• 천문학회지
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• 제29권spc1호
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• pp.63-64
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• 1996

The nature of distant faint blue field galaxies remains a mystery, despite the fact that much attention has been devoted to this subject in the last decade. Galaxy counts, particularly those in the optical and near ultraviolet bandpasses, have been demonstrated to be well in excess of those expected in the 'no-evolution' scenario. This has usually been taken to imply that galaxies were brighter in the past, presumably due to a higher rate of star formation. More recently, redshift surveys of galaxies as faint as B$\~$24 have shown that the mean redshift of faint blue galaxies is lower than that predicted by standard evolutionary models (de-signed to fit the galaxy counts). The galaxy number count data and redshift data suggest that evolutionary effects are most prominent at the faint end of the galaxy luminosity function. While these data constrain the form of evolution of the overall luminosity function, they do not constrain evolution in individual galaxies. We are carrying out a series of observations as part of a long-term program aimed at a better understanding of the nature and amount of luminosity evolution in individual galaxies. Our study uses the luminosity-linewidth relation (Tully-Fisher relation) for disk galaxies as a tool to study luminosity evolution. Several studies of a related nature are being carried out by other groups. A specific experiment to test a 'no-evolution' hypothesis is presented here. We have used the AUTOFIB multifibre spectro-graph on the 4-metre Anglo-Australian Telescope (AAT) and the Rutgers Fabry-Perot imager on the Cerro Tolalo lnteramerican Observatory (CTIO) 4-metre tele-scope to measure the internal kinematics of a representative sample of faint blue field galaxies in the red-shift range z = 0.15-0.4. The emission line profiles of [OII] and [OIII] in a typical sample galaxy are significantly broader than the instrumental resolution (100-120 km $s^{-l}$), and it is possible to make a reliable de-termination of the linewidth. Detailed and realistic simulations based on the properties of nearby, low-luminosity spirals are used to convert the measured linewidth into an estimate of the characteristic rotation speed, making statistical corrections for the effects of inclination, non-uniform distribution of ionized gas, rotation curve shape, finite fibre aperture, etc.. The (corrected) mean characteristic rotation speed for our distant galaxy sample is compared to the mean rotation speed of local galaxies of comparable blue luminosity and colour. The typical galaxy in our distant sample has a B-band luminosity of about 0.25 L$\ast$ and a colour that corresponds to the Sb-Sd/Im range of Hub-ble types. Details of the AUTOFIB fibre spectroscopic study are described by Rix et al. (1996). Follow-up deep near infrared imaging with the 10-metre Keck tele-scope+ NIRC combination and high angular resolution imaging with the Hubble Space Telescope's WFPC2 are being used to determine the structural and orientation parameters of galaxies on an individual basis. This information is being combined with the spatially resolved CTIO Fabry-Perot data to study the internal kinematics of distant galaxies (Ing et al. 1996). The two main questions addressed by these (preliminary studies) are: 1. Do galaxies of a given luminosity and colour have the same characteristic rotation speed in the distant and local Universe? The distant galaxies in our AUTOFIB sample have a mean characteristic rotation speed of $\~$70 km $s^{-l}$ after correction for measurement bias (Fig. 1); this is inconsistent with the characteristic rotation speed of local galaxies of comparable photometric proper-ties (105 km $s^{-l}$) at the > $99\%$ significance level (Fig. 2). A straightforward explanation for this discrepancy is that faint blue galaxies were about 1-1.5 mag brighter (in the B band) at z $\~$ 0.25 than their present-day counterparts. 2. What is the nature of the internal kinematics of faint field galaxies? The linewidths of these faint galaxies appear to be dominated by the global disk rotation. The larger galaxies in our sample are about 2"-.5" in diameter so one can get direct insight into the nature of their internal velocity field from the $\~$ I" seeing CTIO Fabry-Perot data. A montage of Fabry-Perot data is shown in Fig. 3. The linewidths are too large (by. $5\sigma$) to be caused by turbulence in giant HII regions.

