• 대한원격탐사학회지
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• 제31권4호
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• pp.353-360
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• 2015

Earth's gravity field recovery was improved after the pre-processing upgrade of the Gravity Recovery And Climate Experiments (GRACE) satellite's star trackers. The star tracker measurements were filtered with a tighter low-pass filtering of 0.025Hz cutoff frequency, instead of a nominal filtering of 0.1Hz cutoff frequency. In addition, a jump removal algorithm was applied to remove discontinuities, due to direct Sun and/or Moon interventions, in the star tracker measurements. During the K-Band Ranging (KBR) calibration maneuvers, large attitude variations could be detected concurrently by both of the star trackers and the accelerometer. The misalignment angles of star trackers between the true frame and the normal frame could be determined by comparing measurements from these sensors. In this paper, new Earth' gravity field maps were obtained using above improvement. Based on comparisons to nominal Earth's gravity field maps, the new Earth's gravity field maps were found better than the nominal ones. Among the applied methods, the misalignment calibration of the star trackers had a major impact on the improvement of the new Earth's gravity field maps.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2008년도 한국우주과학회보 제17권2호
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• pp.28.2-28.2
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• 2008

Recently, star sensors have been successfully used as main attitude sensors for attitude control in many satellites. This research presents the star visibility analysis for star trackers and the goal of this analysis is to make sure that the star tracker implementation is suitable to the mission profile and scenario and satisfies the requirement of attitude orbit control system. As a main optical attitude sensor imaging stars, accomodations of a star tracker should be optimized in order to improve the probability of the usage by avoiding the blinding (the unavailability) by the Sun and the Earth. For the analysis, a statistical approach and a time simulation approach are used. The statistical approach is based on the generation of numerous cases, to derive relevant statistics about Earth and Sun proximity probabilites for different lines of sight. The time simulation approach is performed for one orbit to check the statistical result and to refine the statistical result and accomodations of star trackers. In order to perform simulations first of all, an orbit and specific mission profiles of a satellite are set, next the earth proximity probability and the sun proximity probability are calculated by considering the attitude maneuvers and the geometry of the orbit, and then finally the unavailability positions are estimated. As a result, the optimized accomodations of two star trackers are suggested for the low earth orbit satellite.

• 한국지구과학회지
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• 제34권5호
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• pp.407-414
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• 2013

This study presents the global star formation efficiency (SFE) of 272 local star-forming galaxies based on the HI gas mass, stellar mass, star formation rate (SFR), and morphology. The SFE increases as the stellar mass increases while the specific SFR decreases. The SFE is enhanced for galaxies with large H$\acute{a}$ equivalent widths, which is primarily due to the large SFR, not due to the large available amount of gas. The SFE is also enhanced by a factor of ~2 for merging systems compared to the normal spirals, showing that the merger-induced high pressure and density environment are crucial for the active star formation. Based on the SFR scaling relation, I present a SFR calibration formula using the HI gas mass.

• 한국항공우주학회지
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• 제35권8호
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• pp.735-740
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• 2007

별센서는 우주 공간상의 별 이미지를 사용하여 초정밀 자세 정보를 제공한다. 그러나 센서가 태양광이나 지구 반사광(Albedo)으로부터의 회피각이 보장되지 않는 경우 센서 출력의 정밀도를 보장할 수 없거나 출력을 얻을 수 없다. 이 논문은 별센서의 탑재 방향에 따른 태양 및 지구 회피각의 특성에 대한 연구 결과를 제시하고 있다. 아울러 지구 관측 임무에 적합한 별센서의 탑재 방향 결정을 위한 체계적인 방법을 제시한다.

• 천문학회보
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• 제19권
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• pp.21.2-22
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• 1994

• 천문학회지
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• 제29권1호
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• pp.19-30
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• 1996

We have examined consequences of strong tidal encounters between a neutron star and a normal star using SPH as a possible formation mechanism of isolated recycled pulsars in globular clusters. We have made a number of SPH simulations for close encounters between a main-sequence star of mass ranging from 0.2 to 0.7 $M_\bigodot$ represented by an n=3/2 poly trope and a neutron star represented by a point mass. The outcomes of the first encounters are found to be dependent only on the dimensionless parameter $\eta'{\equiv}(m/(m+ M))^{1/2}(\gamma_{min}/R_{MS})^{3/2}(m/M)^{{1/6)}$, where m and M are the mass of the main-sequence star and the neutron star, respectively, $\gamma_{min}$ the minimum separation between two stars, and $R_{MS}$ the size of the main-sequence star. The material from the (at least partially) disrupted star forms a disk around the neutron star. If all material in the disk is to be acctreted onto the neutron star's surface, the mass of the disk is enough to spin up the neutron star to spin period of 1 ms.

