본 연구는 국내에서 육종한 품종인 ‘Pink Aurora’ 장미를 보존화로 가공하는 기술의 개발에 관한 것으로 탈수와 탈색 처리를 위한 에탄올의 침지시간과 염색을 위한 보존용액의 온도와 침지시간를 구명하고자 수행하였다. 탈수는 먼셀 H값에서 붉은 색이 완전히 빠지고 시간이 길어질수록 황색이 짙어짐을 고려해 볼 때 12시간이 가장 효과적이었다. 보존용액 처리에 서는 채도값을 나타내는 C의 차이는 크지 않았지만 온도가 높고 처리시간이 길어질수록 색의 맑기가 높아졌다. 낮은 온도 에서 침지시간이 길어짐에 따라 화형의 감소율이 낮았다. 24 시간 건조 후 무게는 모든 온도 처리에서 침지시간이 길어질 수록 53~47% 감소하였고, 건조 48시간의 25℃에서 6시간 침 지에서 73%, 24시간 침지에서 68%의 감소율을 나타내 침지시간이 길어질수록 감소율이 낮았다. 따라서 에탄올로 12시간동 안 탈수하여 염색 보존액을 25℃에서 24시간동안 처리하는 것이 가장 효과적이라고 생각된다.

Research on the useful mushroom was done at Aurora Memorial National Park (AMNP). The Park is situated in Central Luzon Region with a total land area of 5,676 hectares. AMNP has no distinct wet and dry season thus provides a favorable climate, which promotes the growth of useful mushrooms. The photo-documentation and collections were performed to assess diversity. Five Transect Lines (TL) were laid out in five areas, with 20m x 30m quadrat and interval of 100 meters between quadrats. The study resulted in the identification of 36 families, 53 genera, and 104 species of which 97 are basidiomycetes and 6 are ascomycetes. Simpson’s and Shannon diversity indexes resulted in 0.7254 and 1.4295, respectively. In both indexes, useful mushrooms at AMNP showed moderately diverse. While the evenness revealed 0.1565 indicating low species evenness in each TL. Among the significant findings revealed two new possible new species of Microporus and Cymatoderma.

Aurora A kinase is a mitotic serine/threonine kinase whose proposed functions include the maturation of centrosomes, G2/M transition, alignment of chromosomes at metaphase, and cytokinesis. In this study, we investigated the effect of MLN8237, an aurora A kinase inhibitor, on the postovulatory aging of oocytes based on the frequency of oocyte fragmentation, cdk1 kinase activity, and cyclin B degradation. The fragmentation of ovulated oocytes during prolonged culture was inhibited by treatment with MLN8237 in a concentration-dependent manner. The frequency of fragmented oocytes was significantly lower in oocytes treated with 2 μM MLN8237 (13%) than in control oocytes (64%) after two days of culture. Most of the control (non-fragmented) oocytes (91%) were activated after two days of culture. In comparison, only 22% of the MLN8237-treated oocytes were activated; the rest of the oocytes (78%) were still in metaphase with an abnormal spindle and dispersed chromosomes. Next, cdk1 activity and the level of cyclin B were examined. The level of cyclin B and cdk1 activity in MLN8237-treated oocytes were nearly equal to those in control oocytes. Our results indicate that MLN8237 inhibited the fragmentation of ovulated oocytes during prolonged culture, although it blocked the spontaneous decrease in activity of cdk1 and degradation of cyclin B. This mechanism of inhibition is different from that in oocytes treated with nocodazole, which have high levels of cdk1 activity and cyclin B.

Through the coupling between the near-earth space environment and the polar ionosphere via geomagnetic field lines, the variations occurred in the magnetosphere are transferred to the polar region. According to recent studies, however, the polar ionosphere reacts not only passively to such variations, but also plays active roles in modifying the near-earth space environment. So the study of the polar ionosphere in terms of geomagnetic disturbance becomes one of the major elements in space weather research. Although it is an indirect method, ground magnetic disturbance data can be used in estimating the ionospheric current distribution. By employing a realistic ionospheric conductivity model, it is further possible to obtain the distributions of electric potential, field-aligned current, Joule heating rate and energy injection rate associated with precipitating auroral particles and their energy spectra in a global scale with a high time resolution. Considering that the ground magnetic disturbances are recorded simultaneously over the entire polar region wherever magnetic station is located, we are able to separate temporal disturbances from spatial ones. On the other hand, satellite measurements are indispensible in the space weather research, since they provide us with in situ measurements. Unfortunately it is not easy to separate temporal variations from spatial ones specifically measured by a single satellite. To demonstrate the usefulness of ground magnetic disturbance data in space weather research, various ionospheric quantities are calculated through the KRM method, one of the magneto gram inversion methods. In particular, we attempt to show how these quantities depend on the ionospheric conductivity model employed.

We have analyzed the sunspot and aurora data recorded in Go-Ryer-Sa. We have collected 35 records of sunspot observations for 46 days, and 232 records of auroral observations. To objectively estimate the periods of the solar activity appearing in these records a method of calculating the one-dimensional power spectrum from inhomogeneous data is developed, and applied to the sunspot and auroral data. We have found statistically significant 10.5 and 10 year periodicities in the distributions of sunspot and aurora records, respectively. These periods are consistent with the well-known solar activity cycle. There are indications of the long-term variations, but the period is not certain. We have also calculated the cross-correlations between the sunspot and auroral data. In particular, we have divided the aurora data into several subgroups to study their nature. We conclude that the historical records of strong auroral activity correspond to non-recurrent magnetic storms related to the sunspots. On the other hand, the records of weak auroral activity are thought to be related with the recurrent magnetic storms which occur frequently due to the coronal hole near the sunspot minimum.

The auroral observation has been started at Jang Bogo Station (JBS), Antarctica by using a visible All-sky camera (v-ASC) in 2018 to routinely monitor the aurora in association with the simultaneous observations of the ionosphere, thermosphere and magnetosphere at the station. In this article, the auroral observations are introduced with the analysis procedure to recognize the aurora from the v-ASC image data and to compute the auroral occurrences and the initial results on their spatial and temporal distributions are presented. The auroral occurrences are mostly confined to the northern horizon in the evening sector and extend to the zenith from the northwest to cover almost the entire sky disk over JBS at around 08 MLT (magnetic local time; 03 LT) and then retract to the northeast in the morning sector. At near the magnetic local noon, the occurrences are horizontally distributed in the northern sky disk, which shows the auroral occurrences in the cusp region. The results of the auroral occurrences indicate that JBS is located most of the time in the polar cap near the poleward boundary of the auroral oval in the nightside and approaches closer to the oval in the morning sector. At around 08 MLT (03 LT), JBS is located within the auroral oval and then moves away from it, finally being located in the cusp region at the magnetic local noon, which indicates that the location of JBS turns out to be ideal to investigate the variabilities of the poleward boundary of the auroral oval from long-term observations of the auroral occurrences. The future plan for the ground auroral observations near JBS is presented.