미국교회와 文鮮明목사 –미국 성직자들과의 특별좌담-

Geore Ackley부부,R.L.Finney,鄭慶均,朴時仁 세계평화교수협의회 1985 廣場 Vol.142 No.-

Regionalization of Fertility Change Pattern and Its Explanation

Betsy Ackley,Park, Soon-Ho 慶北大學校 社會科學大學 地理學科 1992 地理學論究 Vol.- No.19

본 연구의 목적은 세계적 수준에서 출산율 변화의 공간패턴과 사회 · 경제 그리고 문화적 맥락에서 출산율수준의 변화에 영향을 미치는 핵심요소를 밝히는데 있다. 1965년에서 1990년까지의 총출산율 추세를 검토한 결과 6개 공간패턴으로 구분되었다. 각각의 패턴에 대하여 여성의 사회 · 경제적 지위, 보건서비스와 위생상태, 경제발달 그리고 문화적 요소를 통해 그 특성을 규명하였다. 전체 6개 패턴 중에서 패턴 I, V와 IV등 3개 패턴의 경우에는 출산율 수준은 사회 · 경제적 수준 보다는 오히려 문화적 요소에 의해서 결정되고 있다는 점에 가장 두드러진 특징이 있다. 즉 아프리카 토착종교와 이슬람교와 같은 문화적 요소들이 지배적인 요소로 작용하는 것으로 나타났다. 이들 종교는 가족수가 많은 것에 가치를 부여한다. 즉 이들 국가들에서는 종교적인 이유가 높은 출산수준을 야기했다. 따라서 출산율저하와 경제성장을 위한 각 국가의 노력들은 제한적이였고 그 결과는 고무적이지 못했다. 지금까지의 연구결과에 의하면 일반적으로 출산율감소를 위해서는 경제 · 사회발전, 여성의 지위향상, 의료 · 보건수준의 향상, 가족계획의 이용가능성 · 피임서비스의 증대가 효과적인 방법이라는 것이다. 그러나 아프리카의 개발도상국과 중동국가들의 경우에는 독특한 문화적 요소들로 이상의 일반론이 적용되지 않는다. 반면에 패턴 II의 국가는 중간계급의 등장과 경제발전의 결과로 출산율이 저하되었다. 이 중간계급의 성장은 일반적으로 가족수가 많은 것을 원하지 않는 새로운 소비패턴을 발생시켰다. 이는 출산율 감소에 기여했고 출산율 수준의 저하는 공공의료와 다른 사회서비스에서 향상에 의해 보조되었다. 패턴 III의 서구유럽국가들은 1900년대 이전에 대부분의 국가에서 출산율이 저하되기 시작되었기 때문에 그 요인이 무엇인가를 정확하게 측정하는 것이 어렵다. 그러나 일반적으로 경제발전과 사망률의 저하를 가장 중요한 요인으로 지적되어왔다. 마지막으로 패턴 IV는 최근에 점진적으로 출산율이 저하되고있는 라틴아메리카 국가들의 예이다. 이들 국가간에는 경제발전, 정치시스템, 인종구성, 문화적 배경과 인구정책이 차이가 있는 반면, 거의 모든 사례들은 급속한 변화를 발생시켰다. 이는 1차 의료관리, 특히 어머니와 어린이 건강향상에 주안점을 둔 결과라고 할 수 있다. 대부분의 패턴에 관련되는 일반적인 경향은 출산율 저하와 향상된 의료서비스간의 관련성이 매우 높은 점이다. 6개 패턴 중 5개의 경우에는 영아사망률이 중요한 요소로 밝혀졌다. 그러나 경제발전과 출산율저하와는 직접적인 관련성은 크지 않은 것으로 나타났다. 즉 경제발전이 더 이상 개발도상국이 직면하고있는 인구문제들에 대한 만병통치약이 될 수 없다는 점이다. 이상의 분석결과를 종합해 보면, 앞으로 세계적 수준에서 인구성장을 억제하기 위해서는 각 국가 혹은 지역별 사회 · 경제 · 문화적 맥락에서 철저한 연구분석결과에 기초하여 차별적으로 정책이 수립되고 집행되어야먄 할 것이다. The purpose of this study is to identify spatial pattern of global fertility and to discover the crucial factor that help to change the fertility level in the socio-economic and cultural context. Six patterns of fertility change are emerged through evaluating the trend of Total Fertility Rate change and socio-economic variables such as socio-economic status of women, health service and sanitary condition, and economic development from 1965 to 1990. Three patterns out of six patterns, namely I, V, and VI show that fertility levels are affected by cultural factors rather than the socio-economic development. Indigenous beliefs in Africa and Islamic beliefs figured predominantly in the analysis of each of theses patterns. The fertility levels of coutries in pattern II are affected by the emergence of a viable middle class as well as the implementation of the strong family planning policies. The countries found in pattern III are all developed countries with have already or nearly achieved replacement fertility. This transition from high to low fertility began for most of the countries prior to the 1900s. The countries in patterns IV have recently begun to decline in fertility rates as a result of the emphasis placed on improving primary health care, specifically maternal and child health as a part of family planning. The common thread connecting most of the patterns was the relationship between declining infant mortality rates. This realization may assist in providing a framework and allocating limited resources thereby significantly contributing to developing policies and plans for controlling population.

