• Sleep Medicine and Psychophysiology
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• v.1 no.1
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• pp.3-8
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• 1994

With the recent development of sleep medicine, insomnia has been perceived as a disease from a simple symptom. As there are various causes in a disease, proper treatment according to each cause is necessary for a more effective treatment In general, insomnia is classified into five categrories of physical, physiological, psychological, psychiatric and pharmacological aspects. However, such categorizations are often insufficient in treating insomnia. Furthermore understanding of the developmental mechanisms of insomnia is required. The function of sleep is developed and maintained through the balance of the reciprocal forces of sleep and arousal. These forces are contantly regulated by what is called a circadian rhythm. Sleep is induced by this rhythm which is affected by factors such as awakening time in the morning, amount of intellectual function, amount and time length of physical exercise and sunlight Insomnia could develop when this rhythm is delayed and leads to a "forbidden zone" which is a very difficult period for inducing sleep about two to four hours before the routine bedtime. Whereas sleep gradually develops in line with the circardian rhythm, arousal can occur very abruptly by any cause triggered by emotional discomfort or anxiety. Such characteristic and emotional factors as perfectionism, separation anxiety, secondary gain, insecurity, and negative cognition may provoke the inner anxiety and fear for insomnia, which can lead acute insomnia to a chronic one. As chronic insomnia is developed by multiple causes and factors, integrated approaches through analysis of above mentioned factors will be more effective in the treatment of insomnia than a simple administration of hypnotics.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.72.2-72.2
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• 2012

We present the results of HI 21 cm line observations to explore the nature of the high-velocity (HV) HI gas at - 173${\circ}$, which appears as faint, wing-like, Hi emission that extends to velocities beyond those allowed by Galactic rotation in the low-resolution surveys. We designate this feature as Forbidden Velocity Wing (FVW) 172.8+1.5. Our high-resolution Arecibo HI observations show that FVW 172.8+1.5 is composed of knots, filaments, and ring-like structures distributed over an area of a few degrees in extent. These HV HI emission features are well correlated with the HII complex G173+1.5, which is composed of five Sharpless HII regions distributed along a radio continuum loop of size 4.4${\times}$3.4, or -138 pc ${\times}$ 107 pc, at a distance of 1.8 kpc. G173+1.5 is one of the largest star-forming regions in the outer Galaxy. The HV HI gas and the radio continuum loop seem to trace an expanding shell. Its derived HI parameters including large expansion velocity (55 km/s) imply the SNR interpretation. Hot xray emission is detected within the HII complex, which also supports its SNR origin. The FVW172.8+1.5 is most likely the products of a supernova explosion(s) within the HII complex, possibly in a cluster that triggered the formation of these HII regions.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.1
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• pp.38.2-38.2
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• 2017

We present the observational study toward the multiple outflows around $LkH{\alpha}$ 234 star formation region. The high-resolution, near-IR spectral mapping using the Immersion Grating Infrared Spectrograph (IGRINS) allowed us to distinguish at least four separate outflows with the molecular hydrogen ($H_2$) and forbidden iron ([Fe II]) emission lines. The outflow associated with the radio continuum source VLA 3B is detected in both H2 and [Fe II] emission, while the outflows driven by MM 1, VLA 2 sources were only detected in $H_2$, indicating the different physical conditions of outflows. We confirm the axis of VLA 3B jet, the position angle of ${\sim}240^{\circ}$. We firstly identified the redshifted, near-IR H2 outflow associated with VLA 2, which is coincident with the previous detections of $H_2O$ masers. From the $H_2$ line ratios, we interpret the gas properties of the shock excited blue- and redshifted components, and UV excited surrounding photodissociation region. We also discuss the origin of the high-velocity (|VLSR| > $150km\;s^{-1}$) $H_2$ emission.

