太阳系外行星系统轨道参数的统计研究

自1995年第一颗类太阳恒星周围的系外行星发现以来,随着已发现的系外行星数目的增多,对系外行星性质的统计分析变得重要和有意义。截至2011年6月9日,共发现系外行星555颗。以这些系外行星的轨道参数为依据,对系外行星的性质进行统计分析,得出了一些有意义的结论。同时简要介绍现有的行星形成与演化模型并依据得出的行星统计性质对其进行检验,这对于系外行星的进一步探测具有一定的指导作用。     

系外行星凌星观测指南

为什么要观测凌星？ 当代天文学家对于在茫茫银河系内的千亿颗恒星周围寻找太阳系之外的行星（称“太阳系外行星”,后文简称“系外行星”）,尤其是类似地球这样可能孕育生命的星球（类地行星）有着极高的兴趣和热情。这一方面得益于人类对于探索地外生命与文明的不懈追求,另一方面对这些系外行星的探测及其物理性质的分析,对深入理解行星系统（尤其是我们所处的太阳系）的形成与演化机制也有着重要作用。     

宇宙信息

HARPS新发现32颗太阳系外行星 高精度视向速度行星搜寻（HARPS）计划宣布新发现了32颗太阳系外行星,这使得系外行星的发现总数超过了400颗。这批新发现的系外行星涵盖了过去发现的所有类型,从热类木星、超级海王星和超级地球再到低质量、贫金属恒星周围以及多行星系统中的行星。     

太阳系外行星系统构型的形成与动力学

自从Maryor和Queloz于1995年在51Pegb周围发现了第1颗主序恒星系统内的行星以来,人类已经利用越来越精密的探测方法获得了更多的太阳系外行星系统的信息.截至2010年3月,人类已经探测到了431颗太阳系外行星,其中包含了45个多行星系统.从统计结果来看,系外行星系统的构型以及行星的特点与太阳系存在很多差异.研究这些系统的形成过程可以对太阳系的形成有更深刻的理解,并将推进行星系统形成理论的发展.     

太阳系外行星探测研究进展

太阳系外行星作为研究恒星演化重要的天体和探索生命起源的基础,多年来一直是天文学前沿研究的热点之一,目前已发展出近10种系外行星的探测方法.随着天文观测设备探测精度越来越高,自1992年至今,已发现4 000余颗系外行星.近几年天基天文观测手段日趋成熟,探测系外行星的精度与效率得到了极大提高,并带动着更多地基系外行星探测...     

行星大样本演化的研究进展

随着系外行星观测样本的大量积累,大样本演化方法作为天体物理的重要方法,继在恒星物理中广泛应用后,在行星统计特征的研究中开始变得更加重要。行星大样本演化方法就是通过简化的行星形成演化模型,对大量初始条件(原行星盘参数)和边界条件(星周环境)同时进行模拟,给出行星的各种统计性质,并直接与观测上的行星样本统计特征做比较。该方法对于限制行星形成和演化的理论模型具有重要意义。对行星大样本演化模型进行概述,简要介绍了行星大样本演化的主要统计结果和最新进展,并对其未来发展作出了展望。     

基于Kepler Q1–Q17数据对类太阳型恒星的行星生成率估算

近30年来的系外行星探测揭示了行星在宇宙中普遍存在的事实.为了深入研究适宜生命居住行星的普遍性,一方面需要了解宜居行星的特性;另一方面可以通过分析已发现系外行星的分布特征,推算该类行星在恒星周围的存在几率.在目前已发现的系外行星中,凌星法发现的占据了绝大多数,如Kepler空间望远镜所观测的系外行星共有2344颗. 2018年Kepler正式退役,其科学团队发布了最终版的Kepler Data Release (DR25),包含观测季度Q1–Q17的恒星共198709颗.通过对Kepler数据的分析,使用逆检测效率法和最大似然分析法两种不同的方法对系外行星半径周期参数空间内的行星生成率进行了估算,同时将计算样本根据恒星的光谱类型进行分类,分别估算得到了F、G、K型的Kepler恒星周围的行星生成率及其整体的生成率.对于半径范围1–20 R_⊕(R_⊕为一个地球半径),轨道周期范围0.4–400 d的Kepler凌星系外行星,宿主恒星为F型时逆检测效率法和最大似然法估算得到的行星生成率分别为0.36±0.02和0.47±0.02,宿主恒星为G型时的...     

