Ms
Sirinapa Arjyotha
(Program of Physics, Faculty of Science and Technology, Chiang Rai Rajabhat University, Chiangrai, Thailand 57100)
5/21/15, 8:00 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Cataclysmic Variables (CVs) are close binaries consisting of an accreting white dwarf and a low-mass main sequence companion. We have initiated in searching new CVs using their outburst properties with the primary aim to identify short-period systems which are rare but are great of importance to understand close binary evolution. Here, we present time-resolved photometry of new CVs in...
Dr
David Mkrtichian
(National Astronomical Research Institute of Thailand, Chiang Mai 50200, Thailand)
5/21/15, 8:15 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We present results of study of oscillation of a sample of A-type mass-accreting components of Algol-type eclipsing binary stars (so called oEA stars). This work is a part of ongoing THAi Southern Survey for OEA Stars (THASSOS). High-precision photometry obtained at different observatories was used to investigate the low-amplitude acoustic variations of brightness of primary components. The...
Mr
Khunagorn Chanthorn
(School of Physics, Institute of Science, Suranaree University of Technology, Nakhon Ratchasima 30000, Thailand)
5/21/15, 8:30 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We followed up the new eclipsing white dwarf main sequence SDSS J102102.25+174439.9 with a short orbital period of 0.14 days from the Sloan Digital Sky Survey The system has been observed by using on the 2.4m telescope at the Thai National Observatory (TNO) with ULTRASPEC instrument. Our multi-band observations shows peculiar dips about 15 minute after the primary eclipse. Such dips in WDMS...
Mr
Kittipong Wangnok
(School of Physics, Institute of Science, Suranaree University of Technology, Nakhon Ratchasima 30000, Thailand)
5/21/15, 8:45 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Post common-envelope binaries (PCEBs) are known as one of the end products of the complex common-envelope process. These systems typically consist of white dwarf star with a low mass companion. While most of PCEBs usually have short orbital periods of a few hours, some systems are found to be in long (>1 day) period. In this work, we present the preliminary result of our follow-up photometric...
Ms
Sawatkamol Pichadee
(Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50200, Thailand)
5/21/15, 9:00 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
GJ3470b is a Uranus-mass exoplanet, orbiting around M dwarf (Bonfils et al. 2012). In this work, R-filter transit observations were conducted by using the 0.5-meter telescope at Thai National Observatory (TNO) and the 0.6-meter telescope at Cerro Tololo Inter-American Observatory (CTIO) in 2013-2015. From the light curves, the orbital elements of GJ3470b were obtained. In addition, the time of...
Mr
Lunchakorn Tannukij
(Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400, Thailand)
5/21/15, 9:15 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Massive gravity is one of the well-known modification of Einstein’s general relativity by promoting the massless mediator, so-called graviton, to be a massive one. As the modified gravity, it is natural to consider the black hole solution of the theory. Here we present the static spherically symmetric black hole solution in massive gravity, proposed by de Rham, Gabadadze, and Tolley, along...
Mr
Supakorn Saelue
(Department of Physics, Faculty of Science, Chulalongkorn University, Bangkok, THAILAND 10330)
5/21/15, 9:30 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We attempt to explain the trajectory of a particle around the massive object using an effective gravitational potential obtained from dRGT massive gravity theory. The dRGT massive gravity is the modification of the Einstein’s general relativity (GR) by considering theory with a massive graviton, while in GR the graviton is massless. We start with finding the static and spherically symmetric...
Mr
Orarik Tasuya
(Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50200, Thailand)
5/21/15, 9:45 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We present a study of star formation, stellar age and metallicity, and interactions between galaxies in a low-redshift group, NGC 4065 group. Imaging data were taken from 2.4 meter telescope at Thai National Observatory (TNO) for B, V and R$_\mathrm{C}$ broadband filters and [S$~\small{\mathrm{II}}$] and Red-continuum narrowband filters. There are 21 galaxies in our sample. The star formation...
Mr
Bovornpratch Vijarnwannaluk
(Department of Physics, Faculty of Science, Chulalongkorn University, Bangkok 10330 , Thailand)
5/21/15, 10:00 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We report the ongoing variability monitoring program for a well-defined, flux-limited sample of active galactic nuclei (with Bj<18 mag) through a multi-band optical imaging using Thailand's 0.6-m remotely-operated telescope at Cerro Tololo Inter-American Observatory, Chile. Our goal is to search for month-time scales outbursts to identify potential targets for spectroscopic follow-up to...
Mr
Anut Sangka
(School of Physics, Institute of Science, Suranaree University of Technology, Nakhon Ratchasima 30000, Thailand)
5/21/15, 10:15 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
One of the strongest evidence of the currently favoured standard ΛCDM (Lambda cold dark matter) model with the Big Bang origin came from the Cosmic Microwave Background (CMB) radiation measurement which show us the average temperature of the universe is 2.725 K with the Gaussian fluctuations of about 18 µK RMS. However there presents some anomalies that can be observed by CMB experiment. One...
Dr
Manzoor Ahmad Malik
(Department of Physics, faculty of Physical and Material Sciences, University of Kashmir, Srinagar 190006, India)
5/21/15, 10:30 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Cluster expansion method of statistical mechanics has proved to be a useful tool in describing gravitational galaxy clustering as a cosmological many body problem. The method yields a spatial galaxy distribution function, a generalized Poisson, in excellent agreement with observations and N-body simulation results. Some recent developments include distribution function for a multi component...