• Journal of The Korean Astronomical Society
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• v.54 no.2
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• pp.49-60
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• 2021

Observations of line of sight (LOS) Doppler velocity and non-thermal line width in the off-limb solar corona are often used for investigating the Alfvén wave signatures in the corona. In this study, we compare LOS Doppler velocities and non-thermal line widths obtained simultaneously from two different instruments, Coronal Multichannel Polarimeter (CoMP) and Hinode/EUV Imaging Spectrometer (EIS), on various off-limb coronal regions: flaring and quiescent active regions, equatorial quiet region, and polar prominence and plume regions observed in 2012-2014. CoMP provides the polarization at the Fe xiii 10747 Å coronal forbidden lines which allows their spectral line intensity, LOS Doppler velocity, and line width to be measured with a low spectral resolution of 1.2 Å in 2-D off limb corona between 1.05 and 1.40 RSun, while Hinode/EIS gives us the EUV spectral information with a high spectral resolution (0.025 Å) in a limited field of view raster scan. In order to compare them, we make pseudo raster scan CoMP maps using information of each EIS scan slit time and position. We compare the CoMP and EIS spectroscopic maps by visual inspection, and examine their pixel to pixel correlations and percentages of pixel numbers satisfying the condition that the differences between CoMP and EIS spectroscopic quantities are within the EIS measurement accuracy: ±3 km s-1 for LOS Doppler velocity and ±9 km s-1 for non-thermal width. The main results are summarized as follows. By comparing CoMP and EIS Doppler velocity distributions, we find that they are consistent with each other overall in the active regions and equatorial quiet region (0.25 ≤ CC ≤ 0.7), while they are partially similar to each other in the overlying loops of prominences and near the bottom of the polar plume (0.02 ≤ CC ≤ 0.18). CoMP Doppler velocities are consistent with the EIS ones within the EIS measurement accuracy in most regions (≥ 87% of pixels) except for the polar region (45% of pixels). We find that CoMP and EIS non-thermal width distributions are similar overall in the active regions (0.06 ≤ CC ≤ 0.61), while they seem to be different in the others (-0.1 ≤ CC ≤ 0.00). CoMP non-thermal widths are similar to EIS ones within the EIS measurement accuracy in a quiescent active region (79% of pixels), while they do not match in the other regions (≤ 61% of pixels); the CoMP observations tend to underestimate the widths by about 20% to 40% compared to the EIS ones. Our results demonstrate that CoMP observations can provide reliable 2-D LOS Doppler velocity distributions on active regions and might provide their non-thermal width distributions.

• Journal of the Korean earth science society
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• v.28 no.7
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• pp.847-856
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• 2007

The Planetary nebula NGC 6881 displays quadrupole morphology and it also has a jet feature in its image. We investigated the line profiles of the optical region spectral emission lines, using the Hamilton Echelle Spectrograph (HES) at the Lick observatory. The HES data obtained in this study was the radiation coming from the inner region within the diameter of 4 second of arc. Expansion velocity was obtained, based on the strong emission line profiles of e.g. H, Hel, Hell, [OIII], [NII], [ArIII], [SII], and [SIII}, using the IRAF and StarLink/Dipso reduction packages. The HI recombination lines showed one single peak profile, while the He and forbidden strong lines displayed double peaks. The results of this study show that the outflow velocity of gas increases radially outwards due to the central stellar radiation pressure. It was concluded that three central rings appeared in the HST image are the result of a combined structure of bipolar cones (seen in e.g. HI lines) and a ring (seen in He, [SIII] lines) in projection.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.82.2-82.2
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• 2012

We present Herschel-PACS observations of L1448-MM, a Class 0 protostar with a prominent outflow, part of the DIGIT Key Program (PI: N. Evans). We detect numerous emission lines including CO and $H_2O$ rotational transitions, OH transitions, and [OI] forbidden transitions at wavelengths from 55 to 210 ${\mu}m$. The $H_2O$, [OI], mid-J CO (J < 23), and OH emission distributes along the outflow direction although high-J CO and other OH emission peaks at the central spatial pixel. According to our simple excitation analysis, CO seems to have two temperature components of warm and hot, which might be attributed to the PDR and shock, respectively. After exploring a wide range of physical conditions with a non-LTE LVG code, RADEX, we found that either shock alone or the combination of PDR and shock can explain the observations. The relative fraction of observed line luminosities suggest that L1448-MM is shielded from the UV radiation because $H_2O$ and CO are the dominant coolants rather than OH and [OI]. In addition, our observed fluxes match better with C-shock models rather than J-shocks. The non-LTE LVG model supports that the IR pumping process is important for OH transitions because the OH line ratios are fitted much better when the dust thermal continuum is included.

