of this project is to study the relation between the number of accesses to the media information and how well public learned the information delivered by the media. We prepared questionnaire consisting of seven semi-multiple choices on how public got information about TSE. We gave them choices of what they had heard to measure their basic understanding of TSE. Furthermore we add two "wrong" choices in the last questions to identify less serious respondents. We analyze 60 respondents of Palembang who visited Ampera bridge area. Our result shows no correlation between the number of information access and the level of understanding about TSE. We also found that local media did not provide the scientific content of TSE as well as the national media.

The aim of this research is to detect misconceptions in the concept of physics at high school level by using astronomy questions as a testing instrument. Misconception is defined as a thought or an idea that is different from what has been agreed by experts who are reliable in the field, and it is believed to interfere with the acquisition of new understanding and integration of new knowledge or skills. While lack of concept or knowledge can be corrected with the next instruction and learning, students who have misconceptions have to "unlearn" their misconception before learning a correct one. Therefore, the ability to differentiate between these two things becomes crucial. CRI is one of the methods that can identify efficiently, between misconceptions and lack of knowledge that occur in the students. This research used quantitative- descriptive method with ex-post-facto research approach. An instrument used for the test is astronomy questions that require an understanding of physics concepts to solve the problem. By using astronomy questions, it is expected to raise a better understanding such that a concept can be viewed from various fields of science. Based on test results, misconceptions are found on several topics of physics. This test also revealed that student's ability to analyse a problem is still quite low.

Several two-dimension spherical particles are under influence of gravitational forces of each other and as they are colliding repulsion forces in form of linear spring-dashpot prevent them from collapsed into a single point. Gravitational constant larger than G is used for better and faster stabilization in forming cluster of the particles, accompanied with values of k_N ≈ 10⁴ N/m and yn ≈ 0.5 N·s/m As initial conditions the particles are placed randomly with separation distances among each other. Molecular dynamics method implementing Euler algorithm is used to simulate the developing of particles cluster, which is intending to mimic the process of an asteroid forming. Time step of Δt = 10² s is chosen and results are reported every some period from 1 s to 1000 s, where after each period all particles velocity are forced to be zero. It is observed that not only physical parameters influencing the compaction of the asteroid but also simulation parameters.

We present a study of emission properties and correlations of 3191 type 1 AGN at z < 0.35, selected from Sloan Digital Sky Survey Data Release 12. We supplement the data with ultraviolet spectra from Hubble Space Telescope and International Ultraviolet Explorer along with X-ray properties from Chandra Source Catalog and XMM-Newton Serendipitous Source Catalog and radio measurements from FIRST. We find that the observed spectral diversity of type 1 AGN can be unified by Eddington ratio (L/L_Edd). Objects with higher L/L_Edd tend to have narrower broad Hβ component, strong Ee II emission, systematic blueshift of C IV λ1549, soft X-ray excess, and lower ionization parameter compared to those of the lower L/L_Edd.

Spectroscopic observations in the wavelength range of λλ4000 — 8000 Å of the planetary nebulae (PN), NGC 6543 and NGC 7662, have been undertaken in 2014 using the compact spectrograph attached to the 28-cm Schmidt-Cassegrainian reflector at Koyama Astronomical Observatory. We derived physical parameters of NGC 6543 and NGC 7662 from the analyses of observed emission lines, i.e. electron temperature, density, and elemental abundances. To obtain more reliable physical quantities of NGC 6543 and NGC 7662, the use of photoionization model is needed. We use the computer code, CLOUDY C13.3 to build detailed photoionization models of NGC 6543 and NGC 7662. Model of NGC 6543 and 7662 can be constructed by providing sufficient information on physical parameters of the central stars and the nebula. In this work, input parameters to construct the photoionization model of NGC 6543 and NGC 7662 are distance, temperature and luminosity of central star and nebula parameters. The model results were compared with observational result taken in 2014. Observed and modeled temperatures were deduced from [O III] λλ(4959 + 5007) Å /λ4636 Å and the electron density from [S II] λλ 6716/6731 Å. There are some discrepancies between observed and modeled due to limitations inherent with the resolution and quality of spectroscopic data. Further spectroscopic observations with higher resolution of NGC 6543 and NGC 7662 is recommended.

