New M-Type Variables in Galactic Dark Clouds     

N. D. Melikian  C. Magnan  J. M. Sarkissian  A. A. Karapetian 《Astrophysics》2003,46(1):10-17

The results of the spectral classification of newly discovered M-type variables obtained as part of an H-alpha survey of Galactic dark cloud regions are presented. The survey was carried out with the 40 Schmidt camera of Byurakan Observatory, and the spectra of the variable stars for the classification were obtained with the Observatory's 2.6-m telescope. The observational material allowed register of late M-type variables as well as their brightness variations. Among the 97 newly discovered M-type stars, 22 show brightness variations. The results of the spectral classification of these new variables show that 21 out of 22 are red giants, and in all probability they are Mira Ceti type long period variables.  相似文献   

The Velocity Field and Kinematics of the Galaxy NGC 784 in the Hα Line     

R. A. Kandalyan  A. M. Khassawneh  A. T. Kalloghlian 《Astrophysics》2003,46(1):74-79

In this paper we present the H map, the 2D velocity field and the rotation curve of the galaxy NGC 784 obtained with the ByuFOSC2 scanning Fabry-Perot interferometer, attached at the prime focus of the 2.6-m telescope of Byurakan Observatory. The H image shows several HII condensations along the major axis of the galaxy. The galaxy has an asymmetric distribution of the H emission. The rotation curve is quite symmetric with a low gradient in the central part of the galaxy.  相似文献   

康普顿化的计算-推广的Kompaneets方程与Monte Carlo方法比较     

刘当波  凌家杰  陈磊  尤峻汉  HUA Xin-Min 《天文学报》2003,44(3):286-301

在X射线天文学以及辐射物理学中,当硬X射线穿过" 冷"的等离子体时所发生的Compton软化是一种重要的辐射转移过程.简要介绍推广的Kompaneets方程,该方程在hv〈mec2及kTe〈mec2较宽松的条件下广泛成立,因此不仅能处理Compton硬化过程,而且也适用于Compton软化过程,后者在目前快速发展的X射线和γ射线天文学中十分重要.基于此方程,我们对天体物理中4种常见辐射谱(Gauss型发射谱线、黑体辐射谱、幂律辐射谱和热轫致辐射谱)在Compton软化情况下的谱演化进行了数值求解,并同Monte Carlo模拟结果做比较,证实了推广的Kompaneets方程的正确性和有效性.最后指出此方程在X射线天文学和γ射线天文学中的重要意义和潜在应用.  相似文献   

太阳系早期的短寿期放射性核素   总被引：2，自引：0，他引：2  

徐伟彪 《天文学报》2003,44(3):231-239

较详细地介绍全新的太阳系起源理论——X-wind模式,天体化学实验发现太阳系早期存在大量的短寿期放射性核素(半衰期小于100Ma),这些核素对太阳系的形成和演化有重要的影响,一种理论认为,这些核素是在恒星内部合成,并由星风注入原太阳分子云,星风产生的激波诱发分子云核的塌缩而形成原太阳,另一种理论认为,这些核素是高能粒子与原太阳分子云或太阳星云中的气体和尘埃相互作用的产物。  相似文献   

Scale invariant theory for Bianchi Type VIII and IX space-times with perfect fluid     

G. Mohanty  B. Mishra 《Astrophysics and Space Science》2003,283(1):67-74

In this paper we have taken an attempt to study the feasibility of scale invariant theory (Wesson, 1981a,b) in Bianchi type VIII and IX space-times with a time dependent gauge function (Dirac Gauge i.e. βα )and a matter field in the form of a perfect fluid. It is found that Bianchi type VIII (δ=1) space-time is feasible in this theory whereas Bianchi type IX (δ=-1) space-time is not feasible. In this feasible case a radiating model is constructed and its physical behaviour is discussed. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Giant Vibrations in Dip     

T.C. Teixeira  J. Christensen-Dalsgaard  F. Carrier  C. Aerts  S. Frandsen  D. Stello  T. Maas  M. Burnet  H. Bruntt  J.R. de Medeiros  F. Bouchy  H. Kjeldsen  F. Pijpers 《Astrophysics and Space Science》2003,284(1):233-236

This work reports the discovery of solar-type oscillations in thegiant star Hydrae.  相似文献   

1.2米地平式望远镜指向模型的研究 (1.全天指向模型的建立)   总被引：4，自引：1，他引：3  

郑向明  王武  张云成  冯和生 《天文学报》2003,44(3):330-336

介绍了云南天文台1.2米地平式望远镜用于天文观测和图像采集处理的方法,建立了新的、独特的全天指向模型,大大提高了该望远镜的指向精度,达到1″,并在多年的实际应用中得到验证。  相似文献   

Mode Identification from Line Profiles using the Direct Fitting Technique     

Luis A. Balona 《Astrophysics and Space Science》2003,284(1):121-124

The method of moments and the direct fitting method are the onlyspectroscopic methods of mode identification which allow a determination ofall pulsational parameters. The pulsation parameters are required to predictthe light amplitude and phase which can be important discriminants in modeidentification. The direct fitting method has several advantages over themethod of moments. It is not restricted to low spherical harmonic degree or form of the eigenfunction and is not sensitive to the placement of the continuum. In the last few years the method has been applied to several different types of stars. We briefly describe the method and give someexamples of its application.  相似文献   

低质量X射线双星的毫秒级准周期信号——最近的进展     

YU Wen-fei 《天文研究与技术》2003,(1):12-15

最近对低质量X射线双星中的千赫兹准周期振动的研究表明 ,是辐射压力 ,而不是盘和磁球的相互作用以及处于盘内边界的广义相对论效应在短时标的盘切断机制上起作用。本文给出了一些研究结果及讨论。  相似文献   

Stochasticity of planetary orbits in double star systems. II     

Benest  D.  Gonczi  R.  Gonczi  R. 《Earth, Moon, and Planets》2003,93(3):175-190

Cosmogonical theories as well as recent observations allow us to expect the existence of numerous exo-planets, including in binaries. Then arises the dynamical problem of stability for planetary orbits in double star systems. Modern computations have shown that many such stable orbits do exist, among which we consider orbits around one component of the binary (called S-type orbits). Within the framework of the elliptic plane restricted three-body problem, the phase space of initial conditions for fictitious S-type planetary orbits is systematically explored, and limits for stability had been previously established for four nearby binaries which components are nearly of solar type. Among stable orbits, found up to distance of their sun of the order of half the binarys periastron distance, nearly-circular ones exist for the three binaries (among the four) having a not too high orbital eccentricity. In the first part of the present paper, we compare these previous results with orbits around a 16 Cyg B-like binarys component with varied eccentricities, and we confirm the existence of stable nearly-circular S-type planetary orbits but for very high binarys eccentricity. It is well-known that chaos may destroy this stability after a very long time (several millions years or more). In a first paper, we had shown that a stable planetary orbit, although chaotic, could keep its stability for more than a billion years (confined chaos). Then, in the second part of the present paper, we investigate the chaotic behaviour of two sets of planetary orbits among the stable ones found around 16 Cyg B-like components in the first part, one set of strongly stable orbits and the other near the limit of stability. Our results show that the stability of the first set is not destroyed when the binarys eccentricity increases even to very high values (0.95), but that the stability of the second set is destroyed as soon as the eccentricity reaches the value 0.8.  相似文献