• Journal of the Korean Chemical Society
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• v.41 no.4
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• pp.175-179
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• 1997

Luminescence of $Eu^{3+}$ has been studied in $Sr_{2-2x}Eu_xK_xSnO_4$ with two-dimensional $K_2NiF_4$ structure. The $^5D_o$ → $^7F_o$$Eu^{3+}$ ion represents the J=0 → J=0 transition which is forbidden by a Judd-Ofelt selection rule for electric dipole transition in 4f shell of $Eu^{3+}$ ions. However, the emission line of $^5D_o$ → $^7F_o$$Eu^{3+}$ emission spectra of Sr2-2xEuxKxSnO4$Sr_{2-2x}Eu_xK_xSnO_4$structure around $Eu^{3+}$ ions.

• Journal of The Korean Astronomical Society
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• v.36 no.4
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• pp.271-282
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• 2003

We present results of a $H^{13}CN$ J=1-0 mapping survey of molecular clouds toward the Galactic Center (GC) region of $-1.6^{\circ}{\le}{\iota}{\le}2^{\circ}$ and $-0.23^{\circ}{\le}b{\le}0.30^{\circ}$ with 2' grid resolution. The $H^{13}CN$ emissions show similar distribution and velocity structures to those of the $H^{12}CN$ emissions, but are found to better trace the feature saturated with $H^{12}CN$ (1-0). The bright components among multi-components of $H^{12}CN$ line profiles usually appear in the $H^{13}CN$ line while most of the dynamically forbidden, weak $H^{12}CN$ components are seldom detected in the $H^{13}CN$ line. We also present results of other complementary observations in $^{12}CO$ (J=1-0) and $^{13}CO$ (J=1-0) lines to estimate physical quantities of the GC clouds, such as fractional abundance of HCN isotopes and mass of the GC cloud complexes. We confirm that the GC has very rich chemistry. The overall fractional abundance of $H^{12}CN$ and $H^{13}CN$ relative to $H_2$ in the GC region is found to be significantly higher than those of any other regions, such as star forming region and dark cloud. Especially cloud complexes nearer to the GC tend to have various higher abundance of HCN. Total mass of the HCN molecular clouds within $[{\iota}]{\le}6^{\circ}$ is estimated to be ${\~}2 {\times}10^7\;M_{\bigodot}$ using the abundances of HCN isotopes, which is fairly consistent with previous other estimates. Masses of four main complexes in the GC range from a few $10^5$ to ${\~}10^7\;M_{\bigodot}$ All the HCN spectra with multi-components for the four main cloud complexes were investigated to compare the line widths of the complexes. The largest mode (45 km $s^{-1}$) of the FWHM distributions among the complexes is in the Clump 2. The value of the mode tends to be smaller at the farther complexes from the GC.

• Korean Journal of Heritage: History & Science
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• v.52 no.3
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• pp.130-145
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• 2019

The palaces in South Korea are largely divided into primary palaces (法宮) and secondary palaces (離宮). In the early Joseon period, the primary palace was Gyeongbokgung Palace, and the secondary palace was Changdeokgung Palace. Additionally, there is the concept of imperial palaces (正宮). Gyeongbokgung Palace was the primary palace and the imperial palace. The topography of Gyeongbokgung is based on Mt. Baegak, which is the symbol of royal authority. The location of the palaces was chosen to highlight the king's dignity and authority. The three gates and three courts (三門三朝) were positioned on a straight line based on one axis along the ridge of Mt. Baegak to establish the legitimacy, hierarchy, and unity of the kingship. The secondary palace was built according to the demands of the king and the royal family or the political situation. It was created as a royal living space; thus, creating independent and diverse spaces along multiple axes. The primary palace was chosen to be built on the terrain of Yang, and the secondary palace was chosen to be built on the terrain of Yin; the criteria for laying buildings in the palace areas had to be different. The most important point in the formation of Joseon palaces was that the secret vital energy for the king (王氣) originated from the sacred mountain. Important elements of the palace were the secret vital energy chain of feng shui (風水氣脈) and the forbidden stream (禁川). The secret vital energy chain of feng shui was the gateway to the secret vital energy for the king, and the forbidden stream was a method of preventing the king from leaving the palace grounds. Gyeongbokgung Palace, which is on typical feng shui terrain, faithfully reflects the principles of feng shui. On the other hand, the secondary palace was built on incomplete and irregular feng shui terrain. Feng shui was part of the nature and the geography of the ruling classes in the Joseon Dynasty. By examining their geography, I believe that the perfection of traditional culture inheritance and restoration can be improved.