Regionalization of fertility change pattern and its explanation

Ackley, Betsy 慶北大學校 社會科學大學 地理學科 1999 地理學論究 Vol.- No.19

GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Afrough, M.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Agu American Physical Society 2017 Physical Review Letters Vol.119 No.14

<P>On August 14, 2017 at 10:30:43 UTC, the Advanced Virgo detector and the two Advanced LIGO detectors coherently observed a transient gravitational-wave signal produced by the coalescence of two stellar mass black holes, with a false-alarm rate of less than or similar to 1 in 27 000 years. The signal was observed with a three-detector network matched-filter signal-to-noise ratio of 18. The inferred masses of the initial black holes are 30.5(-3.0)(+5.7)M(circle dot) and 25.3(-4.2)(+2.8) M-circle dot (at the 90% credible level). The luminosity distance of the source is 540(-210)(+130) Mpc, corresponding to a redshift of z = 0.11(-0.04)(+0.03). A network of three detectors improves the sky localization of the source, reducing the area of the 90% credible region from 1160 deg(2) using only the two LIGO detectors to 60 deg(2) using all three detectors. For the first time, we can test the nature of gravitational-wave polarizations from the antenna response of the LIGO-Virgo network, thus enabling a new class of phenomenological tests of gravity.</P>

Search for Tensor, Vector, and Scalar Polarizations in the Stochastic Gravitational-Wave Background

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Afrough, M.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Agu American Physical Society 2018 Physical review letters Vol.120 No.20

<P>The detection of gravitational waves with Advanced LIGO and Advanced Virgo has enabled novel tests of general relativity, including direct study of the polarization of gravitational waves. While general relativity allows for only two tensor gravitational-wave polarizations, general metric theories can additionally predict two vector and two scalar polarizations. The polarization of gravitational waves is encoded in the spectral shape of the stochastic gravitational-wave background, formed by the superposition of cosmological and individually unresolved astrophysical sources. Using data recorded by Advanced LIGO during its first observing run, we search for a stochastic background of genetically polarized gravitational waves. We find no evidence for a background of any polarization, and place the first direct bounds on the contributions of vector and scalar polarizations to the stochastic background. Under log-uniform priors for the energy in each polarization, we limit the energy densities of tensor, vector, and scalar modes at 95% credibility to Omega(T)(0) < 5.58 x 10(-8), Omega(V)(0) < 6.35 x 10(-8), and Omega(S)(0) < 1.08 x 10(-7) at a reference frequency f(0) = 25 Hz.</P>

Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Afrough, M.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Agu American Astronomical Society 2017 ASTROPHYSICAL JOURNAL LETTERS - Vol.851 No.1

