Sobolev approximation can be adopted to a macroscopic supersonic motion comparatively larger than a random (thermal) one. It has recently been applied not only to the winds of hot early type stars, but also to envelopes of late type giants and/or supergiants. However, since the ratio of wind velocity to stochastic one is comparatively small in the winds of these stars, the condition for applying the Sobolev approximation is not fulfilled any more. Therefore the validity of the Sobolev approximation must be checked. We have calculated exact P Cygni profiles with various velocity ratios, V∞/Vsto, using the accelerated lambda iteration method, comparing with those obtained by the Sobolev approximation. While the velocity ratio decrease, serious deviations have been occured over the whole line profile. When the gradual increase in the velocity structure happens near the surface of star, the amount of deviations become more serious even at the high velocity ratios. The investigations have been applied to observed UV line profile of CIV in the Copernicus spectrums of ʃ Puppis and NV of τ Sco. In case of τ Sco which has an expanding envelope with the gradual velocity increase in the inner region, The Sobolev approximation has given the serious deviations in the line profiles.

Bovine oocytes surrounded with compact cumulus cells were cultured for 20 to 22 hours(, 5% ) in modified TCM-199 medium supplemented with 5% superovulated cow serum(SCS) and inseminated by in vitro capacitated spermatozoa. Day 7 to 8 embryos were equilibrated for 10 minutes in 1.3M methyl cellosolve(MC) <1.1M diethylene glycol(DEG), 1.8M ethylene glycol(EG), 1.6M propylene glycol(PG) and 1.1 M 1,3-butylene glycol(BG) solutions. They were then loaded into 0.25ml straws, placed into an alcohol bath freezer at , cooled from to at /minute, seeded, held for 10 minutes, and stored in liquid nitrogen. After thawing in water, the embryos wee rehydrated in TCM-199 medium and then cultured for 48 hours in TCM-199 plus 5% SCS. Embryos were considered viable if they progressed to later developmental stages with a good morphology. Some of the embryos frozen in each cryoprotectant were thawed and transferred non-surgically without removing the cryoprotectant. Hatched embryos survived freezing and one-step dilution as follows : EG(50.0%), MC(53.6%), DEG(56.9%), PG(58.0%) and BG(11.5%). The survival rate of embryos cooled at vs. /minute was not significantly different(P<0.05), however, blastocysts hatched most often (P<0.01) in vitro when cooled at a rate of /minute(64.6%), 31/48) than at /minute(22.6%, 12/53). Pregnancy rates resulting from embryos frozen in the different cryoprotectants were as follows : MC(48%, 10/21); DEG(30%, 3/10); EG(74%, 20/27); and PG(40%, 4/10). These results indicate that MC, DEG, EG and PG have utility as cryoprotectants for the freezing and thawing of IVF Bovine embryos.

치밀 난구세포로 둘러싸인 소 난자를 . 5% 배양기에시 5% superovulated cow serum(SCS)이 첨가된 m-TCM 199 medium 으로 시간 배양하였으며, 수정능이 획득된 정자와 체외수정하였다. 7일8일경의 수정란을 1.3M methyl cellosolve(MC), 1.1M diethylene glycol(DEG), 1.8M ethylene glycol(EG), 1.6M propylene glycol(PG) 및 1.1M 1,3-butylene glycol(BG) 용액에서 10분간 평형시킨 후 0.25 ml 스트로내에 장전하였다. 스트로를 의 alcohol bath freezer에 넣고 까지 /분 속도로 냉각, 식빙 후 10분간 정체시켰으며, /분 또는 /분으로 까지 냉각 후 스트로를 액체질소에 침지하여 보관하였다. 수정란이 들어있는 스트로를 온수에서 융해하였으며, 수정란을 TCM 199 medium 으로 옮긴 후 5% SCS가 첨가된 TCM 199 medium 에서 48시간 배양하였다. 수정란이 양호한 형태를 유지하며 나중의 발육단계로 진행된 것을 생존한 것으로 간주하였다. 각 종류의 동해방지제에서 동결된 수정란의 일부는 융해 후 동해방지제를 제거하지 않고 직접 비외과적으로 이식하였다. 동결-융해 후 동해방지제의 종류에 따른 탈출배반포 발달율은 EG 50.0%, MC 53.6%, DEG 56.9%, PG 58.0% 그리고 BG 11.5%였다. /분 또는 /분 으로 냉각한 수정란의 생존율은 두 그룹간에 유의적인 차이가 없었으나 (P<0.05), 탈출배반포 발달율은 -0.5분 /분(22.6%, 12/53)보다 /분(64.6%, 31/48) 냉각시에 유의적으로 높았다(P<0.01). 동해방지제의 종류에 따른 수정란의 수태율은 MC 48%(10/21). DEG 30%(3/10), EG 74%(20/27) 및 PG 40%(4/10) 였다. 이러한 결과로 보아 MC, DEG, EG 그리고 PG는 소의 체외수정란의 동결을 위한 동해방지제로서 이용될 수 있음을 보여주었다.

