星际分子及其谱线

介绍了星际分子及其谱线的研究历史和现状，分析了如何从分子谱线探索恒星形成区的物理化学性质，简述了探测星际分子谱线的大型射电望远镜。     

世纪之交的天体物理与原子分子物理

20世纪的后叶 ,原子与分子的射电谱线揭示了光学不可见的冷宇宙 ,银河系最大天体 -巨分子云和恒星形成过程的一个普遍存在的重要的相 -双极外流。近十年发射的红外天文卫星ISO,通过对原子与分子的红外谱线的观测 ,在研究动能温度数百度以上的富碳、富氧演化星包层 ,行星状星云、年轻星和恒星形成区复合体的物理与动力学性质方面取得重要的结果 ,并向原子与分子物理学家提出许多问题和要求。原子与分子物理与天体物理在急剧的发展中将互相激发 ,碰撞出更绚丽的火花。     

玫瑰眼（The Rosette Eye）——大质量恒星周围电离氢区前期形成及演化重要过渡阶段的发现

一个由中英德美多国天文学家组成的工作小组近期在距离太阳系5000光年的玫瑰巨分子云核心大质量星形成区域发现了一个处于早期演化阶段的罕见的年轻大质量恒星系统。据估算,中心星体的质量大约为20个太阳质量。观测表明,该大质量星在其形成的吸积塌缩过程中产生的强大紫外辐射正以大张角电离星风的形式从恒星的两极喷射而出,在近红外宽带和分子氢发射线窄带成像中表现为一个沙漏状的双极电离氢区。     

星际分子及其谱线

介绍了星际分子及其谱线的研究历史和现状,分析了如何从分子谱线探索恒星形成区的物理化学性质,简述了探测星际分子谱线的大型射电望远镜.     

星际H2O与OH分子脉泽的统计与激发机制探讨

报告了大质量恒星形成区的星际分子脉泽巡天观测结果.所观测到的H2O与OH分子脉泽可分为三类,它们的数量近似相等,寿命亦近似相等～105年,但HⅡ区普遍短缺.提出了一种新的辐射机制模型,它克服了旧辐射模型的缺点,可以解释星际H2O与OH脉泽的成因,以及作者的观测统计结果.     

来稿摘登

据观测,我们宇宙现在的空间尺度约为10~(26)米(几百亿光年),在这个宽广的空间中有着数以千百万亿计的天体。天体大致可以分成两大类,一类是呈致密状存在的星体,一类是呈弥漫状存在的尘埃、气云以及各种辐射。天体中有轮廓分明的恒星和行星;有分辨不出其大小,好象是“恒星”,光谱中具有红移很大的发射线的类星体;有的发射可见光,有的则是发射无线电波的射电源;有吸积经过其附近的一切物质而没有任何消息透露出来的黑洞,也有不间断地向外发射物质的白洞……,当然,宇宙中还充满着大量的中微子以及背景辐射,我们的宇宙正在不断地膨胀,我们周围     

CO电子基态P线系跃迁谱线的理论研究

基于微分的思想,结合经典的双原子分子跃迁谱线表达式,提出了预言双原子分子P线系高激发振-转跃迁谱线的新解析物理公式.对于某分子电子体系的某一P支跃迁带,利用实验上获得的一组(15条)精确的跃迁谱线和该跃迁带对应的上下振动态的转动常数(B_υ',B_υ″)的精确数据,该公式不仅可以精确地重复已知的实验跃迁谱线,而且还能预测出实验上难以获得的更高激发态的跃迁谱线数据.利用该公式,研究了CO分子电子基态的(2,0)振-转跃迁带的< 关键词： 双原子分子 发射光谱 P线系')" href="#">P线系 CO     

星际型CH3CN—H2含超精细能级的碰撞跃迁速率系数的理论计算

利用ＩＯＳ近似模型，计算了星际分子去条件下Ｅ型ＣＨ３ＣＮ－Ｈ２含超精细能级的碰撞跃迁速率系数。其温度范围是２０Ｋ－１４０Ｋ。为研究分子云与恒星形成区的物理、化学性质提供了大量有用的基础分子数据。     

黑洞体量竟有上限

正星系中心的超大质量黑洞是宇宙间最重的天体,银河系中心黑洞的质量堪比400万个太阳,天文学家还曾发现体重为数十亿个太阳的黑洞。可是这些大质量黑洞究竟能增大到什么程度呢?一位天体物理学家说,质量上限是太阳的500亿倍。黑洞通过围绕其旋转的气体和尘埃组成的吸积盘吸取物质,不断长大。吸积盘的摩擦导致物质向黑洞内部移动,直至被黑洞引力撕碎后吞噬。这一过程使气体温度极高,以致达到发光的程度,这     

