We have performed the high resolution computer simulation with 1D spherical hydrodynamic code in order to study the dynamical evolution of supernova ejecta interacting with a pre-existing fast wind structure. The fast wind structure has been calculated with Min=3×10−6M⊙yr−1 Min=3×10−6M⊙yr−1 and υin=1000km/sec υin=1000km/sec , which velocity is higher than the critical velocity relating to the initial radiative cooling. The fast wind becomes initially adiabatic. After a shell formation time of ∼4000yrs ∼4000yrs , the wind becomes radiative cooling at the shell zone, forming a thin dense radiative shell and an adiabatic wind bubble afterward. When supernova explodes in the wind center at 20,000yrs after the wind evolves, the supernova ejecta, which has a dense distribution of ρ∝r−n ρ∝r−n (here we have n = 9), interacts initially with, the understood wind zone, producing forward and reverse shocks. The reverse shock heats the supernova ejecta and its temperature increases. In this study, as the mass of the supernova ejecta is larger than that of the wind shell (Mej=5M⊙ Mej=5M⊙ , Msw=2M⊙ Msw=2M⊙ ), we can conform two shell structures: an outer shell by the supernova ejecta and a secondarily shocked wind shell by it. The secondarily shocked wind shell should accelerates in this case to be R-T unstable, consequently producing the knots

It has been recognized that the morphologies of the SNRs from the radio observation are "barrel shaped". To interpret the mechanism of the radiation and the physical state of the environments, we have analytically calculated the dynamical structure of the interacting region in the case where the ejectum has a steep power-law density profile(ρ∼r−n ρ∼r−n ) and the ambient medium has a shallow power-law density profile(ρ∼r−s ρ∼r−s ), assuming that the cosmic rays are isotropically accelerated in the shock wave and the magnetic fields are very weak. The calculated synchrotron radio maps show that the emission from the equator is intense and the emissions from the central and polar regions are less intense. Also the thicknesses of the shell are strongly dependent on s and weakly on n. The azimuthal intensity ratio α α increases as the efficiency of the cosmic ray acceleration increases and s decreases. We compared the results with the morphology of the SNR A. D. 1006(type I SNR). It does agree with the case of s = 0, w = 0.3 - 0.5. This value for w is consistent with the results by Eichler(1979). It provides us the evidence of the cosmic ray acceleration in the shock wave.

We have developed a cylindrical mixing layer model of a stellar jet including cooling effect in order to understand an optical emission mechanism along collimated high velocity stellar jets associated with young stellar objects. The cylindrical results have been calculated to be the same as the 2D ones presented by Canto & Raga(1991) because the entrainment efficiency in our cylindrical model has been obtained to be the same value as the 2D model has given. We have discussed the morphological and physical characteristics of the mixing layers by the cooling effect. As the jet Mach number increases, the initial temperature of the mixing layer goes high because the kinetic energy of the jet partly converts to the thermal energy of the mixing layer. The initial cooling of the mixing layer is very severe, changing its outer boundary radius. A subsequent change becomes adiabatic. The number of the Mach disks in the stellar jet and the total radiative luminosity of the mixing layer, based on our cylindrical calculation, have quite agreed with the observations.

The environmental structure of T Tauri star can be understood by its continuum energy distribution. We suggest four evolutionary stages on the base of this environmental change from molecular cloud to the main sequence. A protostar is embedded in a dense envelope which can be attributed to the overall infrared region in continuum spectra. The infalling material from the envelope results in producing a hump in the mid-infrared region. This matter produces a surrounding disk around a central star afterwards. The disk emission changes the spectral index in the overall infrared region. The disk will be developed to a ring structure owing to the formation of planets by its instability and/or the cleaning effect of the inner region of the disk by a central star outflow, contributing to producing a hump in the far-infrared region. The pre-main sequence evolution points of T Tauri stars in H-R diagram strongly support the environmental structure evolution.

This study investigated the effects of variations in the kinetic structure on the science knowledge acquisition and analyzed the kinetic structure of a sience classroom communication. According to the rationale of the kinetic structure theory, a communication with high structure would facilitate greater knowledge acquisition than that with low structure. To testify that hypothesis, a modified non-equivalent pretest-posttest control group design was used. Four classes(8th grade), two classes for each sex, were selected. On the topic of 'Moon and Macs', two tape-recorded lessons differing in the kinetic structure were developed. Each lessons played 14 minutes long. One of them was high structure(B￣₁ = 0.48) and the other was low structure(B￣₁ = 0.19). The results showed that the students with high structure lesson achieved greater than those with low structure lesson(F = 7.03, p $lt; .01). But when the results were analyzed by sex, only boy students' achievement showed a significant difference between low and high structure groups(F = 9.54, p $lt;.01). The results of this study suggest that a high structure communication will facilitate the science learning in the case of boy students. On the other hand, an actual classroom communication on the topic of `Moon and planets' was tape-recorded from a middle school science class(9th grade) and lasted 45 minutes long. It was analyzed by Anderson's and Kim's methods of the kinetic structure analysis. The grand mean fundamental coefficient of the whole communication was 0.20, and the grand mean weighted coefficient was 0.84. This communication showed high mean progression density(D￣s= 0.88 with (NAC)￣=1.14). Thus, in general, this verbal communication had low structure and high progression. Therefore, it can be concluded that this classroom communication will give the students some difficulties in their learning.

