• 천문학논총
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• 제30권2호
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• pp.679-682
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• 2015

The Hiroshima Astrophysical Science Center (HASC) was founded in 2004 at Hiroshima University, Japan. The main mission of this institute is the observational study of various transient objects including gamma-ray bursts, supernovae, novae, cataclysmic variables, and active galactic nuclei by means of multi-wavelength observations. HASC consists of three divisions; the optical-infrared astronomy division, high-energy astronomy division, and theoretical astronomy division. HASC is operating the 1.5m optical-infrared telescope Kanata, which is dedicated to follow-up and monitoring observations of transient objects. The high-energy division is the key operation center for the Fermi gamma-ray space telescope. HASC and the high-energy astronomy group in the department of physical science at Hiroshima University are closely collaborating with each other to promote multi-wavelength time-domain astronomy. We report the recent activities of HASC and some science topics pursued by this multi-wavelength collaboration.

• 천문학회보
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• 제46권1호
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• pp.52.1-52.1
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• 2021

We present the results of multi-epoch, multi-frequency monitoring of a blazar 4C +29.45, which was regularly monitored as part of the Interferometric Monitoring of GAmma-ray Bright AGNs program - a key science program of the Korean Very long baseline interferometry Network (KVN). Observations were conducted simultaneously at 22, 43, 86 and 129 GHz during the 4 years from December 2012 to December 2016. We also used additional data from the 15 GHz Owens Valley Radio Observatory (OVRO) monitoring program. From the 15 GHz light curve, we estimated the variability time scales of the source during several radio flux enhancements. We found that the source experiencesd 6 radio flux enhancements with variability time scales of 9-187 days during the observing period, yielding corresponding variability Doppler factors of 9-27. From the multi-frequency simultaneous KVN observations, we were able to obtain accurate radio spectra of the source and hence to more precisely measure the turnover frequencies 𝜈_r of synchrotron self-absorbed (SSA) emission with a mean value of ${\bar{\nu}_r}=28.9GHz$. Using jet geometry assumptions, we estimated the size of the emitting region at the turnover frequency. Taking into account these results, we found that the equipartition magnetic field strength is up to two orders of magnitudes higher than the SSA magnetic field strength (0.6-99 mG). This is consistent with the source being particle dominated.

• 천문학회보
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• 제39권2호
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• pp.37-37
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• 2014

Magnetic fields appear to be ubiquitous in astrophysical environments. The existence of magnetic fields in the large-scale structure of the universe has been established through observations of Faraday rotation and synchrotron emission, as well as through recent gamma-ray observations. Yet, the nature and origin of the magnetic fields remains controversial and largely unknown. In this talk, I briefly summarize recent developments in our understanding of the nature and origin of magnetic fields. I also describe a plausible scenario for the origin of the magnetic fields; seed fields were created in the early universe and subsequently amplified during the formation of the large-scale structure of the universe. I then discuss the prospect of observation of magnetic fields in the large-scale structure of the universe.

• 천문학회보
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• 제41권1호
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• pp.61.1-61.1
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• 2016

As a new way to explore the universe, astronomers are now performing time-domain astronomy by surveying the universe looking for new transient phenomena and taking movies of the universe with telescopes. Large-area, time-series survey of astronomical objects are uncovering many interesting, fast-changing objects that have now been poorly understood before, such as GRBs, tidal disruption phenomena, and new types of supernova. In order to characterize these new, exciting events, it is very critical to perform follow-up observations, and 1-2m telescopes can effectively contribute to such efforts. Since 2007, our group has been performing follow-up observations of gamma-ray bursts (GRBs) and interesting transients using BOAO and other KASI facilities. Here, we present results from several key transient studies that were done by using BOAO: (1) tidal disruption event Swift J1644+57; (2) SN 2011fe that occurred in M101; and (3) several GRB events. These study demonstrates the usefulness of BOAO as a powerful transient follow-up facility. Finally, we will discuss how BOAO research activities can possibly be bolstered in this newly emerging field of astronomy.

• 천문학회보
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• 제40권2호
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• pp.38.1-38.1
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• 2015

Supernova remnants (SNRs) are one of the most energetic astrophysical events and are thought to be the dominant source of Galactic cosmic rays (CRs). A recent report on observations of gamma rays from the vicinity of SNRs have shown strong evidence that Galactic CR protons are accelerated by the shock waves of the SNRs. The actual gamma-ray emission from pion decay should depend on the diffusion of CRs in the interstellar medium. In order to quantitatively analyze the diffusion of high-energy CRs from acceleration sites, we have performed test particle numerical simulations of CR protons using a three-dimensional magnetohydrodynamics (MHD) simulation of an interstellar medium swept-up by a blast wave. We analyse the CRs diffusion at a length scale of order a few pc, and show the Richtmeyer-Meshkov instability can provide enough turbulence downstream of the shock to make the diffusion coefficient close to the Bohm level for energy larger than 30 TeV for a realistic interstellar medium.

