We show how the rotation emission from isolated interstellar Polycyclic Aromatic Hydrocarbons (PAHs) can explain the so-called anomalous microwave emission (AME). AME has been discovered in the last decade as microwave interstellar emission (10 to 70 GHz) that is in excess compared to the classical emission processes: thermal dust, free-free and synchrotron. The PAHs are the interstellar planar nano-carbons responsible for the near infrared emission bands in the 3 to 15 micron range. Theoretical studies show that under the physical conditions of the interstellar medium (radiation and density) the PAHs adopt supra-thermal rotation velocities, and consequently they are responsible for emission in the microwave range. The first results from the PLANCK mission unexpectedly showed that the AME is not only emitted by specific galactic interstellar clouds, but it is present throughout the galactic plane, and is particularly strong in the cold molecular gas. The comparison of theory and observations shows that the measured emission is fully consistent with rotation emission from interstellar PAHs. We draw the main lines of our PLANCK-AKARI collaborative program which intends to progress on this question by direct comparison of the near infrared (AKARI) and microwave (PLANCK) emissions of the galactic plane.

It has been a big mystery what drives filament eruptions and flares. We have studied in detail an X1.8 flare and its associated filament eruption that occurred in NOAA Active Region 9236 on November 24,2000. For this work we have analyzed high temporal (about 1 minute) and spatial (about 1 arcsec) resolution images taken by Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory, Hα centerline and blue wing (-0.6Å) images from Big Bear Solar Observatory, and 1600 Å UV images by the Transition Region and Corona Explorer (TRACE). We have found that there were several transient brightenings seen in Hα and, more noticeably in TRACE 1600 Å images around the preflare phase. A closer look at the UV brightenings in 1600 Å images reveals that they took place near one end of the erupting filament, and are a kind of jets supplying mass into the transient loops seen in 1600 Å. These brightenings were also associated with canceling magnetic features (CMFs) as seen in the MDI magnetograms. The flux variations of these CMFs suggest that the flux cancellation may have been driven by the emergence of the new flux. For this event, we have estimated the ejection speeds of the filament ranging from 10 to 160 km s-1 for the first twenty minutes. It is noted that the initiation of the filament eruption (as defined by the rise speed less than 20 km s-1) coincided with the preflare activity characterized by UV brightenings and CMFs. The speed of the associated LASCO CME can be well extrapolated from the observed filament speed and its direction is consistent with those of the disturbed UV loops associated with the preflare activity. Supposing the Hα/UV transient brightenings and the canceling magnetic features are due to magnetic reconnect ion in the low atmosphere, our results may be strong observational evidence supporting that the initiation of the filament eruption and the preflare phase of the associated flare may be physically related to low-atmosphere magnetic reconnection.

In this paper, we review recent studies on the magnetic helicity changes of solar active regions by photospheric horizontal motions. Recently, Chae(200l) developed a methodology to determine the magnetic helicity change rate via photospheric horizontal motions. We have applied this methodology to four cases: (1) NOAA AR 8100 which has a series of homologous X-ray flares, (2) three active regions which have four eruptive major X-ray flares, (3) NOAA AR 9236 which has three eruptive X-class flares, and (4) NOAA AR 8668 in which a large filament was under formation. As a result, we have found several interesting results. First, the rate of magnetic helicity injection strongly depends on an active region and its evolution. Its mean rate ranges from 4 to 17 × 10 40 Mx2 h-1. Especially when the homologous flares occurred and when the filament was formed, significant rates of magnetic helicity were continuously deposited in the corona via photospheric shear flows. Second, there is a strong positive correlation between the magnetic helicity accumulated during the flaring time interval of the homologous flares in AR 8100 and the GOES X-ray flux integrated over the flaring time. This indicates that the occurrence of a series of homologous flares is physically related to the accumulation of magnetic helicity in the corona by photospheric shearing motions. Third, impulsive helicity variations took place near the flaring times of some strong flares. These impulsive variations whose time scales are less than one hour are attributed to localized velocity kernels around the polarity inversion line. Fourth, considering the filament eruption associated with an X1.8 flare started about 10 minutes before the impulsive variation of the helicity change rate, we suggest that the impulsive helicity variation is not a cause of the eruptive solar flare but its result. Finally, we discuss the physical implications on these results and our future plans.