Stellar open clusters are useful for studying the structure and evolution of Galaxy. Determination of the open cluster members can be viewed from their kinematics: proper motion and radial velocity. It is because the star cluster members will have a motion in the same direction, towards a convergent point. Parametric method with a double elliptic bivariate gaussian function which contains 11 parameters is used as a model of the proper motion distribution. The value of these parameters are determined numerically by cross entropy method. This method is a method of data fitting using the likelihood function whose value is maximized to get the proper parameters. This method solves the problem of determining the initial value that is often difficult to determine in other numerical methods. There are four open clusters which we have analysed: NGC 2244, ASCC 100, NGC 5168, and NGC 2169. The resulting of proper motion parameters of this method matches the parameters in the literature.

Study on the substructures of Milky Way is very important because it can be used as the stage indicator in the formation process of the Galaxy. Substructures are made by clumps of stars with similar velocity, called as stellar streams. We searched for the stellar streams in thick disk and stellar halo of the Milky Way using data from Geneva-Copenhagen survey. We built velocity curves from data and applied the wavelet transform to find dense area in the velocity distribution. For the significace test, peaks on the wavelet transform of the data are reduced using wavelet transform based on Monte Carlo simulation. We found five streams on thick disk and two in stellar halo. Based on the metallicity distribution, it is shown that both thick disk and halo streams have similar range of metallicity, thus we classified them as dynamical stream.

The sky brightness measurements were performed using a portable photometer. A pocket-sized and low-cost photometer has 20 degree area measurement, and spectral ranges between 320-720 nm with output directly in magnitudes per arc second square (mass) unit. The sky brightness with 3 seconds temporal resolutions was recorded at Jogyakarta city (110° 25' E; 70° 52' S; elevation 100 m) within 136 days in years from 2014 to 2016. The darkest night could reach 22.61 mpass only in several seconds, with mean value 18.8±0.7 mpass and temperature variation 23.1±1.2 C. The difference of mean sky brightness between before and after midnight was about -0.76 mpass or 2.0 times brighter. Moreover, the sky brightness and temperature fluctuations were more stable in after midnight than in before midnight. It is suggested that city light pollution affects those variations, and subsequently duration of twilight. By comparing twilight brightness for several places, we also suggest a 17° solar dip or about 66 minutes before sunrise for new time of Fajr prayer.

We constructed global coronal magnetic fields of the Sun during the Total Solar Eclipse (TSE) 9 March 2016 by using Potential Field Source Surface (PFSS) model. Synoptic photospheric magnetogram data from Helioseismic and Magnetic Imager (HMI) onboard Solar Dynamics Observatory (SDO) was used as a boundary condition to extrapolate the coronal magnetic fields of the Sun. This extrapolated structure was analyzed by comparing the alignment of the fields from the model with coronal structure from the observation. We also used observational data of coronal structure during the total solar eclipse to know how well the model agree with the observation. As a result, we could identify several coronal streamers which were produced by the large closed loops in the lower regime of the corona. This result verified that the PFSS extrapolation can be used as a tool to model the inner corona with several constraints. We also discussed how the coronal structure can be used to deduce the phase of the solar cycle.

A total solar eclipse occurred over Indonesia in the morning hours on 9 March 2016. Ionisations in the ionosphere which is associated with the solar radiation during the total eclipse provided a good opportunity to study the ionospheric irregularities. Using global navigation satellite system (GNSS) data taken from dual-frequency receivers in Manado, we investigated and analysed the total electron content (TEC) perturbations with a time resolution of 60 s to reveal ionospheric irregularities during total eclipse. Result showed that TEC conditions based on IPP were decreased during solar eclipse on March 9, comparing with the neighbour day. The maximum percentage deviation (DTEC) from the average value during eclipse period, 00:00 - 02:40 UT reach -41.5%. The duration of maximum decrement in TEC occurs were around 2-30 minutes after the maximum obscuration.