• 대한수의학회지
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• 제23권2호
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• pp.137-148
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• 1983

This study was made for the better information of the male reproductive system on the meat-type drake, Cherry Belly X White Golden. The epithelium of ductules of epididymal region and deferent duct were observed histologically and histochemically with the progress of their development. India-ink absorbability on the luminal epithelium was also investigated after the administration of India-ink. The results are as follows; 1. Rete testis and various round ductules in immature form appeared in epididymis within 6 weeks after hatching, and simple cuboidal and simple columnar epithelium were found in the epithelia of the ductules within 8 weeks after hatching. Larger ductules were found on epididymal surface which was in the developing stage near to the immature efferent ductule. From 10th to 20th week, various ductules appeared in epididymis, and developing form of efferent ductules were much more increased on epididymal surface. The luminal epithelium of the ductules were composed of ciliated simple columnar and pseudostratified ciliated columnar cells. At the same time, deferent duct appeared. From the 21th week, various ductules in epididymis became abruptly matured. Lumen of rete testis was lined by simple squamous or simple cuboidal epithelium, and that of efferent ductules, having many folds and being larger than any others were lined by pseudostratified ciliated columnar epithelium in which ciliated columnar cells, non-ciliated cells(clear cells) and basal cells were noted. Connecting tubules of star shaped lumen were composed of pseudostratified ciliated columnar epithelium in which ciliated columnar cells, nonciliated cells, and basal cells were observed. The luminal surface of epididymal ducts was smooth and has thick pseudostratified columnar epithelium which was composed of high columnar cells and basal cells. From 26th week after hatching, sperm pooling was started in various ductules. 2. From 4th to 10th week, simple cuboidal epithelium of deferent duct transformed to simple columnar epithelium with the progress of aging. At the basement of epithelium, clear round cells were noted. From 12th to 20th week, high columnar cells with enlongated nucleus were noted on the luminal border of deferent ducts, forming folds of pseuclostratified columnar epithelium. From 20th week, the deferent duct started to have septa in it's lumen and composed mainly of pseudostratified columnar epithelium, and round cells disappeared. From 20th week, the lumen diameter of deferent duct became wider with the progress of aging, but there was no difference among the values of lumen diameter in upper, middle, and lower part of deferent ducts. At 26th week, the pooling period of sperms in deferent ducts, the lumen diameter became rapidly widen, especially in the lower part of deferent ducts. Thickness of muscular layer of ductus deferens showed gradual growth within 24 weeks but did abrupt thickening from 26th week. 3. Saliva resistant PAS granules were dotted on the top of nucleus in efferent ductules epithelium but the amount of the granules were little in the connecting ductules's epithelium. The granules reactive to acid phosphatase were abundant in the some epithelial cells of efferent ductules and connecting ductules, especially above the nucleus of cells. The granules reactive to alkaline phosphatase were noted on the luminal border of efferent ductules. Parts of free border of efferent ductules and middle portion of deferent ducts were stained slightly by alcian blue technique. India ink granules were found mainly in the epithelium of efferent ductules but were few in that of connecting ductules.

• 지능정보연구
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• 제24권4호
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• pp.33-49
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• 2018

TV 드라마는 타 장르에 비해 시청률과 채널 홍보 효과가 매우 크며, 한류를 통해 산업적 효과와 문화적 영향력을 확인시켜줬다. 따라서, 이와 같은 드라마의 흥행 여부를 예측하는 일은 방송 관련 산업에서 매우 중요한 부분임은 주지의 사실이다. 이를 위해서 본 연구에서는 2003년부터 2012년까지 10년간, 지상파 채널을 통해 방송된, 총 280개의 TV 미니시리즈 드라마를 분석하였다. 이들 드라마 중 평균 시청률 상위 45개, 하위 시청률 45개를 선정하여 흥행 드라마의 시청시간 분포 (5%~100%, 11-Step) 모형을 만들었다. 이들 기준 모형과 신규 드라마의 시청시간 분포와의 이격 거리를 Euclidean/Correlation으로 측정한 유사도(Similarity)를 통해, 시청자의 초기(1~5회) 시청시간 분포로 신규 드라마의 성패 여부를 예측하는 모델을 만들었다. 또한 총 방송 시간 중 70% 이상 시청한 시청자를 열혈 시청층(이하 열혈층) 으로 분류하고, 상위/하위 드라마의 평균값과 비교하여, 신규 드라마의 흥행여부를 판별할 수 있도록 설계하였다. 연구 결과 드라마의 초반 시청자 충성도(시청시간)는 드라마의 대흥행 여부를 예측하는데 중요한 요소임을 밝혔으며, 최대 75.47%의 확률로 대흥행 드라마의 탄생을 예측할 수 있었다.

