• 천문학논총
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• 제30권2호
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• pp.559-563
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• 2015

Monitor of All-sky X-ray Image (MAXI) is a Japanese X-ray all-sky surveyer mounted on the International Space Station (ISS). It has been scanning the whole sky since 2009 during every 92-minute ISS rotation. X-ray transients are quickly found by the real-time nova-search program. As a result, MAXI has issued 133 Astronomer's Telegrams and 44 Gamma-ray burst Coordinated Networks so far. MAXI has discovered six new black holes (BH) in 4.5 years. Long-term behaviors of the MAXI BHs can be classified into two types by their outbursts; a fast-rise exponential-decay type and a fast-rise flat-top one. The slit camera is suitable for accumulating data over a long time. MAXI issued a 37-month catalog containing 500 sources above a ~0.6 mCrab detection limit at 4-10 keV in the region ${\mid}{b}{\mid}$ > $10^{\circ}$. The SSC instrument utilizing an X-ray CCD has detected diffuse soft X-rays extending over a large solid angle, such as the Cygnus super bubble. MAXI/SSC has also detcted a Ne emission line from the rapid soft X-ray nova MAXI J0158-744. The overall shapes of outbursts in Be X-ray binaries (BeXRB) are precisely observed with MAXI/GSC. BeXRB have two kinds of outbursts, a normal outburst and a giant one. The peak dates of the subsequent giant outbursts of A0535+26 repeated with a different period than the orbital one. The Be stellar disk is considered to either have a precession motion or a distorted shape. The long-term behaviors of low-mass X-ray binaries (LMXB) containing weakly magnetized neutron stars are investigated. Transient LMXBs (Aql X-1 and 4U 1608-52) repeated outbursts every 200-1000 days, which is understood by the limit-cycle of hydrogen ionization states in the outer accretion disk. A third state (very dim state) in Aql X-1 and 4U 1608-52 was interpreted as the propeller effect in the unified picture of LMXB. Cir X-1 is a peculiar source in the sense that its long-term behavior is not like typical LMXBs. The luminosity sometimes decreases suddenly at periastron. It might be explained by the stripping of the outer accretion disk by a clumpy stellar wind. MAXI observed 64 large flares from 22 active stars (RS CVns, dMe stars, Argol types, young stellar objects) over 4 years. The total energies are $10^{34}-10^{36}$ erg $s^{-1}$. Since MAXI can measure the spectrum (temperature and emission measure), we can estimate the size of the plasma and the magnetic fields. The size sometimes exceeds the size of the star. The magnetic field is in the range of 10-100 gauss, which is a typical value for solar flares.

• 한국전자파학회논문지
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• 제29권6호
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• pp.407-410
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• 2018

일반적으로 전자파의 동작 주파수가 높아짐에 따라 최대 출력이 작아지고, 파동의 파장도 작아지기 때문에, 회로의 크기도 작아질 수밖에 없다. 특히, kW급 이상의 고출력 테라헤르츠파 주파수 대역의 회로를 제작하려면, ${\mu}m{\sim}mm$ 규모의 회로 크기 문제 때문에 제작에 한계점이 있다. 이러한 한계점을 극복하기 위해 본 논문에서는 회로의 지름이 2.4 cm 정도의 원통형으로, 0.1 THz~0.3 GW급의 발생원 설계 기술을 제안한다. 판드로모티브 힘이 생기는 플라즈마 항적장 가속원리와 인위적인 유전체 활용한 체렌코프방사 발생 기술 기반의 고출력 전자파 발생원의 최적화된 설계를 위해 모델링 및 전산모사를 수행하였다. 객관적인 검증 과정을 통해 회로의 크기에 제한을 덜 받도록 하는 대구경 형태의 고출력 테라헤르츠파 진공소자 제작이 용이하도록 효과적인 설계의 가이드라인을 제시하였다.