During solar eclipse, solar radiation to the Earth is blocked by the Moon. Thus, the ionization process in the ionosphere is disrupted, as well as the variation of geomagnetic field. The disturbance of geomagnetic field is caused by electric current in the E layer of the ionosphere. At low latitude, the current which is dominant in quiet day is the Sq currents. The blocking of solar radiation cause decrement in electron density in the blocked region. The aim of the research is to find the effect of total solar eclipse to the geomagnetic field. The measurement of the geomagnetic field variation during total solar eclipse on March 9, 2016 was carried out at the Meteorological station of BMKG in Ternate (0° 49' 45.20 "N; 127° 22' 54.00" E). By eliminating the geomagnetic disturbance that occurred in a daily geomagnetic field variation, the pattern of quiet day which is usually in a shape of smooth curve became affected. During the total solar eclipse on March 9, 2016 from 00:30 until 02:00 UT, we found that the geomagnetic field variation of the quiet day decreased by -5 nT.

Ionospheric responses to solar eclipse is interesting to learn. In this paper, we presented ionspheric F2 responses to total solar eclipse on March 9, 2016 over Indonesia from Biak station (-1 °; 136.0 °) which is within the obscuration 86.55%. The total solar eclipse over Biak occurred at 00:58 UT (09:58 local time) in F2 layer height of ionosphere (h ≈ 300 km). Observation of the ionospheric F2 over Biak during the total solar eclipse investigated using ionosonde with 15 minutes resolution. Ionization and recombination processes that occur in the ionosphere proceed by solar radiation. At the time of the ionosphere receives solar radiation, ionization process dominated in the F2 layer. Diurnal ionosphere parameters changed following the solar radiation. During the solar eclipse, the process of ionization in the F2 layer disturbed. Total solar eclipse on March 9, 2016 affected almost simultaneous decrease in maximum electron density (NmF2) ∼52% and increase hmF2 ∼24% at the elapsed time of totality observed from Biak Station.

We report observation and an early analysis of stellar background from total solar eclipse in Ternate, Indonesia. The eclipse phenomena which occurred on March, 9^th 2016 was observed with certain portable instruments in order to obtain the stars behind the Sun in particular field of view and resolution. From our observation site in Ternate city, solar eclipse occurred in the late morning when the weather was unfortunately cloudy. However, during the darkness of totality, we obtained several point source objects between the gaps of the moving clouds and we suspected them as very faint stars due to their appearance in several frames. Those so called stars have been identified and measured with respect to their positions toward the center of the Sun. The main purpose of this research is to revisit strong lensing calculation of the Sun during total solar eclipse by measuring the deflection angle of the background stars as it had been calculated by Einstein and proved by Eddington at a total solar eclipse in 1919. To accomplish this aim, we need to conduct another observation to measure position of the same stars in the next period when those stars appear in the night sky.

The phenomenon of solar and lunar eclipses can be predicted where and when it will happen. The Total Solar Eclipse (TSE) phenomenon on March 09th, 2016 became revival astronomy science in Indonesia and provided public astronomy education. This research aims to predict the total solar eclipse phenomenon from 2016 until 2100. We Used Besselian calculations and Meeus algorithms implemented in MATLAB R2012b software. This methods combine with VSOP087 and ELP2000-82 algorithm. As an example of simulation, TSE prediction on April 20th, 2042 has 0.2 seconds distinction of duration compared with NASA prediction. For the whole data TSE from year of 2016 until 2100 we found 0.04-0.21 seconds differences compared with NASA prediction.

The observation of the partial solar eclipse in Bandung on March, 9th 2016 was done to measure the surface coverage area and to compare to NASA calculation. We have calculated solar disk coverage area based on image data at the maximum contact until final contact of the eclipse. We obtained that maximum eclipse was at 7:21 a.m. (UT+7) with 84.81% area of solar disk covered by Moon and the end of eclipse was at 8:31 a.m. (UT+7).

One way to introduce astronomy to public, including students, can be handled by solar observation. The widely held device for this purpose is coelostat and heliostat. Besides using filter attached to a device such as telescope, it is safest to use indirect way for observing the Sun. The main principle of the indirect way is deflecting the sun light and projecting image of the sun on a screen. We design and build a simple and low-cost astronomical device, serving as a supplement to increase public service, especially for solar observation. Without using any digital and intricate supporting equipment, people can watch and relish image of the Sun in comfortable condition, i.e. in a sheltered or shady place. Here we describe a design and features of our prototype of the device, which still, of course, has some limitations. In the future, this prototype can be improved for more efficient and useful applications.