• 천문학회지
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• 제24권2호
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• pp.217-271
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• 1991

We have observed dense core around young stellar objects, DR21, S140, Orion-KL, and L1551 using four millimeter-wave transitions of $HC_3N\;J$=4-3, J=5-4, J=10-9, and J=12-11. The spatial distribution of $HC_3N$ emission closely resembles the morphology of the previous CS observations that trace high density gas. These observations reveal the existence of $HC_3N$ dense cores around central IR source, elliptical in shape and almost perpendicular to the CO bipolar outflow axis. Small differences can be explained by that $HC_3N$ molecular line is more optically thin and is seen to be more detailed structure in the neighborhood of central IR sources. In S140 and Orion-KL, massive(${\sim}10\;M_{\odot}$), slowly rotating dense cores lie near at the central IR sources of bipolar outflows. The velocity channel maps of DR21 show that the bipolar outflow gas may have a correlation with the dense core of DR21. We analyzed intensities of the four lines to derive physical conditions in dense core from two methods, LTE and LVG. The column density of $HC_3N$, $N(HC_3N)$, between LTE and LVG calculations agree well with each other. The abundances of $HC_3N$ in each observing source have been estimated using the average values of $n(H_2)$ and $N(HC_3N)$ and assuming the size of dense core. The fractional $HC_3N$ abundances in massive dense cores of DR21, S140, and Orion-KL have a range of $(2-7){\times}10^{-10}$, while that of low mass dense core, L1551, has one order of magnitude greater value of $2{\times}10^{-9}$. This should be considered good agreement with the result by Morris et al.(1976). It may be considered that dense cores of DR21, S140, and Orion-KL may have almost same stage of chemical evolution, and their abundances have a small values relative to that of L1551. The column density $N(HC_3N)$ decreases with increasing distance from the densest part of the cloud, the central infrared source, and have the relation of $N(HC_3N){\varpropto}R^{\alpha}$, where a has a range of 0.65 to 0.89. The values of $n(H_2)$ are not varied with increasing distance from the dense core, and have almost same values. Therefore, it is considered that the dense cores in these regions probably consist of dense clumps in diffuse molecular gas medium, and $n(H_2)$ of each clump is ${\sim}10^5\;cm^{-3}$. Levels in the $T_{ex}$ increases with $n(H_2)$. It is considered that the $HC_3N$ dense cores are not completely thermalized. We examine the relationships between the luminosity of central infrared sources versus mass of the dense cores, and the luminosity of central infrared sources versus molecular hydrogen column density. Luminosities of the central IR sources show good correlation with mass and hydrogen column density of the dense core. Same has been found from CS observations. However, mass and size derived from $HC_3N$ observations are one order of magnitude smaller than those from CS. It can be interpreted that we see more central part of the cloud cores in $NC_3N$ lines than CS lines.

• 만화애니메이션 연구
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• 통권6호
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• pp.152-171
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• 2002

