We explored the effect of galaxy-galaxy interaction on the FIR-radio correlation of star-forming galaxies by comparing the qFIR parameter distribution between interacting and non-interacting galaxies. Our sample galaxies were selected from the SDSS Stripe 82 region, where relatively deep optical images are available in addition to ancillary FIR and radio data. The qFIR values were 2.73±0.49 and 2.53±0.90 for interacting and non-interacting galaxies, respectively. The t-test results indicated that the difference in qFIR values between the two categories is not statistically significant. Our findings align with those of previous studies suggesting that either FIR excess or radio excess occurs only transiently during brief timescales in the merger stages, rather than persisting throughout the majority of merger events identified by features such as tidal tails or double nuclei.

Hydrogen cyanide (HCN) and hydrogen isocyanide (HNC) are isomers with similar chemical properties. However, HNC can be converted into other molecules by reactions with atomic hydrogen (H) and atomic oxygen (O), resulting in a variation of the HCN/HNC abundance ratio. These reaction rates are sensitive to gas temperature, resulting in different abundance ratios in different temperature environments. The emission of HCN and HNC was found to distribute along ring structures in the protoplanetary disk of V883 Ori. HCN exhibits a multi-ring structure consisting of inner and outer rings. The outer ring represents a genuine chemical structure, whereas the inner ring appears to display such characteristics due to the high dust continuum optical depth at the center. However, HNC is entirely depleted in the warmer inner ring, while its line intensity is similar to that of HCN in the colder outer ring. In this study, we present a chemical calculation that reproduces the observed HCN/HNC abundance ratio in the inner and outer rings. This calculation suggests that the distinct emission distribution between HCN and HNC results from a currently ongoing outburst in V883 Ori. The sublimation of HCN and HNC from grain surfaces and the conversion of HNC to HCN determine their chemical distribution in the heated, warm inner disk.

In this paper, we investigate asteroseismic scaling-relations of evolved stars in star clusters observed by Kepler/K2, aiming to address the issue of whether observed stellar oscillations are influenced by environmental factors, as there are interesting phenomena relating to the stellar pulsations observed in star clusters. Specifically, we compare statistical properties of distributions including Δν, νmax, HGauss, δνenv, and δν02 derived from red giant branch (RGB) and red clump (RC) stars in two pairs of star clusters: NGC 2682 - NGC 6819 and NGC 1817 - NGC 6811. We have found that the slopes of relations between νmax and Δν and between HGauss and νmax associated with RC stars in the more compact star clusters, NGC 2682 and NGC 1817, are in common less steep compared with those for NGC 6819 and NGC 6811. It is also found that the slopes of the relation between δνenv and νmax from RC stars in the more compact star clusters are in common steeper compared with those for the others. For the relation between δν02 and Δν obtained from RGB stars, the slope resulting from NGC 2682 and NGC 6819 is indistinguishable. The Kolmogorov–Smirnov tests conducted on RC stars in the pairs of NGC 2682 and NGC 6819, as well as NGC 1817 and NGC 6811, indicate that all the seismic quantities considered in this paper are drawn from different distributions. We conclude, therefore, that the properties of star clusters should be considered when asteroseismic data obtained from stars within star clusters are interpreted.

Carbon fusion is important to understand the late stages in the evolution of a massive star. Astronomically interesting energy ranges for the 12C+12C reactions have been, however, poorly constrained by experiments. Theoretical studies on stellar evolution have relied on reaction rates that are extrapolated from those measured in higher energies. In this work, we update the carbon fusion reaction rates by fitting the astrophysical S-factor data obtained from direct measurements based on the Fowler, Caughlan, & Zimmerman (1975) formula. We examine the evolution of a 20M⊙ star with the updated 12C+12C reaction rates performing simulations with the MESA (Modules for Experiments for Stellar Astrophysics) code. Between 0.5 and 1 GK, the updated reaction rates are 0.35 to 0.5 times less than the rates suggested by Caughlan & Fowler (1988). The updated rates result in the increase of core temperature by about 7% and of the neutrino cooling by about a factor of three. Moreover, the carbon-burning lifetime is reduced by a factor of 2.7. The updated carbon fusion reaction rates lead to some changes in the details of the stellar evolution model, their impact seems relatively minor compared to other uncertain physical factors like convection, overshooting, rotation, and mass-loss history. The astrophysical S-factor measurements in lower energies have large errors below the Coulomb barrier. More precise measurements in lower energies for the carbon burning would be useful to improve our study and to understand the evolution of a massive star.

본 연구는 국내 스포츠 은퇴 선수들의 광고 스타파워 효과성을 검증하여 기업 및 광고 에이전 시의 효율적인 광고 모델 전략을 위한 기초자료를 제공하고자 했다. 따라서 국내 스포츠 은퇴 선수들이 광 고 모델로 선정된 광고를 인지하고 있는 사람들을 표본으로 선정했으며, 206부의 자료를 최종분석에 적용 했다. 자료처리는 SPSS(ver. 21.0) 프로그램으로 빈도 및 신뢰도 분석을 실시했다. 또한 AMOS(ver. 20.0) 프로그램으로 확인적 요인분석, 상관분석, 구조방정식 모형분석, 효과성의 유의성을 검증했다. 연구결과 첫 째, 국내 스포츠 은퇴 선수들의 스타파워는 호감도에 긍정적인 영향이 있는 것으로 나타났다. 둘째, 호감도 는 광고 소비행동에 긍정적인 영향이 있는 것으로 나타났다. 셋째, 스타파워는 광고 소비행동에 긍정적인 영향이 있는 것으로 나타났다. 마지막으로 스타파워는 광고 소비행동에 직접효과가 더 큰 것으로 나타났으 며, 호감도는 부분매개효과가 있는 것으로 검증됐다.

프리지아 ‘Ruby Star’는 농촌진흥청 국립원예특작과학원 에서 보라색 홑꽃 ‘Avilla’와 흰색 반겹꽃 ‘Medeo’를 2012년 교배하여 얻은 종자로부터 2006년 향이 좋고 개화기가 빠른 적색 홑꽃 계통을 선발하여 품종으로 개발되었다. 2014년부 터 2017년까지 생육·개화 특성검정 및 육성계통평가회의 기 호도 평가를 거쳐 선발되었으며 2018년 직무육성품종심의회 를 통해 ‘Ruby Star’로 명명되어 2021년 신품종으로 등록되 었다. ‘Ruby Star’는 빨간색(RHS, R45A) 홑꽃인 절화용 프리 지아 품종으로 개화소요일수가 118.0일이며 초장이 120.5cm 로 대조품종 ‘Rapid Red’보다 약 28.7cm 더 길다. 주당 분 지수는 5.8개로 대조품종에 비해 수확량이 많고 첫번째 분지 의 길이가 32.0cm, 두께가 3.02mm로 절화 특성이 우수하 다. ‘Ruby Star’의 소화수 및 소화폭은 각각 14.8개, 6.3cm 로 소화수가 많은 중대형화이다. 절화수명은 약 8.4일이며 주 당 자구수는 3.8개, 평균 자구중은 2.9g이다. 전자코를 이용 한 PCA 분석 결과 PC1과 PC2의 설명력은 각각 97.9%, 1.8%로 전체 변이의 99.7%를 반영했으며 ‘Ruby Star’와 대 조품종 ‘Rapid Red’는 서로 다른 향기 패턴을 보였다. Radar plot 결과 총 6개의 MOS 센서에서 ‘Ruby Star’의 센서 반응 이 ‘Rapid Red’보다 강하게 나타나 ‘Ruby Star’의 향기가 더 강한 것으로 나타났다.