The 2016 Total Solar Eclipse provided us an opportunity to introduce astronomy to a much wider audience. The path of totality crossed the Indonesia from Sumatra to the Maluku Islands and ended its journey in the Pacific Ocean. Its path crossed over 4 major islands, 12 provinces and many cities. Most of the cities have minimum exposure to astronomy. langitselatan travelled to observe the eclipse and to do astronomy outreach at the eastern most island under the eclipse path. We chose Maba, a small village in East Halmahera, North Maluku as our site to observe the eclipse as well as conduct a workshop for teachers and students. The aim of the workshop is to introduce astronomy taking advantage of the eclipse as well as raise awareness and curiosity among students. In this paper, we will share a short report regarding the whole trip and event in Maba.

Viewing astronomy objects from space is superior to that from Earth due to the absence of terrestrial atmospheric disturbances. Since decades ago, there has been an idea of building gigantic spaceships to live in, i.e., low earth orbit (LEO) settlement. In the context of solar eclipse, the presuming space settlements will accommodate future solar eclipse chasers (amateur or professional astronomers) to observe solar eclipse from space. Not only for scientific purpose, human personal observation from space is also needed for getting aesthetical mental impression. Furthermore, since space science indirectly aids solar eclipse observation, we will discuss the related history and development of Indonesian space experiments. Space science is an essential knowledge to be mastered by all nations.

The path of Total Solar Eclipse (TSE) on March 9^th 2016 passed through several cities in Indonesia and one of them is Palangkaraya, Central Kalimantan. The TSE natural phenomenon provided a special moment and gave unforgettable and lifelong experiences for children who live in Palangkaraya. Some miss-information and a bad impression can be felt by children who do not understand about TSE that causes momentary darkness during totality phase. Therefore we designed a children education programs about the TSE that as follow: (1) socialization about TSE, (2) Popular astronomy seminar, (3) How to observe the Sun? (4) writing competition about TSE and (5) TSE observation. The events were held on March 8^th - 9^th 2016. More than 200 representatives of elementary school students and teachers throughout Palangkaraya have actively participated. The keynote speaker was an Indonesian expert astronomer with help from alumni of astronomy olympiad in order to provide inspiration for the participants, especially to the students. We conclude that students as young generation of the nation may have more motivation to work in science by direct learning from natural phenomena.

The objective of the research was to determine the effect of microgravity simulation by 3D clinostat on Cavendish banana (Musa acuminata AAA group) ripening process. In this study, physical, physiological changes as well as genes expression were analysed. The result showed that in microgravity simulation condition ripening process in banana was delayed and the MaACOl, MaACSl and MaACS5 gene expression were affected.

Several research showed that space flown treated seeds had a different characteristic with that of ground treated seed, which eventually produced a different characteristic of growth and productivity. Research was conducted to study the physical, chemical and biological properties, such as the rate of germination and the growth of tomato (Lycopersicum esculentum) space flown seeds compared with that of control one. Observations of physical properties using a SEM showed that there were pores on the surface of some tomato space flown seeds. Observations using a stereo and inverted microscope showed that the coat layer of space flown seeds was thinner than control seeds. The total mineral content in the control seeds (22.88%) was averagely higher than space flown seeds (18.66%), but the average carbohydrate content in control seed was lower (15.2 ± 2.79%) than the space flown seeds (9.02 ± 1.87%). The level of auxin (IAA) of control seeds (142 ± 6.88 ppm) was averagely lower than the space flown seeds (414 ± 78.84 ppm), whereas the level of cytokinins (zeatin) for the control seeds (381 ± 68.86 ppm) was higher than the space flown seeds (68 ± 9.53 ppm), and the level of gibberellin (GA3) for the control seeds (335 ± 10.7 ppm) was higher than the space flown seeds (184 ± 7.4 ppm). The results of this study showed that the physical and chemical properties of tomato space flown seeds were generally different compare with that to control seeds, so that it might also be resulted in different germination and growth characteristic. The germination test showed that space flown seeds had lower germination rate compare to control. The growth pattern indicated that planted space flown seeds generally grew better than control. However, those data were more homogenous in control seeds compare to that in space flown tomato seeds.