Rak Chitchamnong
(Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400 Thailand)
5/21/15, 10:45 AM
Astronomy, Astrophysics, and Cosmology
Oral presentation
The rotation curve of the visible stars and gas in a galaxy can be presented by plotting its orbital velocity. However the galaxy rotation curve obtained by using the relation of Newton’s universal gravitation fails to explain the observed rotation curve. This has led to the dark matter hypothesis. At present there is no direct evidence for the detection of dark matter and the area is still...
Ms
Tatphicha Promfu
(Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50200, Thailand)
5/21/15, 1:00 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Io magnetic footprint (IFP) is a result of interaction between Jovain magnetosphere and Io. Due to Jupiter’s fast rotation in comparison with Io, magnetospheric plasmas collide with atmospheric particles of Io at high speeds. Therefore the interaction region expands into an extended area behind Io. As a result, aurora spot is extended into a tail-like structure. This research study factors...
Dr
Suwicha Wannawichian
(Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50200, Thailand)
5/21/15, 1:15 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
FUV images of Jupiter’s auroral region have been taken since the early observational era of the Hubble Space Telescope (HST). In the vicinity of the main auroral oval, an emission spot was detected and appeared to be evidence of electromagnetic interaction between Jupiter’s magnetospheric plasma and Io’s atmosphere. In previous works, the brightness of this emission, which is called Io’s...
Dr
Alejandro Sáiz
(Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400 Thailand)
5/21/15, 1:30 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
The Princess Sirindhorn Neutron Monitor (PSNM) has operated since late
2007 at the summit of Doi Inthanon, Thailand's highest mountain, in
Chiang Mai province. PSNM records the flux of galactic cosmic rays
(GCRs) impinging on Earth's atmosphere, as well as the GCR flux
variations with time due to solar activity. PSNM has the world's
highest cosmic ray vertical cutoff rigidity...
Dr
Pierre-Simon Mangeard
(National Astronomical Research Institute of Thailand, Chiang Mai 50200, Thailand)
5/21/15, 1:45 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Neutron monitors (NMs) are large ground-based instruments for precise time tracking of the variations in the Galactic cosmic ray (GCR) flux at GeV-range. NMs are counting the secondary particles (mostly neutrons) issued from the interaction of the cosmic rays in the atmosphere. The sensitivity to GCR variations depends on the geomagnetic cutoff at the location of measurement. Since late 2007,...
Dr
Warit Mitthumsiri
(Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400 Thailand)
5/21/15, 2:00 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Ionizing radiation in the Earth’s troposphere is mainly due to Galactic cosmic rays, high-energy particles from outside the Solar System. Typical solar energetic particles do not have enough energy to penetrate to aircraft or cloud altitudes. However, occasionally solar storms can produce relativistic ions with such enormous intensity that their ionization effect in the Earth’s lower...
118.
Overcoming the Seeing Limitations at 2.4-m Thai National Telescope with Lucky Imaging Technique
Rattanawadee Tekavong
(Department of Physics, Faculty of Science, King Mongkut's University of Technology Thonburi, Bangkok, Thailand 10140)
5/21/15, 2:15 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Resolving power of large telescopes is limited by seeing condition, the blurring due to the Earth's atmospheric turbulence. This limits the capability of large telescopes, including the 2.4-m diameter Thai National Observatory (TNO) in Chiang Mai, Thailand, from reaching its fullest resolving power. We present an effort to overcome this limitation through the ‘Lucky Imaging' technique, which...
Dr
Tiberiu Harko
(Department of Mathematics, University College London, Gower Street, London WC1E 6BT, United Kingdom)
5/21/15, 2:30 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We consider the possibility that the dark matter, which is required to explain the dynamics of the neutral hydrogen clouds at large distances from the galactic center, could be in the form of a Bose-Einstein condensate. To study the condensate we use the non-relativistic Gross-Pitaevskii equation. By introducing the Madelung representation of the wave function, we formulate the dynamics of the...
Dr
Matthew Lake
(The Institute for Fundamental Study, Naresuan University, Phitsanulok 65000, Thailand)
5/21/15, 2:45 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
We outline a model of abelian-Higgs strings with variable scalar and vector core radii.
In general, the functions determining the time and position-dependent core widths may be
expressed as arbitrary left or right movers, of which the usual constant values are a particular solution. In this case the string may carry momentum, even if the embedding of its central axis remains fixed, and the...
Wirin Sonsrettee
(Faculty of Engineering and Technology, Panyapiwat Institute of Management, Nonthaburi 11120, Thailand)
5/21/15, 3:00 PM
Astronomy, Astrophysics, and Cosmology
Oral presentation
Most of the field line random walk (FLRW) theories proposed in the past were strongly influenced by studies of the limit of weak fluctuations. In this limit, the behavior of the FLRW can be characterized by the Kubo number $R=(b/B_0)(\ell_\parallel/\ell_\perp)$, where $b$ is the root mean squared fluctuation, $\ell_\parallel$ and $\ell_\perp$ are turbulence coherence scales parallel and...