This study analyses the avatar service, which is recognized as an alternative strategy of animation industry. The research questions of this study are following: (1) How have the avatar services been developed and what are the present dominant types? (2) Which structural characteristics of e-business environment are needed for the success of avatar services? (3) What is the economic characteristics of avatar business model? To solve these research questions, the basic conditions and the structural characteristics of avatar services have been investigated. In the first place, two forms of avatar service are classified. One is the internet service site whole primary service is to provide chatting service based on avatar service. The other is the portal site in which many kinds of products and services are presented as bundles to meet the needs of internet users. So avatar service is one of bundles which those portal sites are providing with. In this study, the big five internet service sites are selected based on the profits they earned through the sales of avatar service. The result of analysis is that the pricing strategy of those big five sites is very different from those of traditional off-line markets. The pricing mechanism are based on the value which internet users endow with the avatar items, not based on the costs of making the products. Avatar is the representative informative goods. The informative goods have the original cost structures, constant fixed costs and zero marginal costs, so the providers of avatar services make much of the subjective values of consumers. The sayclub, which is the most successful avatar service site and earn the average sales of 3 billing won a month, takes the aggressive strategy of pricing avatar items at highest price in the industry. The avatar service providers which make lots of profits are planning of making differentiate the services, introducing well-known brand items and star-named items. Nevertheless, the fact that the members of the sayclub are not decreasing means that the network effect of the site is so strongly manifest. Moreover, the costs the members have paid for the avatar items are so big not as to switch from one site to the other site, it can be very costly. These switching costs are endemic in high-technology industries and digital contents industries. It can be so large that switching suppliers is virtually unthinkable, a situation known as 'lock-in'. When switching costs are substantial, competition can be intense to attract new customers, since, one they are locked in, they can be a substantial source of profit. The consumers of avatar items have switching costs if they subscribe for the new avatar service site. The switching costs can be subscription costs as well as the costs of giving up the items they already paid for. One common example of switching costs involves specialized supplies, as with inkjet printer cartridges. In this example, the switching cost is the purchase of a new printer. The market is competitive ex ante, but since cartridges are incompatible, it is monopolized dx post. So the providers of printer/cartridges set pricing printer so cheap and cartridges expensive. On the contrary, since the avatar service can be successful with the strong network effect, the providers of avatar services have to compete aggressively for new customers. So they allow the subscription at a low price(almost marginal cost) in the early market. The network effect can be maximized when the members are sufficiently growing. The providers which have the monopoly power with sufficient subscribers. begin to raise the prices over the lifetime of the product and make profits.

• 지능정보연구
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• 제17권2호
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• pp.39-60
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• 2011

웹 2.0 기술이 소개된 이후 소셜 네트워크 서비스는 미래 정보기술의 기초로서 중요하게 인식되고 있다. 이에, 웹2.0 환경에서 소셜 네트워크를 구축하기 위하여 온톨로지 기반의 사용자 프로필 기술 도구인 FOAF를 활용하기 위한 다양한 연구가 이뤄지고 있다. 그러나 FOAF를 이용하여 소셜 네트워크를 생성 및 관리하는 대부분의 방법은 시간의 흐름에 따라 변화하는 사용자의 소셜 네트워크를 자동적으로 반영하기 어려운 단점이 있으며 다양한 소셜 미디어 서비스가 제공되는 환경에서는 FOAF를 동적으로 관리하기가 쉽지 않다. 따라서 본 논문에서는 기존 FOAF를 이용한 소셜 네트워크 추출방법의 한계를 극복하기 위하여 사용자 프로파일 기술 언어인 FOAF와 웹 저작물 출판 매커니즘인 RSS를 OLAP 시스템에 적용시켜 동적으로 FOAF를 갱신하고 관리하기 위한 방법을 제안한다. 본 논문에서 제안하는 방법은 수집한 FOAF와 RSS 파일들을 스타스키마로 설계된 데이터베이스에 넣어 OLAP 큐브를 생성한다. 그리고 OLAP 연산을 이용하여 사용자의 연결관계를 분석하고 FOAF에 그 결과를 반영한다. 본 논문에서 제안하는 방법은 이기종 분산처리 환경 하에서 데이터의 상호호환성을 보장할 뿐만 아니라 시간의 흐름에 따른 사용자의 관심 및 이슈 등의 변화를 효과적으로 반영한다.