Koren-Feingold (KF) model, a model that relates growth of cloud thickness (H) and cloud number concentration (N) is discussed and analyzed in this work. Two boundary conditions are required by this model, where the first is cloud thickness potential H₀ and the second is aerosol concentration N₀. The initial conditions are simply H(0) = 0 and N(0) = 0. Several pairs of (H₀, N₀) values are chosen in calculating the precipitation. Three categories of rainfall are used in this work, which are no drizzle D0, light drizzle D1, and drizzle D2. As H evolves in time t, it produces maximum cloud thickness H_max and saturation cloud thickness H_sat, as also N does N_max and N_sat. Two kinds of cloud thickness difference, ΔH₁ = H₀ - H_max and ΔH₂ = H₀ - H_sat are proposed and also for cloud concentration difference ΔN₁ and ΔN₂ with similar definitions. Pairs of (ΔH₁, ΔN₁) and (ΔH₂, ΔN₂) are used in analyzing simulation results. The first pair can be used as prediction of rainfall occurrence, while the second pair is more for confirmation and understanding the relation between cloud thickness and cloud concentration in producing rainfall. It is observed that H < H₀ and N < N₀ are always fulfilled. Rainfall in category D2 will have significant differences in H and N, while in category D0 will not. Typical differences for H are about 80% and 30-50% for both cases. Deeper discussion about (ΔH₁, ΔN₁) and (ΔH₂, ΔN₂) is presented in this work.

Islamic prayer times are based on the astronomical position of the Sun in the sky. One of them is the Fajr prayer. It is marked by some indicators in the morning twilight which is white light spread in the Eastern horizon. However, determining the true time of twilight can be difficult. One of the reasons is the effect of atmospheric humidity to the appearance of morning twilight. The higher the humidity, the redder twilight sky appearance. This paper discusses this effect. It is shown that despite of the same Sun's position, sky color can vary considerably. Observations of various solar dip angle have been made to study this effect. Visibility for different angle can change accordingly. We obtained that the average solar dip for Fajr prayer by morning twilight images was -18°39'29.4".

High altitude clouds have been observed in the Martian atmosphere. However, their properties still remain to be characterized. Mars Climate Sounder (MCS) aboard Mars Reconnaissance Orbiter (MRO) is an instrument that measures radiances in the thermal infrared, both in limb and nadir views. It allows us to retrieve vertical profiles of radiance, temperature and aerosols. Using the MCS data and radiative transfer model coupled with an automated inversion routine, we can investigate the chemical composition of the high altitude clouds. We will present the first results on the properties of the clouds. CO₂ ice is the best candidate to be the main component of some high altitude clouds due to the most similar spectral variation compared to water ice or dust, in agreement with previous studies. Using cloud composition of contaminated CO₂ ice (dust core surrounded by CO₂ ice) might improve the fitting result, but further study is needed.

Asteroid collisions and cometary outgassing produce grains and dust that cause to fill the interplanetary space. The particles are temporarily trapped into orbit of the Earth to develop a circumsolar dust ring. The ring encloses the Sun-Earth equilateral triangular libration points in terms of Restricted Three-Body Problem (RTBP). On the other hand, regions close to the triangular points are preferable as locations for placing astronomical satellite. Here we study the planar-circular RTBP of Sun-Earth system with considers the oblateness of Earth and the presence of a circumsolar dust ring. Perturbation of the dust ring on linear stability of the points is discussed and we find that the points are still stable. However, in general the presence of the circumsolar (resonant) dust ring decreases value of the critical mass parameter.

Many exoplanetary systems have been found to harbour more than one planet. Some of them have commensurability in orbital periods of the planets (resonant-planet pair). The aim of this work is to analyse the stability of resonant-planet pair configuration in two multiexoplanetary systems which have two planets in near mean-motion resonances, i.e. Kepler- 9 and HD 10180 systems. This work considers numerical and comparative empiric-analytical studies. Numerical studies are performed using the integrator package SWIFT with an integration time of 10 Myr. Results from numerical integrations indicate that all orbital solution sets of the systems are stable. Further numerical explorations also demonstrate that the systems are stable for small perturbations in the orbital elements and mass variations. Analyses of stability based on comparative empiric-analytical are done by applying a known stability criterion to all systems. We find that all systems tend to be stable.