The interaction of an isotropic stellar wind with a stratified environment leads to collimate the stellar wind outflow, forming a narrow jet especially in non-adiabatic cases. A jet opening angle, i.e, a jet collimation increases with a jet cooling, in which a free-free radio continuum is dominantly contributed. After a qualitative comparison of the theoretically derived jet boundaries with the optically observed ones have been carried out in order to know the physical parameters of the observed ones as well as to study the jet dynamical interaction with the surrounding medium. Instead of the morphological jet boundary fitting, the free-free radio continuum shapes have been suggested and recalculated.

One of fundamental bases for the desirable Science Education is effective evaluation, and the objectives of the Science Education can be used for the reasonable basis of this evaluation. In this paper, to study the current state of the high school Earth Science Education, comparison was made between the objectives of Education proposed by textbook and those to be measured by Scholastic Achievement test, and the result was analyzed. 1. The objectives of both the textbook and Scolastic Achievement test are highly oriented to obtain theory and comprehension. 2. The objectives which measure the Process of Scientific Inquiry are to some extent satisfied by the textbook but not by the Scholastic Achievement test. Consequently the future evaluation process should be modified in order to evaluate properly the ability for the process of Scientific Inquiry of the students properly.

A jet plasmoid model for 3C.449 has been constructed by introducing a plasma.ejecting black hole orbiting around the center of its parent cD galaxy. We examined the characteristics of the jet trajectory by varying the values of (1) orbiting radius and velocity of the black hole, (2) plasma ejection velocity, (3) size, mass and space velocity of the parent galaxy, (4) size of the galactic core and (5) the density of the intergalactic medium. In our model calculation the effect of the gravity by the parent galaxy and the ram pressure by the intergalactic medium have been taken in account. It is found that our dynamical model accounts reasonably well for the observed structure of 3C449. Our proposed model suggests that the buoyancy force near the galactic center plays an important role in the formation of the curved structure of the radio jet.

The proposed evaporation disk model is improved to figure out two flow system ~n the observed bipolar molecular outflow and stellar optical jet. Using the improved model, we can interpret the dymanical interactions of the two flows as well as obtain the physical parameter distributions along the flows Numerical & analytical adiabatic hydrodynamic calculations of the stellar jet inside show that the jet Mach number increases with an inversely proportional to the jet radius and M₁∼35, V₁∼150㎞/sec, Z₁∼0.1 pc, R₁∼0.05pc, T₁∼10³K, ρ₁-4.3×10^(-3)g/㎤(n₁∼25/㎤) at the end of the flow. By the way, in the case of the molecular flow. which is developed from the evaporated disk wind, the same calculations show that the flow Mach number increases with an inversely proportional to the mass flux distribution and M_d∼15, V₁∼15㎞/sec, Z_d∼1pc, R_d∼025pc, T_d∼10²K, ρ_d∼4.0×10^(-3)g/㎤(n_d∼25/㎤) at the flow end Most of the calculated physical parameters in the two flows consistent with the observational ones very well. The theoretically calculated flows develope the supersonic flows to make the shocked regions at the ends of flows. These regions are gravitationally unstable to produced the fragmentations whose masses are∼2 M- in the stellar let case and 0.3 M_⊙ in the bipolar flow case. This mass distribution supports that both the origins of Herbig-Haro objects and the birth of low mass stars are attributed to the instabilities of the shocked regions in the stellar jets and the bipolar molecular flows respectively.

A simple analytic model has been made to describe the radio appearance of nonspherical stro¨mgren region(e. q. comet-shaped H II region), assuming that(1) ionizing photons are conserved to a given solid angle within which they are emitted, and (2) a supersonic motion of a surrounding medium creates a shocked region in front of the non-spherical Sro¨mgren region. On the basis of this calculation, a model for the cometary H II region G34. 3+0.2 has been constructed to obtain dynamical parameter of the surrounding medium(V=100㎞/tsec at a_0=1㎞/sec)with a value of n_u=103㎝^(-3). The theoretical radio appearance of the model reproduces both the emission maximum at' the head part and the dominant shell structure as the radio observation of G34.3+0.2 has displayed.