光深对大质量恒星形成团块化学性质研究的影响（英文）

本文使用文献中的N_2H+(1-0)、H~(13)CO+(1-0)、HCN(1-0)和HN~(13)C(1-0)谱线数据研究大质量恒星形成团块的化学性质和演化,发现H~(13)CO~+和HN~(13)C的丰度受H_2柱密度的影响.由于从A阶段到B阶段这两个丰度的中值增加了近10倍,H~(13)CO~+和HN~(13)C适合追踪大质量恒星形成团块的演化.从A到B阶段四种分子丰度增长速度从高到低依次为H~(13)CO~+、HCN、HN~(13)C、N_2H~+.结果表明进行光学薄分子谱线的高分辨率观测对于研究大质量恒星形成团块的化学演化是必要的。     

大质量恒星的形成:理论与观测

文章简要叙述了有关大质量恒星形成的理论以及相关观测证据。目前大质量恒星形成的理论主要有两种，即吸积说和并合说．吸积说认为，大质量星可能与小质量星形成于相似的过程；并合说主张大质量星可能是由小质量年轻星碰撞合并而成．解决这两种理论争论的关键在于在大质量星附近能否观测到吸积盘的存在，最新的观测表明大质量星更有可能是通过吸积增加自身的质量，但最终解决这一问题可能还需要更多的观测证据。文章还提出了一些本领域尚未解决的问题，为感兴趣的研究者提供参考。     

Accreting neutron stars as probes of dense matter physics

There are over 100 accreting neutron stars in our galaxy, in which matter (typically H/He) is tidally transferred from a secondary companion to the neutron star. Accretion of this matter perturbs the thermal structure of the interior away from that of an isolated cooling neutron star. In this paper. we review how this accretion induces reactions in the crust of the neutron star that keep the interior hot. If the accretion is intermittent, then the heated surface layers are directly observable when accretion stops. This heating also affects the unstable ignition of light elements in the neutron star envelope. Observations of the neutron star cooling following an accretion outburst can in principle constrain the thermal properties of the crust and core.     

星际型CH_3CN－H_2含超精细能级的碰撞跃迁速率系数的理论计算

利用ＩＯＳ近似模型，计算了星际分子云条件下Ｅ型ＣＨ３ＣＮ－Ｈ２含超精细能级的的碰撞跃迁速率系数。其温度范围是２０Ｋ－１４０Ｋ。为研究分子云与恒星形成区的物理、化学性质提供了大量有用的基础分子数据。     

Quasar microlensing

Quasar microlensing deals with the effect of compact objects along the line of sight on the apparent brightness of the background quasars. Due to the relative motion between quasar, lenses and observer, the microlensing magnification changes with time which results in uncorrelated brightness variations in the various images of multiple quasar systems. The amplitudes of the signal can be more than a magnitude with time scales of weeks to months to years. The effect is due to the “granular” nature of the gravitational microlenses—stars or other compact objects in the stellar mass range. Quasar microlensing allows to study the quasar accretion disk with a resolution of tens of microarcseconds, hence quasar microlensing can be used to explore an astrophysical field that is hardly accessible by any other means. Quasar microlensing can also be used to study the lensing objects in a statistical sense, their nature (compact or smoothly distributed, normal stars or dark matter) as well as transverse velocities. Quasar microlensing light curves are now being obtained from monitoring programs across the electromagnetic spectrum from the radio through the infrared and optical range to the X-ray regime. Recently, spectroscopic microlensing was successfully applied, it provides quantitative comparisons with quasar/accretion disk models. There are now more than a handful of systems with several-year long light curves and significant microlensing signal, lending to detailed analysis. This review summarizes the current state of the art of quasar microlensing and shows that at this point in time, observational monitoring programs and complementary intense simulations provide a scenario where some of the early promises of quasar microlensing can be quantitatively applied. It has been shown, e.g., that smaller sources display more violent microlensing variability, first quantitative comparison with accretion disk models has been achieved, and quasar microlensing has been used to determine the fraction of dark matter in a lensing galaxy for the first time. This is the quantitative beginning. The future of quasar microlensing is bright.     

