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1968년 ~ 2022년까지 1,161 건의 한국천문학회지를 격월간 확인하실 수 있습니다.
- The Korean Astronomical Society (The Korean Astronomical Society)
- 계간 (Quarterly)
- ISSN : 1225-4614 (ISSN : 1225-4614)
1225-4614
- DB구축현황 : 1,161건 (DB Construction : 1,161 Articles)
총 게시글 1,161건
페이지 4/117
31
- Hwang, Jeong-Sun
- Journal of the Korean astronomical society = 천문학회지
- 54, n.2
- pp.71-88
- 2021
- 원문 바로보기
We use N-body/hydrodynamic simulations to study the evolution of the spin of a Milky Way-like galaxy through interactions. We perform a controlled experiment of co-planar galaxy-galaxy encounters and study the evolution of disk spins of interacting galaxies. Specifically, we consider cases where the late-type target galaxy encounters an equally massive companion galaxy, which has either a late or an early-type morphology, with a closest approach distance of about 50 kpc, in prograde or retrograde sense. By examining the time change of the circular velocity of the disk material of the target galaxy from each case, we find that the target galaxy tends to lose the spin through prograde collisions but hardly through retrograde collisions, regardless of the companion galaxy type. The decrease of the spin results mainly from the deflection of the orbit of the disk material by tidal disruption. Although there is some disk material which gains the circular velocity through hydrodynamic as well as gravitational interactions or by transferring material from the companion galaxy, it turns out that the amount of the material is generally insufficient to increase the overall galactic spin under the conditions we set. We find that the spin angular momentum of the target galaxy disk decreases by 15-20% after a prograde collision. We conclude that the accumulated effects of galaxy-galaxy interactions will play an important role in determining the total angular momentum of late-type galaxies.
32
- Kim, Minjin
- Journal of the Korean astronomical society = 천문학회지
- 54, n.2
- pp.37-47
- 2021
- 원문 바로보기
Reverberation mapping (RM) is an efficient method to investigate the physical sizes of the broad line region (BLR) and dusty torus in an active galactic nucleus (AGN). The Spectro-Photometer for the History of the Universe, Epoch of Reionization and Ices Explorer (SPHEREx) mission will provide multi-epoch spectroscopic data at optical and near-infrared wavelengths. These data can be used for RM experiments with bright AGNs. We present results of a feasibility test using SPHEREx data in the SPHEREx deep regions for torus RM measurements. We investigate the physical properties of bright AGNs in the SPHEREx deep field. Based on this information, we compute the efficiency of detecting torus time lags in simulated light curves. We demonstrate that, in combination with complementary optical data with a depth of ~ 20 mag in B-band, lags of ≤ 750 days for tori can be measured for more than ~ 200 bright AGNs. If high signal-to-noise ratio photometric data with a depth of ~ 21-22 mag are available, RM measurements are possible for up to ~ 900 objects. When complemented by well-designed early optical observations, SPHEREx can provide a unique dataset for studies of the physical properties of dusty tori in bright AGNs.
33
- Lee, Jae-Ok
- Journal of the Korean astronomical society = 천문학회지
- 54, n.2
- pp.61-70
- 2021
- 원문 바로보기
We investigate 20 post-coronal mass ejection (CME) blobs formed in the post-CME current sheet (CS) that were observed by K-Cor on 2017 September 10. By visual inspection of the trajectories and projected speed variations of each blob, we find that all blobs except one show irregular 'zigzag' trajectories resembling transverse oscillatory motions along the CS, and have at least one oscillatory pattern in their instantaneous radial speeds. Their oscillation periods are ranging from 30 to 91 s and their speed amplitudes from 128 to 902 km s-1. Among 19 blobs, 10 blobs have experienced at least two cycles of radial speed oscillations with different speed amplitudes and periods, while 9 blobs undergo one oscillation cycle. To examine whether or not the apparent speed oscillations can be explained by vortex shedding, we estimate the quantitative parameter of vortex shedding, the Strouhal number, by using the observed lateral widths, linear speeds, and oscillation periods of the blobs. We then compare our estimates with theoretical and experimental results from MHD simulations and fluid dynamic experiments. We find that the observed Strouhal numbers range from 0.2 to 2.1, consistent with those (0.15-3.0) from fluid dynamic experiments of bluff spheres, while they are higher than those (0.15-0.25) from MHD simulations of cylindrical shapes. We thus find that blobs formed in a post-CME CS undergo kinematic oscillations caused by fluid dynamic vortex shedding. The vortex shedding is driven by the interaction of the outward-moving blob having a bluff spherical shape with the background plasma in the post-CME CS.