• Journal of Astronomy and Space Sciences
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• 제22권4호
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• pp.377-384
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• 2005

감마선 폭발체는 1973년 처음으로 알려진 후 현재까지 많은 과학자들에 의해 연구되고 있다. 짝은 지속 기간을 가진 감마선 폭발체에 비해 비교적 긴 시간 척도를 가진 잔유휘광의 분광 분석자료는 감마선 폭발체 생성 환경 연구에 중요한 정보를 제공한다. 그러나, 모든 감마선 폭발체에서 모든 영역의 잔유휘광이 관측되는 것은 아니다. 전파나 엑스선 영역의 잔유휘광 관측 불능은 검출기나 광대역 모니터의 한계로 인한 문제로 보고 있으며, 광학 잔유휘광 관측 불능은 광원내부 또는 소속 은하내의 먼지 그리고 성간 매질의 흡수에 의한 것으로 보고 있다. 우리는 이러한 잔유휘광이 관측되지 않은 경우에 대해 의문을 가지고, 광학 관측으로 거리가 정해진 감마선 폭발체의 거리에 따른 에너지 영역별 잔유휘광 개수 분포를 비교 분석해 보았다. 그 결과 우리는 엑스선 잔유휘광이 관측된 감마선 폭발체들이나 광학 잔유휘광이 관측된 감마선 폭발체들의 거리 분포가 같다는 것을 알 수 있었다. 이같은 결과로부터 우리는 광학 잔유휘광이 성간 물질에 의한 소광으로 관측되지 않을 수 있다는 이론은 타당치 못하다는 결론을 주장해 본다.

• 한국버섯학회지
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• 제21권4호
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• pp.247-253
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• 2023

본 연구는 감마선을 조사한 목이의 변이 양상을 균사 생장 조사, 자실체 수량 및 생육특성 조사, 자실체의 맛, 향 그리고 구성물질 분석을 통해 확인하였다. 감마선 세기에 따른 균사 생장을 조사한 결과 200 Gy처리구에서 가장 우수하였다. 자실체의 수량 또한 200 Gy에서 가장 높았으며, 다음으로 800 Gy와 control이 대등하게 나타났다. 이를 기반으로 200 Gy와 800 Gy를 우수한 특성을 가진 처리구로 선발하였고, 이들을 대상으로 물질분석을 진행하였다. 자실체의 맛 패턴을 비교했을 때, control과 200 Gy, 그리고 800 Gy가 비슷하게 나타났다. 향기 패턴을 비교한 결과 200 Gy가 control 및 처리구와 다른 양상을 보였다. 선발된 처리구들과 control간의 총 식이섬유 함량을 비교했을 때 큰 차이를 확인할 수 없었다. 칼슘과 아연의 함량을 확인했을 때 칼슘 함량은 800Gy, 아연은 200Gy처리에서 높아, 감마선 처리에 따라 함량이 다르게 나타났다. 따라서 감마선 조사는 목이 수확량을 늘리고 칼슘과 아연의 함량을 향상시킬 수 있다.

• 천문학회보
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• 제35권2호
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• pp.36.2-36.2
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• 2010

CQUEAN (Camera fo QUasars in EArly uNiverse) is a newly developed camera by CEOU for the 2.1m telescope at the McDonald Observatory, Texas, USA. We report the early science results from the commissioning run of CQUEAN which include the observations of the gamma-ray burst (GRB) afterglows and quasars at z ~ 5.5. Although the data were originally taken to test the instrument performance, the results are already very encouraging. We uncovered GRB afterglows at z = 0.8 - 1.4, with our data being used for the international collaboration research to understand the nature of GRBs. The unique filter sets we employed are providing the data which are effective for selecting quasars at z ~ 5.5. The special aspects of CQUEAN - high sensitivity at 0.8-1.1 ${\mu}m$ and fast readouts - will allow us to produce many interesting through surveys of high redshift quasars and fast follow-up of transient objects such as GRBs and exoplanets in future.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2005년도 한국우주과학회보 제14권1호
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• pp.34-34
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• 2005

• Journal of Radiation Protection and Research
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• 제47권1호
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• pp.16-21
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• 2022

Background: Epidemiological observations such as mental retardation, physical deformities, etc., in children besides different types of cancer in the adult population of the Malwa region have been reported. The present study is designed to get insight into the role of naturally occurring radioactive material (NORM) in causing detrimental health effects observed in the general population of this region. Materials and Methods: Deep soil samples were collected from different locations in the Malwa region. Their activity concentrations were determined using low-level background gammaray spectrometry. High efficiency and high purity germanium detector capped in a lead-shielded chamber having a resolution of 1.8 keV at 1,173 keV and 2.0 keV at the 1,332 keV line of ⁶⁰Co was used in the present work. Data were evaluated with Genie-2000 software. Results and Discussion: Mean activity concentrations of ²³⁸U, ²³²Th, and ⁴⁰K in deep soil were found to be 101.3 Bq/kg, 65.8 Bq/kg, and 688.6 Bq/kg, respectively. The mean activity concentration of ²³⁸U was found to be three and half times higher than the global average prescribed by the United Nations Scientific Committee on the Effects of Atomic Radiation (UNSCEAR). It was further observed that the activity concentration of ²³²Th and ⁴⁰K has a magnitude that is nearly one and half times higher than the global average prescribed by UNSCEAR. In addition, the radioisotope ¹³⁷Cs which is likely to have its origin in radiation fallout was also observed. It is postulated that the NORM present in high quantity in deep soil somehow get mobilized into the water aquifers used by the general population and thereby causing harmful health problems. Conclusion: It can be stated that the present work has been able to demonstrate the use of low background gamma-ray spectrometry to understand the role of NORM in causing health-related effects in a general population of the Malwa region of Punjab, India.