<P>The first observation of a binary neutron star (NS) coalescence by the Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors offers an unprecedented opportunity to study matter under the most extreme conditions. After such a merger, a compact remnant is left over whose nature depends primarily on the masses of the inspiraling objects and on the equation of state of nuclear matter. This could be either a black hole (BH) or an NS, with the latter being either long-lived or too massive for stability implying delayed collapse to a BH. Here, we present a search for GWs from the remnant of the binary NS merger GW170817 using data from Advanced LIGO and Advanced Virgo. We search for short-(less than or similar to 1 s) and intermediate-duration (less than or similar to 500 s) signals, which include GW emission from a hypermassive NS or supramassive NS, respectively. We find no signal from the post-merger remnant. Our derived strain upper limits are more than an order of magnitude larger than those predicted by most models. For short signals, our best upper limit on the root sum square of the GW strain emitted from 1-4 kHz is h(rss)(50%) = 2.1 x 10(-22) Hz(-1/2) detection efficiency. For intermediate-duration signals, our best upper limit at 50% detection efficiency is h(rss) (50%) = 8.4 x 10(-22) Hz(-1/2) for a millisecond magnetar model, and h(rss)(50%) = 5.9 x 10(-22) Hz(-1/2) for a bar-mode model. These results indicate that post-merger emission from a similar event may be detectable when advanced detectors reach design sensitivity or with next-generation detectors.</P>

Exploring the sensitivity of next generation gravitational wave detectors

Abbott, B P,Abbott, R,Abbott, T D,Abernathy, M R,Ackley, K,Adams, C,Addesso, P,Adhikari, R X,Adya, V B,Affeldt, C,Aggarwal, N,Aguiar, O D,Ain, A,Ajith, P,Allen, B,Altin, P A,Anderson, S B,Anderson, W Institute of Physics 2017 Classical and quantum gravity Vol.34 No.4

<P>The second-generation of gravitational-wave detectors are just starting operation, and have already yielding their first detections. Research is now concentrated on how to maximize the scientific potential of gravitational-wave astronomy. To support this effort, we present here design targets for a new generation of detectors, which will be capable of observing compact binary sources with high signal-to-noise ratio throughout the Universe.</P>

GW170817: Measurements of Neutron Star Radii and Equation of State

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Aguiar, O. D.,A American Physical Society 2018 Physical Review Letters Vol.121 No.16

<P>On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parametrization of the defining function p(rho) of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as R-1 = 10.8(-1.7)(+2.0) km for the heavier star and R-2 = 10.7(-1.5)(+2.1) km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than 1.97 M-circle dot as required from electromagnetic observations and employ the equation-of-state parametrization, we further constrain R-1 = 11.9(-1.4)(+1.4) km and R-2 = 11.9(-1.4)(+1.4) km at the 90% credible level. Finally, we obtain constraints on p(rho) at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5(-1.7)(+2.7) x 10(34) dyn cm(-2) at the 90% level.</P>

Multi-messenger Observations of a Binary Neutron Star Merger

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Afrough, M.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Agu American Astronomical Society 2017 ASTROPHYSICAL JOURNAL LETTERS - Vol.848 No.2

<P>On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of similar to 1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of 40(-8)(+8) Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M-circle dot. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at similar to 40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over similar to 10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position similar to 9 and similar to 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.</P>

GW170608: Observation of a 19 Solar-mass Binary Black Hole Coalescence

Abbott, B. P.,Abbott, R.,Abbott, T. D.,Acernese, F.,Ackley, K.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Adya, V. B.,Affeldt, C.,Afrough, M.,Agarwal, B.,Agathos, M.,Agatsuma, K.,Aggarwal, N.,Agu American Astronomical Society 2017 ASTROPHYSICAL JOURNAL LETTERS - Vol.851 No.2

<P>On 2017 June 8 at 02:01:16.49 UTC, a gravitational-wave (GW) signal from the merger of two stellar-mass black holes was observed by the two Advanced Laser Interferometer Gravitational-Wave Observatory detectors with a network signal-to-noise ratio of. 13. This system is the lightest black hole binary so far observed, with component masses of 12(2)(+7) M-circle dot and 7(2)(+2) M-circle dot (90% credible intervals). These lie in the range of measured black hole masses in low-mass X-ray binaries, thus allowing us to compare black holes detected through GWs with electromagnetic observations. The source's luminosity distance is 340(-140)(+140) Mpc, corresponding to redshift 0.07(-0.03)(+0.03). We verify that the signal waveform is consistent with the predictions of general relativity.</P>