• 천문학회지
• /
• 제46권6호
• /
• pp.235-242
• /
• 2013

We compare mass-loss rates of OH/IR stars obtained from radio observations with those derived from the dust radiative transfer models and IR observations. We collect radio observational data of OH maser and CO line emission sources for a sample of 1533 OH/IR stars listed in Suh & Kwon (2011). For 1259 OH maser, 76 CO(J=1-0), and 55 CO(J=2-1) emission sources, we compile data of the expansion velocity and mass-loss rate. We use a dust radiative transfer model for the dust shell to calculate the mass-loss rate as well as the IR color indices. The observed mass-loss rates are in the range predicted by the theoretical dust shell models corresponding to $\dot{M}=10^{-8}M_{\odot}/yr-10^{-4}M_{\odot}/yr$. We find that the dust model using a simple mixture of amorphous silicate and amorphous $Al_2O_3$ (20% by mass) grains can explain the observations fairly well. The results indicate that the dust radiative transfer models for IR observations generally agree with the radio observations. For high mass-loss rate OH/IR stars, the mass-loss rates obtained from radio observations are underestimated compared to the mass-loss rates derived from the dust shell models. This could be because photon momentum transfer to the gas shell is not possible for the physical condition of high mass-loss rates. Alternative explanations could be the effects of different dust-to-gas ratios and/or a superwind.

• 천문학회보
• /
• 제35권1호
• /
• pp.52.1-52.1
• /
• 2010

The relationship between orbital periods of cataclysmic variables (CV) and mass-loss rates of their donor stars is an important subject of theoretical researches. The observed donor's radii are oversized in comparison with those of isolated unperturbed stars of the same mass, which is thought to be a consequence of the mass-loss. Using the empirical mass-radius relation of CVs and the Hayashi theory for changes in effective temperature, orbital period, and luminosity of the donor with the stellar radius, we find the mass-loss rate of CVs as a function of the orbital period P. The derived mass-loss rate is more or less constant at 10-9.6-10-10M$\odot$ yr-1 with P above 90 minutes and declines very rapidly with P below 90 minutes, reaching 10-10.3-10-11.7M$\odot$ yr-1 when P is close to the minimum period. The turnaround behavior of the mass-loss rate shape with P near the minimal period is much less pronounced than suggested by earlier numerical models, making observational detection of the turnaround highly unlikely. When applied to our new results, SDSS 1035, 1507, 1501 and 1433 systems, previously known as post-bounce CVs, are more likely to be systems that have yet to reach the minimal period.

• 대한물리의학회지
• /
• 제18권4호
• /
• pp.37-45
• /
• 2023

PURPOSE: The coexistence of age-related skeletal muscle mass loss and obesity poses a substantial health risk for individuals because it combines the detrimental effects of muscle mass reduction associated with aging and the health complications from obesity. This study aimed to identify the incidence rate and key influencing elements among Korean men in their thirties. METHODS: A cross-sectional study involving 934 male participants was performed using complex sampling analysis. Various influencing elements were investigated, including age, height, weight, body mass index, waist circumference, skeletal muscle mass index, smoking and drinking behaviors, systolic and diastolic blood pressure, fasting glucose levels, triglyceride, and cholesterol levels. RESULTS: The incidence rate was 2.90%. The key influencing elements were age, height, weight, body mass index, waist circumference, skeletal muscle index, systolic blood pressure, fasting glucose, triglyceride, and total cholesterol (p < .05). CONCLUSION: This study identified the incidence rate and key influencing element for CALSMO among Korean younger community-dwelling men.

