For each group stars, both the surface gravity and the stellar mass increase with increasing effective temperature.
对每一类恒星，其质量和表面重力都随着有效温度的增高而线性增大。
For example, the stellar mass-to-light ratio could be anomalously large; equilibrium demands more velocity for more mass.
例如，恒星的质光比可能呈现异常得大；为了平衡越大的质量就需要越大的速度。
Stellar mass is an indispensable parameter in the studies of stellar physics and stellar dynamics.
恒星质量是恒星物理以及恒星系统动力学研究中一个不可或缺的参量。
Brown dwarf star is a class of stellar objects as a mass of about 5-90 Jupiter.
棕矮星是类恒星天体的一种，质量约为5至90个木星之间。
In the present paper the mass of RR Lyrae is determined on the basis of Zhevakin's theory of stellar variability.
从这个数值计算出的振动非绝热度同日瓦金理论中对造父变星的条件相符合。
The average range of nonthermal radiation particles is direct proportion to the energy extent of nonthermal radiation particle, but also inverse proportion to the density of stellar gas, however, to the stationary black hole with mass multipole moment and nonstationary black hole, the average range of their nonthermal radiation particle still has something to do with direction, which are the new results reported firstly.
非热辐射粒子的平均射程与非热辐射粒子的能量范围成正比、与星际气体的密度成反比；对动态黑洞和一类具有质量多极矩的稳态黑洞而言，非热辐射粒子的平均射程还与方向有关。这些都是首次报道的新结果。
In fact, the process otherwise appears to be just like the accretion process feeding M81's stellar mass black holes, even though the central black hole is millions of times more massive.
事实上，这个过程看上去就像给M81内恒星量级的黑洞吸积过程，尽管中央黑洞质量要大上数百万倍。
Using degenerate Fermi statistics theory and considering the relativistic effect of electronic move - ment, this paper derives limited mass of White Dwarf Stars-Chandrasekhar limit, and then discusses the importance of Chandrasekhar limit in the stellar evolution process.
利用简并费米统计理论，并考虑到电子运动的相对论效应，求出白矮星的极限质量&Chan-drasekhar极限质量，并进一步讨论了这一极限质量在恒星演化过程中的意义。
By studying the variety of inner structure of stars, an attitude that different demarcation point of stellar evolutional stages can affects the evolutionary track in the Hertzsprung-Russell diagram is developed, based on mass loss rate is a consecutive piecewise function in the stellar evolution calculations.
通过分析恒星内部结构的变化，基于在演化计算中质量损失率公式应采取连续的分段函数的考虑，提出恒星演化阶段的分界点的不同会影响恒星在赫罗图中演化轨迹的观点。
The binary-technique is the line profile analysis method which is the most accurate one being applied in a ζ Aur/VV Cep binary system to detect the mass-loss-rates of the stellar wind of the red-giant or of the red-super-giants.
用双星技术（Binary－technique）的谱线分析方法来测定双星系统中的红巨星或红超巨星的星风物质损失率是目前最为精确的。
Also the reasonable model parameters, such as the metal yield and the stellar initial mass function, make it possible to re-produce the observed bimodal distribution of the color-magnitude diagram.
我们选取的合理的参数，如金属产率，恒星初始质量函数等使得我们能预言星系颜色分布的双峰结构。
For each type of galaxy, the size distribution at given luminosity (or stellar mass) is well described by a log-normal function, characterized by its median R and dispersion InR.
对于给定形态的星系，在给定光度（或恒星质量）处其大小的分布较好的遵从一对数正态函数，因此可由其中值R和弥散σ（lnR）两个参数加以定量描述。
Observational evidence for stellar winds obtained from radio, infrared, visible, UV and X-ray regions are given. And two important parameters, terminal velocity and mass loss rate, are discussed.
在观测方面，给出了从射电、红外，可见光、紫外和X射线各波段得到的观测证据，并介绍了星风的两个重要参数、星风的终速和质量损失率。
In the first chapter of this paper we introduce the concept and the category of the gravitational effect before presentation of the mass-defect effect. Then we simply introduce the basic knowledge in stellar and accreting theory relating to the mass-defect effect.
本文第一章中，首先介绍引力效应的概念及所属范畴，然后引出质量亏损效应，并介绍了与这一效应相关的恒星物理学及吸积理论的基本知识。
Stellar-mass black holes are thought to form when giant, dying stars collapse, leaving corpses that are so dense not even light can escape their gravitational pull.
现有的理论认为：当一颗巨大的星体衰老时，它的残骸形成密度极大的星体，甚至连光也无法逃脱它的重力吸引，这就是恒星级黑洞的形成过程。
And this may be the mechanism for driving the strong stellar winds of RGB stars and AGB stars with very low surface temperature and faint radiation pressure. PRESSURE DROP OF VARIABLE MASS FLOW IN HORIZONTAL PERFORATED WELL BORE
我们认为湍流压效应可能就是造成有效温度低因而辐射压也低的RGB星产生强星风，以及AGB星产生超星风的物理原因。射孔完井水平井筒变质量湍流压降规律研究
If the magnetic stress bears up the gravitation in the stellar evolution, the big mass neutron star over the neutron - star mass can not collapse into a black hole.
如果在恒星演化过程有磁应力来支撑引力，超过中子星质量上限的大质量中子星则不致于坍缩成黑洞。
The correlation between metallicity and stellar mass of cluster galaxies is also confirmed. It is concluded that galaxy cluster Abell 2255 is formed by the gravitational interaction after the individual galaxies are formed, which supports the hierarchical model of cluster formation.
此外还确认了团星系的金属丰度与恒星质量之间的相关性，并推断星系团Abell2255是在单个星系形成后，经过引力相互作用而形成的，这一结果支持了等级成团理论。
Anisotropy Losses of Mass due to Steller Wind in the Rotating Stellar
自转恒星中各向异性的星风物质损失的研究
High-mass stars form in dense regions of gas, and later in life expel strong stellar winds that blow away the surrounding material.
大量的星星存在于稠密的气体中间，在接下来的日子中，强有力的恒星风将会将其周围的物体吹走。