• 천문학회지
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• 제12권1호
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• pp.41-70
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• 1979

From $B\ddot{o}hm$-Vitense's atmospheric model calculations, the relations, [$T_e$, (B-V)] and [B.C, (B-V)] with respect to heavy element abundance were obtained. Using these relations and evolutionary model calculations of Rood, and Sweigart and Gross, analytic expressions for some physical parameters relating to the C-M diagrams of globular clusters were derived, and they were applied to 21 globular clusters with observed transition periods of RR Lyrae variables. More than 20 different parameters were examined for each globular cluster. The derived ranges of some basic parameters are as follows; $Y=0.21{\sim}0.33,\;Z=1.5{\times}10^{-4}{\sim}4.5{\times}10^{-3},\;age,\;t=9.5{\sim}19{\times}10^9$ years, mass for red giants, $m_{RG}=0.74m_{\odot}{\sim}0.91m_{\odot}$, mass for RR Lyrae stars, $m_{RR}=0.59m_{\odot}{\sim}0.75m_{\odot}$, the visual magnitude difference between the turnoff point and the horizontal branch (HB), ${\Delta}V_{to}=3.1{\sim}3.4(<{\Delta}V_{to}>=3.32)$, the color of the blue edge of RR Lyrae gap, $(B-V)_{BE}=0.17{\sim}0.21=(<(B-V)_{BE}>=0.18),\;[\frac{m}{L}]_{RR}=-1.7{\sim}-1.9$, mass difference of $m_{RR}$ relative to $m_{RG},(m_{RG}-m_{RR})/m_{RG}=0.0{\sim}0.39$. It was found that the ranges of derived parameters agree reasonably well with the observed ones and those estimated by others. Some important results obtained herein can be summarized as follows; (i) There are considerable variations in the initial helium abundance and in age of globular clusters. (ii) The radial gradient of heavy element abundance does exist for globular clusters as shown by Janes for field stars and open clusters. (iii) The helium abundance seems to have been increased with age by massive star evolution after a considerable amount (Y>0.2) of helium had been attained by the Big-Bang nucleosynthesis, but there is not seen a radial gradient of helium abundance. (iv) A considerable amount of heavy elements ($Z{\sim}10{-3}$) might have been formed in the inner halo ($r_{GC}$<10 kpc) from the earliest galactic co1lapse, and then the heavy element abundance has been slowly enriched towards the galactic center and disk, establishing the radial gradient of heavy element abundance. (v) The final galactic disk formation might have taken much longer by about a half of the galactic age than the halo formation, supporting a slow, inhomogeneous co1lapse model of Larson. (vi) Of the three principal parameters controlling the morphology of C-M diagrams, it was found that the first parameter is heavy clement abundance, the second age and the third helium abundance. (vii) The globular clusters can be divided into three different groups, AI, BI and CII according to Z, Y an d age as well as Dickens' HB types. BI group clusters of HB types 4 and 5 like M 3 and NGC 7006 are the oldest and have the lowest helium abundance of the three groups. And also they appear in the inner halo. On the other hand, the youngest AI clusters have the highest Z and Y, and appear in the innermost halo region and in the disk. (viii) From the result of the clean separations of the clusters into three groups, a three dimensional classification with three parameters, Z, Y and age is prsented. (ix) The anomalous C-M diagrams can be expalined in terms of the three principal parameters. That is, the anomaly of NGC 362 and NGC 7006 is accounted for by the smaller age of the order of $1{\sim}2{\times}10^9$ years rather than by the helium abundance difference, compared with M 3. (x) The difference in two Oosterhoff types I and II can be explained in terms of the mean mass difference of RR Lyrae variables rather than in terms of the helium abundance difference as suggested by Stobie. The mean mass of the variables in Oosterhoff type I clusters is smaller by $0.074m_{\odot}$ which is exactly consistent with Rood's estimate. Since it was found that the mean mass of RR Lyrae stars increases with decreasing Z, the two Oosterhoff types can be explained substantially by the metal abundance difference; the type II has Z<$3.4{\times}10^{-4}$, and the type I has higher Z than the type II.