34
- Lee, Chung-Uk
- Journal of the Korean astronomical society = 천문학회지
- 54, n.4
- pp.113-119
- 2021
- 원문 바로보기
It is difficult for observers to conduct an optical alignment at an observatory without the assistance of an optical engineer if optomechanical parts are to be replaced at night. We present a practical tilt correction method to obtain the optimal optical alignment condition using the symmetricity of optical aberrations of a wide-field on-axis telescope at night. We conducted coarse tilt correction by visually examining the symmetry of two representative star shapes obtained at two guide chips facing each other, such as east-west or north-south pairs. After coarse correction, we observed four sets of small stamp images using four guide cameras located at each cardinal position by changing the focus positions in 10-㎛ increments and passing through the optimum focus position in the range of ±200 ㎛. The standard deviation of each image, as a function of the focus position, was fitted with a second-order polynomial function to derive the optimal focus position at each cardinal edge. We derived the tilt angles from the slopes converted by the distance and the focus position difference between two paired guide chip combinations such as east-west and north-south. We used this method to collimate the on-axis wide-field telescope KMTNet in Chile after replacing two old focus actuators. The total optical alignment time was less than 30 min. Our method is practical and straightforward for maintaining the optical performance of wide-field telescopes such as KMTNet.
35
- Kim, Yonggi
- Journal of the Korean astronomical society = 천문학회지
- 53, n.2
- pp.43-48
- 2020
- 원문 바로보기
We report an analysis of two poorly studied eclipsing binary stars, GSC 04396-00605 and GSC 04395-00485 (recently named V455 Dra and V454 Dra, respectively). Photometric data of the two stars were obtained using the 1-m Korean telescope of the LOAO operated by KASI while monitoring the cataclysmic variable DO Dra in the frame of the Inter-Longitude Astronomy (ILA) project. We derived periods of 0.434914 and 0.376833 days as well as initial epochs JD 2456480.04281 and JD 2456479.0523, respectively, more accurate than previously published values by factors 9 and 6. The phenomenological characteristics of the mean light curves were determined using the New Algol Variable (NAV) algorithm. The individual times of maxima/minima (ToM) were determined using the newly developed software MAVKA, which outputs accurate parameters using 'asymptotic parabola' approximations. The light curves were approximated using phenomenological and physical models. In the NAV algorithm, the phenomenological parameters are well determined. We derived physical parameters using the Wilson-Devinney model. In this model, the best-fit parameters are highly correlated, thus some of them were fixed to reasonable values. For both systems, we find evidence for the presence of a cool spot and estimate its parameters. Both systems can be classified as overcontact binaries of EW type.
36
- Morgan, Hannah L.
- Journal of the Korean astronomical society = 천문학회지
- 53, n.6
- pp.117-123
- 2020
- 원문 바로보기
We investigate the plausibility of mass return, from stellar mass loss processes within the central ~100 pc region of the Milky Way (the inner nuclear bulge), as a mass supply mechanism for the Circumnuclear Disk (CND). Gas in the Galactic disk migrates inward to the Galactic centre due to the asymmetric potential caused by the Galactic bar. The inward migration of gas stops and accumulates to form the central molecular zone (CMZ), at 100-200 pc from the Galactic center. It is commonly assumed that stars have formed in the CMZ throughout the lifetime of the Galaxy and have diffused inward to form a 'r-2 stellar cusp' within the inner nuclear bulge. We propose that the stars migrating inward from the CMZ supply gas to the inner nuclear bulge via stellar mass loss, resulting in the formation of a gas disk along the Galactic plane and subsequent inward migration down to the central 10 pc region (CND). We simulate the evolution of a gas distribution that initially follows the stellar distribution of the aforementioned stellar cusp, and illustrate the potential gas supply toward the CND.