• 한국안전학회지
• /
• 제23권6호
• /
• pp.84-90
• /
• 2008

The mass loss rate and heat release rate of puzzle mats were analysed using variable external irradiation level. Five samples of puzzle mat were tested in this study : Type A, B, C, D and E. Type A, B and C are all general grades whereas Type D and E are both Flame retardant grades. Incident heat fluxs of $25kW/m^2$, $35kW/m^2$, $50kW/m^2$ and $70kW/m^2$ were selected for these experiments. All samples were tested in the horizontal orientation and were wrapped in a single layer of aluminum foil. Each sample was nominally 20mm thick and 100mm square. The combustion heat and mass loss rate were carried out from Oxygen bomb calorimeter and mass loss calorimeter according to ISO 5660-1 respectively. Heat release rates were calculated using the equation ${\dot{Q}}=A_f{\dot{m}}"_X{\Delta}H_c=0.75A_f{\dot{m}}"{\Delta}H_c$. where $A_f$ is the horizontal burning area of the sample, $\dot{m}"$ is mass loss rate per unit area, ${\Delta}H_c$ is complete heat of combustion and 0.75 is combustion efficiency.

• 천문학회보
• /
• 제35권2호
• /
• pp.76.2-76.2
• /
• 2010

We present the final results of our study on the mass-loss rate of donor stars in cataclysmic variables (CVs). Observed donors are oversized in comparison with those of isolated single stars of the same mass, which is thought to be a consequence of the mass loss. Using the empirical mass-radius relation of CVs and the homologous approximation for changes in effective temperature T2, orbital period P, and luminosity of the donor with the stellar radius, we find the semi-empirical mass-loss rate M2dot of CVs as a function of P. The derived M2dot is at ~10-9.5-10-10 $M\odot$/yr and depends weakly on P when P > 90 min, while it declines very rapidly towards the minimum period when P < 90 min. The semi-empirical M2dot is significantly different from, and has a less-pronounced turnaround behavior with P than suggested by previous numerical models. The semi-empirical P-M2dot relation is consistent with the angular momentum loss due to gravitational wave emission, and strongly suggests that CV secondaries with 0.075 $M\odot$ < M2 < 0.2 $M\odot$ are less than 2 Gyrs old. When applied to selected eclipsing CVs, our semi-empirical mass-loss rates are in good agreement with the accretion rates derived from the effective temperatures T1 of white dwarfs. Based on the semi-empirical M2dot, SDSS 1501 and 1433 systems that were previously identified as post-bounce CVs have yet to reach the minimal period.

• 천문학회보
• /
• 제45권1호
• /
• pp.42.3-42.3
• /
• 2020

We investigate the observational properties of Wolf-Rayet stars, suggest the constraint of their mass-loss rate and apply our results to the observed progenitor candidates of Type Ib/Ic supernovae (iPTF13bvn and SN 2017ein). For this purpose, we adopt the WR star models with various mass-loss rates and wind terminal velocities. We obtain the high resolution spectra of those models at the pre-supernova phase using the radiative transfer code CMFGEN. We verify the optically faint property of SN Ic progenitors and show that the optical faintness is mainly originated by the high effective temperature at the photosphere. We also show that a simple analytic model for WR winds using a constant opacity can roughly predict the photospheric parameters. We show that the change of the mass-loss rate and the terminal wind velocity critically affects the optical luminosity. We find the optical luminosities of SN Ic progenitor models with our fiducial mass-loss rate prescription are fainter than the detection limits. We also suggest the mass-loss rate of WR stars may not exceed 2 times of our fiducial value by comparing our predictions with the detection limit of SN Ib/Ic progenitors. The directly observed progenitor candidate of iPTF13bvn can be explained by our SN Ib progenitor models. We find that the SN 2017ein progenitor candidate is too bright and too blue to be a SN Ic progenitor.