• 벤처창업연구
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• 제11권3호
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• pp.97-109
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• 2016

우리나라의 신생기업은 5년 후 생존율이 29.6%로 낮아진다. 이는 초기의 창업기업들이 중견기업에 비해 자원이 풍부하지 못하기 때문에 생존율이 낮다고 볼 수 있다. 따라서 창업기업의 마케팅특성이 주요 원인으로 부각되고 있다. 이번 연구에서는 학습지향성, 마케팅경험, 경쟁지향성 등은 창업기업에 따라 다르게 소유하고 있으며, 특히 창업기업의 경우 마케팅전략에 미치는 영향은 다르게 조사될 수 있다고 판단되어 학습지향성, 마케팅경험, 경쟁지향성이 창업기업의 마케팅전략에 미치는 관계를 검정하였다. 이를 바탕으로 기업성과를 측정하여 창업기업의 대표자들에게 창업기업의 생태계에 관련된 내용을 시사하고자 하는데 목적을 두었다. 본 연구의 표본은 2015년도를 기준으로 창업한지 3년 6개월 이내의 창업기업가들을 대상으로 2015년 11월 20일부터 12월 20일까지 창업 기업 종사자 250명을 대상으로 조사를 실시하였다. 이를 데이터클리닝 한 결과 207개의 표본을 대상으로 SPSS 20.0 통계프로그램을 이용하여 빈도분석, 신뢰도분석, 상관관계분석 및 회귀분석을 실시하여 다음과 같은 결론을 도출하였다. 독립변수인 창업기업의 마케팅환경이 매개변수인 마케팅전략에 미치는 영향은 학습지향성, 마케팅경험, 경쟁지향성에 있어 제품전략, 유통 전략, 촉진전략에 정(+)의 영향을 미치는 것으로 나타났으며, 매개변수인 마케팅전략이 종속변수인 기업성과에 미치는 영향에 대해 제품전략, 유통전략, 촉진전략은 재무성과와 비재무성과에 정(+)의 영향을 미치는 것으로 조사되었다. 또한 마케팅전략의 매개효과는 학습지향성, 마케팅경험, 경쟁지향성이 재무성과에 미치는 영향에 있어서 제품전략과 유통전략이 확실한 매개효과를 보이는 것으로 조사되었으며, 학습 지향성과 마케팅경험, 경쟁지향성이 비재무성과에 미치는 영향에 있어서 제품전략만이 매개효과를 보이는 것으로 조사되었다. 연구결과의 요약을 종합해보면 창업기업이 기업의 성과를 높이기 위해서 마케팅전략을 펼쳐야 하는데 특히 학습지향성과 마케팅경험이 중요시되며 창업마케팅특성이 기업성과를 높이는데 있어서 제품전략과 유통전략이 재무성과를 높일 수 있다. 그리고 제품전략은 재무성과와 비재무성과를 높인다고 볼 수 있다. 이에 창업기업 마케팅특성을 수행하는데 있어서 기업의 성과를 높이기 위해 창업마케팅특성에 따른 마케팅전략을 펼치는 것이 바람직하다고 사료된다.

• 철학연구
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• 제147권
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• pp.117-146
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• 2018

이 논문은 인공지능시대에도 종교는 가능한가, 오직 인간만이 종교신앙의 주체일 수 있는가, 인간의 마음을 탑재한 초지능기계들도 신앙의 주체일 수 있는가를 다룬다. 초지능기계들이 인간과 동일한 조건에서 신앙의 주체가 되려면, 인간의 고유한 특성인 감정, 의지, 자의식 등을 가질 수 있어야 한다. '특이점' 이후의 초지능기계들은 종교신앙의 주체를 넘어서서, 신과 같은 존재로서 인간과 자연과 세계를 지배하게 될 것이다. 이는 모라벡, 커즈와일, 하라리의 공통된 견해이다. 칸트가 구상한 '순수이성의 이념'과 '실천이성의 요청'으로서 신 개념은 제시 베링이 앞서 말한 것처럼 '간극의 신'처럼 보일 수 있다. 종교적 신앙 주체는 항상 도덕적인 선을 행하려고 부단하게 노력해야 하지만, 그런 노력 자체만으로는 완전선(完全善)에 도달할 수 없기 때문에 영혼불멸성을 요청하였다. 그러나 특이점을 넘어서 출현한 초지능기계가 지능폭발로 신적 지위를 가질 수 있다면, 인공지능로봇은 칸트적인 의미에서 종교적 수행을 불필요하게 여길 것이다. 에른스트 블로흐의 경우에는 초지능기계가 신적 존재라고 하더라도, 그것이 악신인가 선신인가를 비판적으로 물어야 한다. 칸트의 매트릭스에서는 선신일 수 있는 초지능기계가 블로흐의 매트릭스에서는 악신으로 추락할 수도 있다. 따라서 초지능기계-신이 우리를 유일한 종교신앙의 완성으로 이끌어 가는지, 인류와 지구촌의 몰락으로 내몰아갈 것인지를 부단하게 비판적으로 성찰해야 한다.

