Detection of Soil Microbial Activity by Infrared Thermography (irt)

Bjorn Kluge,Andre Peters,Jaane Krueger,Gerd Wessolek 한국토양비료학회 2014 한국토양비료학회 학술발표회 초록집 Vol.2014 No.6

Environmental Hazardousness of Spent Oil Shale: A Critical Review

( Jaan Habicht ) 한국폐기물자원순환학회 2011 ISWA Vol.2011 No.0

「國語」と「日本語」と

子安宣邦 한국일어일문학회 2003 日語日文學硏究 Vol.45 No.2

독일발트문학과 발트국 특집> : 신의 언어로서의 에스토니아어 - 언어숭배의 관점

얀운두스크 ( Jaan Undusk ) 한국독일어문학회 2014 독일어문학 Vol.65 No.-

본 논문은 단순히 에스토니아어와 독일어, 그리고 한국어와의 비교를 통한 유사 성에만 집중한 것은 아니다. ‘신의 언어’로 알려진 에스토니아어에 대한 자긍심을 바탕으로 에스토니아어를 새로운 관점, 즉 언어숭배의 관점에서 분석하고자 하였 다. 에스토니아어는 우랄어족에 핀-우그르어군 속하며, 알타이어족에 속하는 한국어 와 유사성을 갖고 있다. 이러한 측면에서 에스토니아어는 울림의 소리와 구문론적 특징, 어순의 배열이 인도-유럽어의 특징에 속하는 굴절어가 아니며, 교착어로서 언 어표현의 무한한 가능성을 가지고 있다. 이외에도 논문에서는 19세기 에스토니아 문학의 형성에 미친 독일어와 독일발트문학과의 관계도 함께 다루었다. 이 과정에서 에스토니아어는 한국어와의 비교 연구에서 새롭게 주목할 만한 특 징을 가지고 있음을 시사했으며, 이는 이 연구의 또 다른 목적이 되기도 한다.

위상배열 초음파 탐상장비의 현장 적용 방안

권세곤(Segon Kwon),서종민(Jongmin Seo),구자안(Jaan Gu),김영수(Youngsu Kim),성덕룡(Deok-Yong Sung) 한국철도학회 2020 한국철도학회논문집 Vol.23 No.8

직류 전기아크로를 제어하기 위한 전원장치로서의 AC/DC 공진형 컨버터

유병우(Byoung-woo Ryu),최재호(Jae-ho Choi),Jaan Jarvik 전력전자학회 2002 전력전자학술대회 논문집 Vol.- No.-

본 논문에서는 직류 전기아크로의 전원장치로서 AC/DC 공진형 컨버터가 묘사된다. 또한 무효전력을 보상하기 위한 커패시터와 인덕터를 각각 직렬과 병렬로 연결되어 있다. 그러므로 무부하부터 단락회로까지의 범위에서 역률이 매우 높다. 이 컨버터는 직류 아크로의 전원장치로서 매우 적당하다.

Infalling groups and galaxy transformations in the cluster A2142

Einasto, Maret,Deshev, Boris,Lietzen, Heidi,Kipper, Rain,Tempel, Elmo,Park, Changbom,Gramann, Mirt,Heinä,mä,ki, Pekka,Saar, Enn,Einasto, Jaan Springer-Verlag 2018 Astronomy and astrophysics Vol.610 No.-