• Korean Journal of Heritage: History & Science
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• v.54 no.1
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• pp.70-99
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• 2021

Yeong-am's 'Jeongwon (貞元)' stone monument, designated as the Jeollanam-do Cultural Heritage, is considered to be the oldest of the epigraphs in Jeollanam-do. Immediately after the discovery, the possibility of it being a Maehyangbi of Memorial Inscriptions was mentioned and attracted attention. However, there is an absolute age of the 'Jeongwon (貞元) of 2 years' (786), so despite it is a relatively early epigraph (金石文), there are not many papers on the theme related to this stone monument. I believe that this stone monument is a Maehyangbi (埋香碑). While reviewing and comparing the results of the existing research, I decoded the text from the 42nd character of the 4th line. As a result of the review, that was conducted, it was confirmed that this stone monument is truly a Maehyangbi (埋香碑). In particular, it was recorded in the literature of the late Joseon Dongguk-myungsanggi (東國名山記) that the letters of the Maehyangbi (埋香碑) are not recognizable. However, it is clearly stated that this stone monument is a Maehyangbi (埋香碑). Although there is no common expression for 'bury (埋)' or 'incense burial (埋香)' in the traditional Maehyangbi (埋香碑), which were popular in the late Goryeo and early Joseon Periods, it can be seen that it is a Maehyangbi (埋香碑) from the words "hide (呑藏)" and "10 bundles of fragrant incense (合香十束)" that are engraved on the stone monument with the name 'Jeongwon.' In other words, it is thought that it meant 'hide (呑藏)' instead of 'bury (埋)'. Circumstantial evidence for the monument of Jingamseonsa (眞鑑禪師), built in 888, contains the an epigraph from the Unified Silla Era. There is a phrase on it that says 'Plant incense on the shore (海岸植香)' on the monument of Jingamseonsa (眞鑑禪師), and it conveys its meaning without using the character 'bury (埋)'. As a result of the absence of the character 'bury (埋)' on the stone monument with the name 'Jeongwon', it is not considered as a Maehyangbi (埋香碑). However, there is evidence that the stone monument with the name 'Jeongwon (貞元)' is in fact a Maehyangbi (埋香碑) and it is also in the Geumpyoseok (禁標石; Forbidden Stone) around Gukjangsaeng (國長生) and at the entrance of Dogapsa Temple (道甲寺). The letters written on the gold sign suggest the possibility that the charcoal used to burn incense (香炭) at the royal tombs of King Jeongjo (正祖) was produced around at Dogapsa Temple (道甲寺) in Wolchulsan (月出山). Since the charcoal used to burn incense (香炭) is naturally related to incense (香), it has been shown that the area around Wolchulsan, where Dogapsa Temple is located, has a long history related to incense (香). The letters visible on the stone monument, the record of Dongguk-myungsanggi (東國名山記) in the late Joseon Dynasty, and the letters on the Geompyoseok (禁標石; Forbidden Stone), all show that the stone monument with the name 'Jeongwon (貞元)' is a Maehyangbi (埋香碑). Considering the fact that the earliest Maehyangbi (埋香碑) in existence is the Maehyangbi (埋香碑) in Yeongam (靈巖) Ippam-ri (笠巖里), which has two dates from 1371 at the end of Goryeo and 1410 at the beginning of Joseon, the stone monument with the name 'Jeongwon' which was set up in 786, would be the oldest Maehyangbi (埋香碑) that we know of. In addition, there is a historical significance in that the Maehyangbi (埋香碑) is proven in the record of Dongguk-myungsanggi (東國名山記), a document from the late Joseon period.