We have considered the mass loss effects on the analytical PMS stellar evolutionary model of Stein(1966). In this calculation, we have assumed the mass loss law, M˙=K(L/C)(R/GM)'-,which should be reasonable for PMS stellar wind mechanism. The numerically obtained evolutionary tracks in H-R diagram indicate that the higher mass losses PMS star have, the later they reach the radiative equilibrium. We have considered the composition effect on the evolution such as the composition difference between Pop. I and Pop. II PMS stars. We have also compared the tracks under the mass loss law, M˙=K'LR/GM.

We study the luminosity and mass functions of open clusters using the data published by the United States Navel Observatory to figure out the relationships between these functions and the cluster ages. Slope ranges of the luminosity (dlogN/dMv) and mass function (-dlogN/d(log m/m@)) are 0.09-0.52(avg.=0.26, var.=0.01), 0.43-5.49(avg.=1.7, var.=0.63) respectively. These large ranges do not support the mass function is universal, but the function is time dependent. Despite of the poor relationship between the luminosity function and the cluster age, we obtain a good relationship in the mass function. We can understand this good relationship with a viewpoint of stellar evolution. We do age analyses in terms of the metal abundance and the number density of the open clusters. We get the fact that the less metal abundances and the less number densities, the more steep in the slopes of the mass function.

Three galaxies, NGC 0891(Sb),NGC 3359(SBc) and NGC 7640(SBc) have been taken to figure out the radio structural differences of spiral and barred spiral galaxies. Those galaxies have been observed in 21 cm neutral hydrogen emission line with 300 feet N.R.A.O, radio telescone(Rots, 1979). As Rots' observational line profiles have low angular resoulution, we could not distinguish the radix structural differences of those galaxies: Instead, the neutral hydrogen gases of each galaxy have been shown to tie widely distributed and the HI extents are much larger than the photographically shown ones. Furthermore, as peak column density regions coincide with the central regions of the galaxies, the large extensive radio structures may reveal the neutral gas distributions of the halo parts. The neutral hydrogen mass of each galaxy has been derived from the column density distributions. The line profiles of each galaxy help to obtain the velocity curves, from which the total kinematic mass can be calculated.

In order to explain the apparent alternation in VLA jet structures, we appeal to evaporation from an outer disk to switch the direction of the central energetic flow by a process of 'optical depth modulated' choking, That is as the radiation from a central engine heats the surface of an extended disk surrounding the engine, the disk surface will evaporate thermal gas, expanding the disk atmosphere and creating a disk wind. We argue that its dynamic pressure plays a very important role in confining the central energetic flow. If the disk has initially an asymmetric density distribution in the upper and lower atmospheres (i. e., asymmetric distribution of optical depth), then this can initiate the alternating jets(flip-flop jets), A flip-flop time scale is calculated from the rate of optical depth variation in the disk atmosphere(e.g., the optically thin atmosphere becomes optically thick due to the mass influx from the central engine), This gives a time scale of 3×10^7 yrs, which value, however, is strongly dependent on the size of the jet cavity where in the density(optical depth) is varied. We compare the theoretically derived flip-flop time scale to those estimated observationally for the standard straight, as well as the rotationally and mirror symmetric radio sources. The prediction is found to be reasonably consistent with the observationally derived time scales of the standard straight radio sources, however it is likely to be longer than those in the rotationally and mirror symmetric radio sources.

The learning subjects of primary and secondary levels of educational astronomy appears in cyclic developmental phases throughout education levels. To improve their learnings effectively, it is important to study the correlations of conceptional connection between previous and succeeding learnings, In this study, we select the astronomical unit subjects from the primary and secondary levels of science text books, analysing the conceptional connections between each unit subject and the unit subject of it's previous learning. We finally find that the conceptional connections of each unit are generally well made. Several units, however, have neither connections nor previous learnings which are reexamined, Therefore, we discuss the fitness of intellectual levels of students and the motives of interests to compensate the incomplete conceptional connections.

An evaporation disk model is proposed_to figure out shapes of molecular disks with density distributions of ρ_d∝r^(-n)(n$gt;1.8) using the energy and pressure equilibrium conditions as well as to explain the collimation mechanism of optical and radio jets with an openning angle of about 10 inside bipolar molecular outflows. Numerical hydrodynamic calculation of the jet inside shows that the jet velocity increases with a dependence on z^(1-5) and the Mach number of the jet converges to √3 . Mechanical energy of the jet heats the jet material, increasing the jet temperature with a distance. Calculated Ha flux in shock condition and radio continuum intensity at 5GHz are surely comparable to the observed ones. These results strongly support the evaporation disk model in collimating jet.