<P><I>Context.</I> Superclusters of galaxies provide dynamical environments for the study of the formation and evolution of structures in the cosmic web from galaxies, to the richest galaxy clusters, and superclusters themselves.</P><P><I>Aims.</I> We study galaxy populations and search for possible merging substructures in the rich galaxy cluster A2142 in the collapsing core of the supercluster SCl A2142, which may give rise to radio and X-ray structures in the cluster, and affect galaxy properties of this cluster.</P><P><I>Methods.</I> We used normal mixture modelling to select substructure of the cluster A2142. We compared alignments of the cluster, its brightest galaxies (hereafter BCGs), subclusters, and supercluster axes. The projected phase space (PPS) diagram and clustercentric distributions are used to analyse the dynamics of the cluster and study the distribution of various galaxy populations in the cluster and subclusters.</P><P><I>Results.</I> We find several infalling galaxy groups and subclusters. The cluster, supercluster, BCGs, and one infalling subcluster are all aligned. Their orientation is correlated with the alignment of the radio and X-ray haloes of the cluster. Galaxy populations in the main cluster and in the outskirts subclusters are different. Galaxies in the centre of the main cluster at the clustercentric distances 0.5 h<SUP>−1</SUP> Mpc (<I>D</I>c∕<I>R</I>vir < 0.5, <I>R</I>vir = 0.9 h<SUP>−1</SUP> Mpc) have older stellar populations (with the median age of 10−11 Gyr) than galaxies at larger clustercentric distances. Star-forming and recently quenched galaxies are located mostly at the clustercentric distances <I>D</I>c ≈ 1.8 h<SUP>−1</SUP> Mpc, where subclusters fall into the cluster and the properties of galaxies change rapidly. In this region the median age of stellar populations of galaxies is about 2 Gyr. Galaxies in A2142 on average have higher stellar masses, lower star formation rates, and redder colours than galaxies in rich groups. The total mass in infalling groups and subclusters is <I>M</I> ≈ 6 × 10<SUP>14</SUP> h<SUP>−1</SUP><I>M</I>⊙, that is approximately half of the mass of the cluster. This mass is sufficient for the mass growth of the cluster from redshift <I>z</I> = 0.5 (half-mass epoch) to the present.</P><P><I>Conclusions.</I> Our analysis suggests that the cluster A2142 has formed as a result of past and present mergers and infallen groups, predominantly along the supercluster axis. Mergers cause complex radio and X-ray structure of the cluster and affect the properties of galaxies in the cluster, especially at the boundaries of the cluster in the infall region. Explaining the differences between galaxy populations, mass, and richness of A2142, and other groups and clusters may lead to better insight about the formation and evolution of rich galaxy clusters.</P>

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Einasto, Maret,Gramann, Mirt,Park, Changbom,Kim, Juhan,Deshev, Boris,Tempel, Elmo,Heinä,mä,ki, Pekka,Lietzen, Heidi,Lä,hteenmä,ki, Anne,Einasto, Jaan,Saar, Enn EDP Sciences 2018 Astronomy and astrophysics Vol.620 No.-

<P><I>Context</I>. Superclusters with collapsing cores represent dynamically evolving environments for galaxies, galaxy groups, and clusters.</P><P><I>Aims</I>. We study the dynamical state and properties of galaxies and groups in the supercluster SCl A2142 that has a collapsing core, to understand its possible formation and evolution.</P><P><I>Methods</I>. We find the substructure of galaxy groups using normal mixture modelling. We have used the projected phase space (PPS) diagram, spherical collapse model, clustercentric distances, and magnitude gap between the brightest galaxies in groups to study the dynamical state of groups and to analyse group and galaxy properties. We compared the alignments of groups and their brightest galaxies with the supercluster axis.</P><P><I>Results</I>. The supercluster core has a radius of about 8 <I>h</I><SUP>−1</SUP> Mpc and total mass <I>M</I>tot ≈ 2.3 × 10<SUP>15</SUP> h<SUP>−1</SUP><I>M</I>⊙ and is collapsing. Galaxies in groups on the supercluster axis have older stellar populations than off-axis groups, with median stellar ages 4 − 6 and < 4 Gyr, correspondingly. The cluster A2142 and the group Gr8 both host galaxies with the oldest stellar populations among groups in SCl A2142 having the median stellar age <I>t</I> > 8 Gyr. Recently quenched galaxies and active galactic nuclei (AGNs) are mostly located at virial radii or in merging regions of groups, and at clustercentric distances <I>D</I>c ≈ 6 <I>h</I><SUP>−1</SUP> Mpc. The most elongated groups lie along the supercluster axis and are aligned with it. Magnitude gaps between the brightest galaxies of groups are less than one magnitude, suggesting that groups in SCl A2142 are dynamically young.</P><P><I>Conclusions</I>. The collapsing core of the supercluster, infall of galaxies and groups, and possible merging groups, which affect galaxy properties and may trigger the activity of AGNs, show how the whole supercluster is evolving.</P>

Tracing a high redshift cosmic web with quasar systems

Einasto, Maret,Tago, Erik,Lietzen, Heidi,Park, Changbom,Heinä,mä,ki, Pekka,Saar, Enn,Song, Hyunmi,Liivamä,gi, Lauri Juhan,Einasto, Jaan EDP Sciences 2014 Astronomy and astrophysics Vol.568 No.1