Recent observations have shown that coronal magnetic fields in the northern (southern) hemisphere tend to have negative (positive) magnetic helicity. There has been controversy as to whether this hemispheric pattern is of surface or sub-surface origin. A number of studies have focused on clarifying the effect of the surface differential rotation on the change of magnetic helicity in the corona. Meanwhile, recent observational studies reported the existence of transient shear flows in active regions that can feed magnetic helicity to the corona at a much higher rate than the differential rotation does. Here we propose that such transient shear flows may be driven by the torque produced by either the axial or radial expansion of the coronal segment of a twisted flux tube that is rooted deeply below the surface. We have derived a simple relation between the coronal expansion parameter and the amount of helicity transferred via shear flows. To demonstrate our proposition, we have inspected Yohkoh soft X-ray images of NOAA 8668 in which strong shear flows were observed. As a result, we found that the expansion of magnetic fields really took place in the corona while transient shear flows were observed in the photosphere, and the amount of magnetic helicity change due to the transient shear flows is quantitatively consistent with the observed expansion of coronal magnetic fields. The transient shear flows hence may be understood as an observable manifestation of the pumping of magnetic helicity out of the interior portions of the field lines driven by the expansion of coronal parts as was originally proposed by Parker (1974).

Lithium intercalated carbon (LIC) are basically employed as an anode for currently commercialized lithium secondary batteries. However, there are still strong interests in modifying carbon surface of active materials of the anode because the amount of irreversible capacity, charge-discharge capacity and high rate capability are largely determined by the surface conditions of the carbon. In this study, the carbonaceous materials were coated with tin oxide and copper by fluidized-bed chemical vapor deposition (CVD) method and their coating effects on electrochemical characteristics were investigated. The electrode which coated with tin oxides gave the higher capacity than that of raw material. Their capacity decreased with the progress of cycling possibly due to severe volume changes. However, the cyclability was improved by coating with copper on the surface of the tin oxides coated carbonaceous materials, which plays an important role as an inactive matrix buffering volume changes. An impedance on passivation film was decreased as tin oxides contents and it resulted in the higher capacity.

Soluble-NSF attachment protein receptor (SNARE) proteins play a role in vesicle fusion, exocytosis, and intracellular trafficking in neuronal cells as well as in fertilization and embryogenesis. We investigated the expression patterns of two SNARE proteins, SNAP-25 and synaptotagmin VII (SytVII), and their regulation by pregnant mare serum gonadotropin (PMSG) during mouse ovarian follicular development. Ovaries were obtained at 0, 12, 24, 36, and 48 h post-PMSG injection of immature mice. SNAP-25 and SytVII mRNA expression levels increased gradually in a time-dependant manner. However, protein levels revealed different patterns of expression, suggesting different translational regulation following PMSG stimulation. SNAP-25 and SytVII expression was closely associated with thickening of the granulosa cell (GC) layer and follicle morphological changes from a flattened to a cuboidal shape. To explore follicle stimulating hormone receptor (FSHR)-mediated regulation of their expression, GCs from preantral follicles were cultured to examine the effects of FSHR siRNA knockdown. FSHR siRNA abolished upregulation of the SNAREs in both PMSG and FSH-stimulated GCs. This abolished gene expression was rescued by adding dibutyryl cyclic AMP to the cultures. These results suggest that SNAP-25 and SytVII expression is regulated via the FSHR-cAMP pathway during follicular development.

본 시험은 종간교잡을 이용한 효과적인 보리 반수체 육성에 관한 체계적인 방법을 수립코자 실시하였다. 반수체 배 생산은 보리 품종 Bruce, Klages 와 Rodeo를 모본으로, H. bulbosum을 부본으로 하였다. 1. 총 1,687 화를 교배하여 1,079립의 종자를 수확하여 46% 교잡율을 얻었다. 2. 1,079립의 종자로부터 834개의 배를 생산하여 77%의 배 형성율을 얻었다. 3. 근 발육촉진을 위해서는 IAA가 NAA보다 효과적이었고, 4. 0ppm, 1ppm, 5ppm, 10ppm과 30 ppm의 IAA 농도중 1ppm이 가장 효과적이었다. 5. 콜치신에 의한 염색체 증가율은 82%이었다.