We introduce the National Science Curriculum issued by the Education Ministry in Korea. Astronomy should be given and taught as compulsory courses in Nature of elementary school, Science of middle school, General Science of high school, and as elective courses in Earth Science I, II. Astronomy concepts have been designed in sprial pattern. College levels of astronomy have been given as majoring in astronomy course, cultivating one for earth science pre-teacher students and cultural subjects for non-major students

The evolution of solar magnetic arcades is investigated with the use of MHD simulations imposing resistivity on sheared magnetic fields. It is found that there is a critical amount of shear, over which magnetic reconnection can take place ill an arcade-like field geometry to create a magnetic island. The process leading to reconnect ion cannot. be solely attributed to a tearing instability, but rather to a reactive evolution of the magnetic arcade under resistivity. The natures of the arcade reconnection are governed by the spatial pattern of resistivity. A fast reconnection with a small shock angle can only be achieved when the diffusion region is localized. In this case. a highly collimated reconnect ion outflow can tear the plasmoid into a pair, and most of principal features in solar eruptive processes are reproduced.

We have solved the radiative transfer problem using a Sobolev approximation with an escape probability method in case of the supersonic expansion of a stellar envelope to an ambient medium. The radiation from the expanding envelope turns out to produce a P-Cygni type profile. In order to investigate the morphology of the theoretical P-Cygni type profile, we have treated V∞,Vsto,β (parameter for the velocity field), M and є (parameter for collisional effect) as model parametrs. We have found that the velocity field and the mass loss rate affect the shapes of the P-Cygni type profiles most effectively. The secondarily important factors are V∞, Vsto. The collisional effect tends to make the total flux increase but not so .much in magnitude. We have infered some physical parameters of 68 Cyg, HD24912, and ℇ persei such as V∞, M from the model calculation, which shows a good agreement with the observational results.

To understand the dynamical structures of stellar wind bubble, one and two-dimensional calculations has been performed. Using FCT Code with cooling effects and assuming constant mass loss rate and ambient medium density, we could divide stellar winds into the regime of slow and fast winds. The slow wind driven bubble shows initially radiative and becomes partially radiative bubble in which shocked stellar wind zone is still adiabatic. In contrast., the fast wind driven bubble shows initially fully adiabatic and becomes adiabatic bubbles with radiative outer shell. We also determine analytically the onset of thin-shell formation time in case of fast wind driven bubble with power-law energy injection and ambient density structure. We solve the line transfer problem with numerical results in order to calculate line profile of [OIII] forbidden line.

The results of the Crab pulsar observations with the photometrical MANIA (Multichannel Analysis of Nanosecond Intensity Alterations) complex at the 6-m telescope are presented. More than 12 millions photons in UBVR-bands simultaneously with time resolution of 10-7s were detected. Using the original software for search for optical pulsar period, we obtained the light curves of the object with time resolution of about 3.3 μs. Their detailed analysis gives the spectral change during pulse and subpulse, the shape of the pulse peaks, which are plateaus (with the duration of about 50 μs for the main pulse), limits for an amplitude of fine temporal (stochastic and regular) structure of pulse and sub pulse and the interpulse space intensity. The results of CCD-spectroscopy of the Crab pulsar show that its summarized spectrum is flat. There are no lines, neither emission nor absorbtion ones. Upper limit for line intensity or depth is 3.5% with the confidence probability of 95%.