• 천문학회보
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• 제45권1호
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• pp.35.2-35.2
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• 2020

Submillimeter galaxies (SMGs) have played an important role in the understanding of galaxy evolution and cosmic star formation history at high redshift because they are known as being located at z ~ 2 and harbor a vigorous star formation. Therefore studying properties of SMGs can lead us to understand evolution of massive and actively star forming galaxies and distribution of cosmic star formation density. Recently we detected 548 SMGs near North Ecliptic Pole with JCMT/SCUBA-2 from the JCMT large program covering about 2 deg2 so far. To derive their physical parameters, we compiled a multi-wavelength photometry ranging from optical (0.3 ㎛) to submillimeter (850 ㎛) by cross-identifying counterparts at different wavelengths. In order to find counterparts, we used either VLA-1.4 GHz image and/or Spitzer/IRAC 3.6 ㎛, 4.5 ㎛ image. The number of SMGs with relatively robust counterparts is 349. In this talk, we present photometric redshifts, stellar mass, star formation rates, total infrared luminosity, and AGN fraction of these 349 SMGs derived through SED fitting analysis.

• 한국지구과학회지
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• 제35권5호
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• pp.362-374
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• 2014

This study investigated the initial mass function (IMF) and star formation history of high-mass stars in the Small Magellanic Cloud (SMC) using a population synthesis technique. We used the photometric survey catalog of Lee (2013) as the observable quantities and compare them with those of synthetic populations based on Bayesian inference. For the IMF slope (${\Gamma}$) range of -1.1 to -3.5 with steps of 0.1, five types of star formation models were tested: 1) continuous; 2) single burst at 10 Myr; 3) single burst at 60 Myr; 4) double bursts at those epochs; and 5) a complex hybrid model. In this study, a total of 125 models were tested. Based on the model calculations, it was found that the continuous model could simulate the high-mass stars of the SMC and that its IMF slope was -1.6 which is slightly steeper than Salpeter's IMF, i.e., ${\Gamma}=-1.35$.

• 한국지구과학회지
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• 제38권3호
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• pp.209-221
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• 2017

가까운 은하에서 폭발적 항성생성은하의 분광 관측을 수행하여 별생성률이 높은 은하에서 별생성이 일어나는 시간 규모에 따라 방출선의 방출 기작, 별생성률, 항성질량, 금속함량 등의 물리량 혹은 물리량 상호 간의 관계가 어떻게 다른지를 살펴보았다. 관측 대상은 별생성 나이가 매우 어린 울프-레이에 은하 21개와 상대적으로 긴 시간 규모의 별생성이 진행 중인 자외선 초과복사 은하 13개로 보현산 천문대의 1.8 m 망원경과 4K CCD, 긴 슬릿 분광기를 이용해 광학영역에서의 스펙트럼을 얻었다. BPT 분석도표를 그려 관측된 은하들에서 기체를 이온화시키는 원인을 살펴보면 전체적으로는 별생성(약 50%)이 비항성적 요소인 활동은하핵(약 15%)에 비해 훨씬 높았다. 별생성과 활동은하핵이 모두 기여하는 경우도 전체의 35%였는데, 이러한 경우에 속하는 은하는 대부분 상대적으로 나이가 많을 것으로 추정되는 자외선 초과복사 은하였다. 관측된 은하의 항성질량 범위는 대부분 $10^{9-11}M_{\odot}$이고 별생성률은 $0.01-100M_{\odot}yr^{-1}$로, SDSS에서 관측된 은하들로 구성된 별생성 주계열에 위치한다. 울프-레이에 은하와 자외선 초과복사 은하들의 항성질량, 별생성률에서 큰 차이는 없었다. 또한 폭발적 항성생성은하는 질량-금속함량 관계를 보이며, 비슷한 항성질량을 가진 SDSS 은하와 비교했을 때 금속함량이 낮게 나타났다. 이는 이 은하들에서 별생성으로 인한 강한 피드백이 일어나고 있음을 보여준다.

• 한국지구과학회지
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• 제38권1호
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• pp.1-10
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• 2017

공생별 AG Peg는 적색거성(GS)과 백색왜성(WD)으로 구성된 성운으로 둘러싸인 쌍성계이다. AG Peg의 분광자료는 1998년, 2001년, 그리고 2002년의 세 시기에 미국 Lick 천문대에서 관측한 자료로 HI 발머 방출선 자료를 분석하였다. AG Peg의 선세기와 폭은 각 시기에 따라 변하는데, $H{\alpha}$와 $H{\beta}$ 선에서 모두 청색편이, 적색편이, 넓은 폭 성분이 나타났다. 가스 성운의 운동학적 특성을 보여주는 방출선은 WD주변에 형성된 강착원반의 반경이 매우 큼을 보여준다. 관측자의 시선 방향을 고려하면, 1998년 관측은 AG Peg의 GS와 WD가 나란히 하늘에 있는 반면, 2002년에는 WD가 GS의 전면에, 2001년에는 WD가 GS의 뒷면에 위치하였다. 이러한 상대적인 위치와 분광선의 변화를 고려하여, 우리는 GS에서 WD로의 가스유입이 지속적으로 이루어지고, 그 결과 형성된 두꺼운 원반의 회전이 관측된 분광선 윤곽의 형성을 가져온 것으로 결론지었다.