• 한국화재소방학회논문지
• /
• 제25권2호
• /
• pp.126-131
• /
• 2011

화점높이 변화에 따른 회오리 화염의 질량감소속도와 공기유입속도를 알아보기 위하여 회오리 화염 연구에서 많이 사용되고 있는 인화성 액체인 메탄올과 노말 헵탄을 사용하였다. 용기의 재질은 스테인레스로 100mm ${\times}$ 100mm ${\times}$ 50mm 크기의 사각형으로 제작하여 연소실험에 사용하였다. 외부로부터 화염으로 의 공기유입속도는 화점의 높이를 0cm에서 30cm로 변화시켰을 때, 0cm의 높이에서 가장 빠른 공기유입속도를 나타냈으며, 동일한 화점의 높이에서는 다점풍속기의 높이가 30cm인 경우에 가장 빠른 평균 공기유입속도와 최대 공기유입속도를 나타내었다. 또한 메탄올과 노말 헵탄의 회오리 화염의 결과로부터 질량감소속도는 노말 헵탄이 메탄올에 비해 1.33~1.58배, 외부로부터 화염으로의 공기유입속도는 노말 헵탄이 메탄올에 비해 4.38~5.44배 각각 빠름을 알 수 있었다. 결론적으로, 회오리 화염에서 질량감소속도와 외부에서 화염으로의 공기유입속도는 화점의 높이가 증가할수록 감소하며, 같은 실험조건에서 시료의 고위/저위 발열량이 높을수록 증가한다는 것을 확인할 수 있었다.

• 한국화재소방학회논문지
• /
• 제22권5호
• /
• pp.72-78
• /
• 2008

본 연구에서는 EPS 샌드위치 패널 심재에 대한 일정한 외부 복사열에 의한 질량감소속도와 열방출특성을 분석하였다. 일정한 외부 복사열원에 노출된 EPS 샌드위치 패널 심재의 질량감소속도와 열방출특성을 분석하기 위해 3가지 Type의 시료를 사용하였으며, 연소열을 측정하기 위해 Oxygen bomb calorimeter를 질량감소속도와 열방출특성을 분석하기 위해 Mass loss calorimeter를 사용하였다. 질량감소속도와 열방출 특성을 분석하기 위해 $100mm{\times}100mm{\times}50mm$ 크기의 시료를 사용하였다. 연구결과 50 kW/$m^2$의 외부복사열원에서 평균질량감소속도는 Type A와 B의 경우 각각 2.7 g/$m^2s$, 2.8 g/$m^2s$로 비슷한 경향을 나타낸 반면, Type C는 2.3 g/$m^2s$로 상대적으로 낮게 나타났으며, 평균열방출속도는 Type B와 C의 경우 각각 47.19 kW/$m^2$, 50.06 kW/$m^2$으로 큰 차이가 없었으나, Type A는 58.23 kW/$m^2$으로 상대적으로 높게 나타났다. 열방출특성의 결과를 캐나다 분류체계에 적용할 경우 Type A와 C의 경우 C-3등급, Type B의 경우 C-2등급으로 분류되었다. 향후 콘칼로리미터법을 이용한 샌드위치 패널 심재에 대한 열방출율 특성과의 비교연구가 필요할 것으로 판단된다.

• Journal of Astronomy and Space Sciences
• /
• 제8권1호
• /
• pp.11-23
• /
• 1991

The dynamical evolution of globular clusters is studied using the orbit-averaged multicomponent Fokker-Planck equation. The original code developed by Cohn(1980) is modi-fied to include the effect of stellar evolutions. Plommer's model is chosen as the initial density distribution with the initial mass function index $\alpha$=0.25, 0.65, 1.35, 2.35, and 3.35. The mass loss rate adopted in this work follows that of Fusi-Pecci and Renzini(1976). The stellar mass loss acts as the energy source, and thus affects the dynamical evolution of globular clusters by slowing down the evolution rate and extending the core collapse time Tcc. And the dynamical length scale $$R_c, $$R_h is also extended. This represents the expansion of cluster due to the stellar mass loss.

• 천문학회보
• /
• 제43권2호
• /
• pp.38.2-38.2
• /
• 2018

To understand the assembly of the galaxy population in clusters today, it is important to first understand preprocessing, the impact of environments prior to cluster infall. We use 15 cluster samples from YZiCS, a hydrodynamic cluster zoom-in simulation to determine the significance of preprocessing, and focus on the tidal mass loss of dark matter halos. We find ~48% of the cluster member halos were once satellites of another host. The preprocessed fraction depends on each cluster's recent mass growth history. Also, we find that the total mass loss is a clear function of the time spent in a host. However, two factors can increase the mass loss rate considerably. First, if the satellite mass is approaching the mass of its host. Second, when the halo suffers tidal mass loss at a higher redshift. Being in hosts before cluster infall enables halos to experience tidal mass loss for an extended period of time.