37
- Gould, Andrew
- Journal of the Korean astronomical society = 천문학회지
- 53, n.5
- pp.99-102
- 2020
- 원문 바로보기
I show that when the observables (π<sub>E</sub>, t<sub>E</sub>, θ<sub>E</sub>, π<sub>s</sub>, µ<sub>s</sub>) are well measured up to a discrete degeneracy in the microlensing parallax vector π<sub>E</sub>, the relative likelihood of the different solutions can be written in closed form P<sub>i</sub> = KH<sub>i</sub>B<sub>i</sub>, where H<sub>i</sub> is the number of stars (potential lenses) having the mass and kinematics of the inferred parameters of solution i and B<sub>i</sub> is an additional factor that is formally derived from the Jacobian of the transformation from Galactic to microlensing parameters. Here t<sub>E</sub> is the Einstein timescale, θ<sub>E</sub> is the angular Einstein radius, and (π<sub>s</sub>, µ<sub>s</sub>) are the (parallax, proper motion) of the microlensed source. The Jacobian term B<sub>i</sub> constitutes an explicit evaluation of the 'Rich Argument', i.e., that there is an extra geometric factor disfavoring large-parallax solutions in addition to the reduced frequency of lenses given by H<sub>i</sub>. I also discuss how this analytic expression degrades in the presence of finite errors in the measured observables.
38
- Lee, Byeong-Cheol
- Journal of the Korean astronomical society = 천문학회지
- 53, n.1
- pp.27-34
- 2020
- 원문 바로보기
We report the detection of exoplanet candidates in orbits around HD 60292 and HD 112640 from a radial velocity (RV) survey. The stars exhibit RV variations with periods of 495 ±3 days and 613±6 days, respectively. These detections are part of the Search for Exoplanets around Northern Circumpolar Stars (SENS) survey using the fiber-fed Bohyunsan Observatory Echelle Spectrograph installed at the 1.8-m telescope of the Bohyunsan Optical Astronomy Observatory in Korea. The aim of the survey is to search for planetary or substellar companions. We argue that the periodic RV variations are not related to surface inhomogeneities; rather, Keplerian motions of planetary companions are the most likely interpretation. Assuming stellar masses of 1.7 ± 0.2M<sub>⊙</sub> (HD 60292) and 1.8 ± 0.2M<sub>⊙</sub> (HD 112640), we obtain minimum planetary companion masses of 6.5 ± 1.0M<sub>Jup</sub> and 5.0 ± 1.0M<sub>Jup</sub>, and periods of 495.4 ± 3.0 days and 613.2 ± 5.8 days, respectively.
39
- Hyung, Siek
- Journal of the Korean astronomical society = 천문학회지
- 53, n.2
- pp.35-42
- 2020
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We analyze high dispersion emission lines of the symbiotic nova AG Pegasi, observed in 1998, 2001, and 2002. The Hα and Hβ lines show three components, two narrow and one underlying broad line components, but most other lines, such as H<sub>I</sub>, He<sub>I</sub>, and He<sub>II</sub> lines, show two blue- and red-shifted components only. A recent study by Lee & Hyung (2018) suggested that the double Gaussian lines emitted from a bipolar conical shell are likely to form Raman scattering lines observed in 1998. In this study, we show that the bipolar cone with an opening angle of 74°, which expands at a velocity of 70 km s<sup>-1</sup> along the polar axis of the white dwarf, can accommodate the observed double line profiles in 1998, 2001, and 2002. We conclude that the emission zone of the bipolar conical shell, which formed along the bipolar axis of the white dwarf due to the collimation by the accretion disk, is responsible for the double Gaussian profiles.
40
- Gould, Andrew
- Journal of the Korean astronomical society = 천문학회지
- 53, n.1
- pp.9-26
- 2020
- 원문 바로보기
At q = 1.81 ± 0.20 × 10<sup>-5</sup>, KMT-2018-BLG-0029Lb has the lowest planet-host mass ratio q of any microlensing planet to date by more than a factor of two. Hence, it is the first planet that probes below the apparent 'pile-up' at q = 5-10 ×10<sup>-5</sup>. The event was observed by Spitzer, yielding a microlens-parallax π<sub>E</sub> measurement. Combined with a measurement of the Einstein radius θ<sub>E</sub> from finite-source effects during the caustic crossings, these measurements imply masses of the host M<sub>host</sub> = 1.14<sup>+0.10</sup><sub>-0.12</sub> M<sub>⊙</sub> and planet M<sub>planet</sub> = 7.59<sup>+0.75</sup><sub>-0.69</sub> M<sub>⊕</sub>, system distance D<sub>L</sub> = 3.38<sup>+0.22</sup><sub>-0.26</sub> kpc and projected separation a<sub>⊥</sub> = 4.27<sup>+0.21</sup><sub>-0.23</sub> AU. The blended light, which is substantially brighter than the microlensed source, is plausibly due to the lens and could be observed at high resolution immediately.