• 만화애니메이션 연구
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• 통권33호
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• pp.597-616
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• 2013

캐릭터산업은 저작권리를 중심으로 한 지식기반산업이면서 제조업과 서비스업의 판매가치를 촉진시키고 매출효과를 강화하는 보완재적 산업특성을 지니고 있어서 전 산업분야에 걸쳐 기능적으로 작동될 수 있는 창조경제의 핵심동력이다. 2003년부터 시작된 정부의 캐릭터관련 정책은 연관산업간의 연계효과 극대화, 국내 캐릭터의 해외진출확대, 유통구조 개선을 통한 저작권 강화, 캐릭터상품의 질적강화를 통한 산업기반 확대 등에 중점을 두었다. 이러한 정책성과로 인해, 2007년 이후, 연관콘텐츠의 성공사례가 구체화되기 시작했고, 국내외 캐릭터산업은 보다 체계적인 진화과정을 거치게 된다. 창작캐릭터의 자체적인 산업육성 노하우가 축적되고, 만화, 애니메이션, 게임, 소설, 영화, 뮤지컬 등으로 시작된 연관캐릭터가 시장세분화전략에 의해 활성화되면서 캐릭터산업의 범위 및 산업적 통계의 재설정이 요구되기 시작했다. 특히, 2009년 이후 정부는 '세계 5대 캐릭터 강국'으로의 목표를 설정하고, 글로벌 스타캐릭터 발굴, 연관산업간 네트워크 구축지원, 홍보채널 다양화 및 프로모션 강화, 라이선싱 비즈니스 활성화 등의 정책을 발굴하게 된다. 특히, 2013년을 기점으로 캐릭터를 활용한 캐릭터 체험전 등의 전시시장, 키즈카페 등의 시간관리형 캐릭터 실내테마파크, SNS의 이모티콘을 중심으로 한 디지털캐릭터 수요시장, 캐릭터 뮤지컬을 중심으로 한 공연시장 등 새로운 캐릭터시장이 지속적으로 개발되고, 기존 오프라인의 불법복제시장이 국내외적으로 대형화되면서 그에 따른 체계적인 정책대안이 필요하게 되었다. 진화하는 캐릭터 소비시장과 플랫폼 다양화 시대에 대응하여, 캐릭터산업을 활성화시키고 새로운 캐릭터디자인 및 관련 콘텐츠를 지원하기 위해서는 캐릭터산업의 정책변인을 전제로 한 전략방향의 입체적 설정이 요구된다. 지난 정부의 정책성과와 국내외 캐릭터산업의 시장현황, 그리고 진화방향을 분석하여 정책변인을 구체화시키면 다음과 같다. 현재 국내캐릭터산업의 정책변인은 플랫폼 다양화에 따른 디지털 캐릭터시장의 소비다층화, 한류중심의 캐릭터상품 융합콘텐츠화, 불법콘텐츠의 지하경제 양성화, 세분화된 시장의 수용자 편향성관리 등으로 분석되며, 이는 미국과 일본 및 유럽의 기존 캐릭터산업 강국들과는 다른 차원의 정책이슈를 발굴하게 된다. 결국 국내외시장의 연관콘텐츠 저작권계약 모델개발, 플랫폼 경제의 수익모델 다각화, 한류확대에 연계된 목표시장 추가개발, 평생캐릭터의 연령별 맞춤형 시장전략 등이 캐릭터 수요시장진화에 따른 대안으로 제시된다.