<P>Context. To understand the formation, evolution, and present-day properties of the cosmic web we need to study it at low and high redshifts. Aims. We trace the cosmic web at redshifts that range from 1.0 ≤ z ≤1.8 by using the quasar (QSO) data from the SDSSDR7QSO catalogue. Methods. We apply a friend-of-friend algorithm to the quasar and random catalogues to determine systems at a series of linking length and analyse richness and sizes of these systems. Results. At the linking lengths l ≤ 30 h<SUP>−1</SUP> Mpc, the number of quasar systems is larger than the number of systems detected in random catalogues, and the systems themselves have smaller diameters than random systems. The diameters of quasar systems are comparable to the sizes of poor galaxy superclusters in the local Universe. The richest quasar systems have four members. The mean space density of quasar systems, ≈10<SUP>−7</SUP> (h<SUP>−1</SUP> Mpc)<SUP>−3</SUP>, is close to the mean space density of local rich superclusters. At intermediate linking lengths (40 ≤ l ≤70 h<SUP>−1</SUP> Mpc), the richness and length of quasar systems are similar to those derived from random catalogues. Quasar system diameters are similar to the sizes of rich superclusters and supercluster chains in the local Universe. The percolating system, which penetrate the whole sample volume appears in a quasar sample at a smaller linking length than in random samples (85 h<SUP>−1</SUP> Mpc). At the linking length 70 h<SUP>−1</SUP> Mpc, the richest systems of quasars have diameters exceeding 500 h<SUP>−1</SUP> Mpc. Quasar luminosities in systems are not correlated with the system richness. Conclusions. Quasar system catalogues in our web pages and at the Strasbourg Astronomical Data Center (CDS) serve as a database for searching superclusters of galaxies and for tracing the cosmic web at high redshifts.</P>

Precession and atmospheric CO₂ modulated variability of sea ice in the central Okhotsk Sea since 130,000 years ago

Lo, Li,Belt, Simon T.,Lattaud, Julie,Friedrich, Tobias,Zeeden, Christian,Schouten, Stefan,Smik, Lukas,Timmermann, Axel,Cabedo-Sanz, Patricia,Huang, Jyh-Jaan,Zhou, Liping,Ou, Tsong-Hua,Chang, Yuan-Pin Elsevier 2018 Earth and planetary science letters Vol.488 No.-

<P><B>Abstract</B></P> <P>Recent reduction in high-latitude sea ice extent demonstrates that sea ice is highly sensitive to external and internal radiative forcings. In order to better understand sea ice system responses to external orbital forcing and internal oscillations on orbital timescales, here we reconstruct changes in sea ice extent and summer sea surface temperature (SSST) over the past 130,000 yrs in the central Okhotsk Sea. We applied novel organic geochemical proxies of sea ice (IP<SUB>25</SUB>), SSST ( TEX L 86 ) and open water marine productivity (a tri-unsaturated highly branched isoprenoid and biogenic opal) to marine sediment core MD01-2414 (53°11.77′N, 149°34.80′E, water depth 1123 m). To complement the proxy data, we also carried out transient Earth system model simulations and sensitivity tests to identify contributions of different climatic forcing factors. Our results show that the central Okhotsk Sea was ice-free during Marine Isotope Stage (MIS) 5e and the early-mid Holocene, but experienced variable sea ice cover during MIS 2–4, consistent with intervals of relatively high and low SSST, respectively. Our data also show that the sea ice extent was governed by precession-dominated insolation changes during intervals of atmospheric CO<SUB>2</SUB> concentrations ranging from 190 to 260 ppm. However, the proxy record and the model simulation data show that the central Okhotsk Sea was near ice-free regardless of insolation forcing throughout the penultimate interglacial, and during the Holocene, when atmospheric CO<SUB>2</SUB> was above ∼260 ppm. Past sea ice conditions in the central Okhotsk Sea were therefore strongly modulated by both orbital-driven insolation and CO<SUB>2</SUB>-induced radiative forcing during the past glacial/interglacial cycle.</P> <P><B>Highlights</B></P> <P> <UL> <LI> The first orbital timescale proxy-model sea ice-sea surface temperature records from the northwestern subarctic Pacific Ocean. </LI> <LI> Strong precession forcing controlled and sea ice variations are modulated by greenhouse gas radiative forcing. </LI> <LI> Sea ice remained free in the central Okhotsk Sea during MIS 5e due to high greenhouse gas radiative forcing. </LI> </UL> </P>