The Restricted Three-Body Problem (R3BP) considers motion of a third infinitesimal object under the gravitational influences of the primaries (bigger and smaller massive bodies) whose orbits are around the center of mass. If the orbits are elliptical, this belongs to Elliptic R3BP (ER3BP). In planar case it possesses five equilibrium points consisting of three collinear (L₁, L₂, and L₃) and two triangular (L₄ and L₅). To mimic a better astrophysical R3BP, such as motion of a satellite in star-planet system, the classical problem can be generalized by considering the effects of radiation pressure and oblate spheroid shape on the primaries. We study analytically the locations and the stability of L₄ and L₅ equilibrium points in the frame of ER3BP with incorporating the effects of radiation for bigger primary and oblateness for smaller primary. Our study suggests that the oblateness factor (A₂) and the radiation factor (q₁) shift the positions of L₄ and L₅ points compared with the classical ones. We also find that there is a stability limit for motion of the third body around these points.

We present the new result of our investigation on the extraction of proton radius and the impact of different proton radii on the radius of neutron star, after correcting the mistake in the previous calculation of the proton radius. The new value of the extracted proton radius is 0.864 fm. The effect of this correction on the calculated neuron star radius is trivial.

The spectral evolution of the Nova V5668 Sgr has been observed on 12 June, 23 June, and 15 August 2015 using NEO-R1000 spectrograph attached to the C-11 telescope at Bosscha Observatory, Lembang, Indonesia. The observed spectra indicate that the nova has been entering the nebular phase. The spectra during this phase showed strong forbidden lines of [O I] λ6300, 6364, [O II] λ7320, and [O III] λ5007, [N II] λ5755. The spectra also showed emission line of Fe II λ4924, 5169, 5317, 6149. We classify Nova V5668 Sgr into the Fe II type. We present and discuss the variation of nebular abundance N(X)/N(H) of the Nova V5668 Sgr in the light of its evolutionary stages.

Bubble Nebula is a bubble formed by the interaction between the stellar wind of BD+60°2522 with ambient interstellar gas. We use a web-based stellar evolution code, the EZ- web, to construct the evolution of BD+60°2522. From the evolution, we obtain the age of the system needed for the interstellar bubbles model. Then from the model, we determine parameters such as radius, expansion velocity, luminosity, temperature, and density of the Bubble.

A type I supemovae (SN Ia) is an exploding white dwarf, whose mass exceeds Chandrasekar limit (1.44 solar mass). If a white dwarf is in a binary system, it may accrete matter from the companion, resulting in an excess mass that cannot be balanced by the pressure of degenerated electrons in the core. SNe Ia are highly luminous objects, that they are visible from very high distances. After some corrections (stretch (s), colour (c), K-corrections, etc.), the variations in the light curves of SNe Ia can be suppressed to be no more than 10%. Their high luminosity and almost uniform intrinsic brightness at the peak light, i.e. M_B ∼ -19, make SNe Ia ideal standard candle. Because of their visibility from large distances, SNe Ia can be employed as a cosmological measuring tool. It was analysis of SNe Ia data that indicated for the first time, that the universe is not only expanding, but also accelerating. This work analyzed a compilation of SNe Ia data to determine several cosmological parameters (H₀, Ω_m, Ω_a, and w). It can be concluded from the analysis, that our universe is a flat, dark energy dominated universe, and that the cosmological constant A is a suitable candidate for dark energy.

Ultraluminous X-ray sources (ULXs) are defined as non-nuclear point-source objects with apparent X-ray luminosities, Lx > 2×10³⁹ erg s^-1, in the 0.3-8 keV band. ULXs are often explained using two different scenarios, (1) ULXs as intermediate mass black hole (IMBH) with sub-Eddington accretion and (2) ULXs as stellar mass black hole with super-Eddington accretion. There are two methods that commonly used to study the characteristics of ULXs. One method is to study the X-ray spectra of ULXs, to determine the characteristics of their accretion flows from fitting their spectra using available spectral models. The other method is to investigate how population of ULXs correlate with their environment, in this case their host galaxies. Our goal is to find correlation between ULXs and the properties of its host galaxies, for example with Star Formation Rate (SFR), mass and morphology. From this study we found a positive correlation between ULXs number and SFR. From X-ray luminosity function, we found upper limit of black holes mass that power ULXs is about 100 M⊙.