Neutrino crown of a protoneutron star in the process of collapse: Physical formulation of the problem

A spherically symmetric gravitational collapse of the iron core of a star develops in the form of a hydrodynamic process, where the role of intrinsic neutrino radiation ever increases. The early stage of the collapse has a homological character within the interior of the core, but there is a delay in exterior layers. Hydrodynamic calculations reveal that, at the late stage of the collapse (it is the stage within which the majority of neutrinos are emitted), a structure is formed that consists of a neutron-star germ nontransparent to neutrinos and exterior layers accreting onto it, which are, on the contrary, transparent to neutrinos. They are separated by a semitransparent layer occurring between the front of the accretion shock wave and the germ surface forming a neutrinosphere. By using a typical quasistationary character of this layer, which is referred to as the neutrino crown of a protoneutron star, a stationary model is developed here that supplements hydrodynamic calculations of the collapse process, which are rather rough within this model. In particular, these calculations reveal the crucial significance of the semitransparent crown for a possible transition of the collapse into an explosion having a scale of a supernova explosion. If there is no such possibility, the same crown determines the important properties of a quiet collapse that are associated with the development of convective instability, etc., in it. The model formulated here, which is comparatively simple (in relation to hydrodynamic calculations) owing to an adequate physical formulation of problem, is intended for analyzing special features of the crown. This formulation of the problem demonstrates some new possibilities of neutrino hydrodynamics, which is an analog of the well-known radiative hydrodynamics involving photons instead of neutrinos.     

Numerical solution of the radiation transport equation in disk geometry

We describe an efficient numerical method for solving the problem of radiation transport in a dusty medium with two dimensional (2-D) disk geometry. It is a generalization of the one-dimensional quasi-diffusion method in which the transport equation is cast in diffusion form and then solved as a boundary value problem. The method should be applicable to a variety of astronomical sources, the dynamics of which are angular-momentum dominated and hence not accurately treated by spherical geometry, e.g. protoplanetary nebulae, circumstellar disks, interstellar molecular clouds, accretion disks, and disk galaxies. The computational procedure and practical considerations for implementing the method are described in detail. To illustrate the effects of 2-D radiation transport, we compare some model results (dust temperature distributions and i.r. flux spectra) for externally heated, interstellar dust clouds with spherically symmetric and disk geometry.     

Current diversion in the accretion disk of a magnetized neutron star

Summary We revisited the magnetized accretion disk problem and studied the currents flowing in the magnetosphere. We noted the importance of the radial currents in the disk and examined how these radial currents can be diverted to flow along the magnetic-field lines. One fluid magneto-hydrodynamic analysis was applied to the model neutron star and the self-consistent current system was obtained. This work was supported by Korea Institute of Technology and Korea Science and Engineering Foundation.     

Slim Discs with Varying Accretion Rates

It was revealed in our previous studies that there exists a maximal possible accretion rate for slim discs with constant accretion rates because the correctly calculated vertical gravitational force can only gather some limited amount of accreted matter. Here we show that when the accretion rate is not constant and instead decreases with decreasing radius because of outflows, such that the amount of accreted matter is adjusted to be within the allowed limit, global slim disc solutions can be constructed even for the case that accretion rates at large radii apparently exceed the maximal possible value. This result further demonstrates that outflows seem to be unavoidable for accretion flows with large accretion rates at large radii.     

Effect of magnetic field on beta processes in a relativistic moderately degenerate plasma

The effect of a magnetic field of arbitrary strength on the beta decay and crossing symmetric processes is analyzed. A covariant calculation technique is used to derive the expression for the squares of S-matrix elements of these reactions, which is also valid in reference frames in which the medium moves as a single whole along magnetic field lines. Simple analytic expressions obtained for the neutrino and antineutrino emissivities for a moderately degenerate plasma fully characterize the emissivity and absorbability of the studied medium. It is shown that the approximation used here is valid for core collapse supernovae and accretion disks around black holes; beta processes in these objects are predominantly neutrino reactions. The analytic expressions obtained for the emissivities can serve as a good approximation for describing the interaction of electron neutrinos and antineutrinos with the medium of the objects in question and hold for an arbitrary magnetic field strength. Due to their simplicity, these expressions can be included in the magnetohydrodynamic simulation of supernovae and accretion disks to calculate neutrino and antineutrino transport in them. The rates of beta processes and the energy and momentum emitted in them are calculated for an optically transparent matter. It is shown that the macroscopic momentum transferred in the medium increases linearly with the magnetic field strength and can substantially affect the dynamics of supernovae and accretion disks in the regions of a degenerate matter. It is also shown that the rates of beta processes and the energy emission for a magnetic field strength of B ? 10¹⁵ G typical of supernovae and accretion disks are lower than in the absence of field. This suppression is stronger for reactions with neutrinos.     

Optical results of the black hole microquasar SS 433

We present optical spectroscopic observations of SS 433 during different precessional and orbital phases. Our 2004, 2007 and 2008 data provide us a good chance to study the variability of the Hα line at different orbital phases for nearly the same disk inclination. The data show that the Hα of SS 433 usually had a symmetric profile between orbital phases 0.25–0.75, while an asymmetric structure with a strong red peak was observed for other orbital phases. We suggest that the orbital variability of Hα emission is connected with accretion flow from the donor star to the accretion disk. In addition, we attribute the dramatic increase of Hα emission during our 2007 observational run, which had a time scale of one day, to the emergence of strong jets.