系外行星大气研究现状

探测系外行星的最终目的是为了寻找系外生命和宣居行星,而系外行星大气是人们了解行星宜居特性的窗口,所以系外行星大气的研究至关重要。近10年来,系外行星大气的理论研究和观测都发展迅速。受观测技术限制,目前观测到大气的系外行星主要是用凌星法探测到的热木星和超级地球,还有用直接成像法探测到的离主星较远的年轻气态巨行星。力求在系外行星大气领域飞速发展之际,对该领域研究现状做简明介绍。首先介绍系外行星大气的观测方法,随后介绍热木星和超级地球的大气概况和研究现状,最后对系外行星大气探测的有关项目进行简要介绍,以展示未来系外行星大气研究的前景。     

双星系统中行星的形成及动力学

自1995年在类太阳恒星周围发现第1颗太阳系外行星(简称系外行星)以来,到目前为止发现的系外行星数目已达500多个.恒星一般诞生在双星系统中,因此在双星系统中发现行星是很自然的.目前的观测统计显示,双星系统中具有行星的恒星比例大概为17％.显然这个比例应该看成一个下限,因为很强的观测选择效应使很多行星观测计划避开了双星系统.目前发现的有行星的双星系统大都为S型,即一颗伴星围绕着里面的恒星-行星系统公转.一般S型的双星轨道间距在100 AU以上,不过目前也发现了4个S型双星轨道间距在20 AU左右.这些系统包括Gamma Cephei、GJ 86、HD41004和HD 196885.除了以上介绍的S型双星,还有一类叫P型,即行星围绕两个恒星公转.P型的双星到目前为止只发现并确认了两例.本论文将主要研究S型双星系统中的行星形成. 在第1章,我们首先概括了到目前为止有关单星和双星系统中行星的观测特征.然后,我们系统地介绍了有关行星形成的理论模型,特别是这些理论模型应用到双星系统中时需要考虑的情况变化.双星系统中,由于伴星的引力扰动,行星形成与之在单星系统中相比变得更加复杂.伴星的引力可以激发起星子的轨道,从而使得它们的碰撞速度增大到大于星子的表面逃逸速度,甚至大于使星子碎裂的极限速度.行星形成的中间(第2)阶段—从星子到行星胚胎,因此变得问题重重和扑朔迷离.我们接下来的内容将主要集中在这个问题很多的中间阶段,看星子能否以及如何顺利通过这个阶段.     

深入“特丝”巡星之旅

凌星太阳系外行星巡天卫星正在革新人类对太阳邻域中行星的认识,但发现新的行星只是开始。1995年,在类太阳恒星旁发现了首颗太阳系外行星。到2005年,太阳系外行星搜寻仍处于襁褓中。天文学家当时依然不清楚,环绕其他恒星的行星是普遍存在的,还是罕见的个案。     

Radiative association of C and P, and Si and P atoms

The rate coefficients for the formation of carbon monophosphide (CP) and silicon monophosphide (SiP) by radiative association are estimated for temperatures ranging from 300 to 14 100 K. In this temperature range, the radiative association rate coefficients are found to vary from  1.14 × 10⁻¹⁸  to  1.62 × 10⁻¹⁸ cm³ s⁻¹  and from  3.73 × 10⁻²⁰  to  7.03 × 10⁻²⁰ cm³ s⁻¹  for CP and SiP, respectively. In both cases, rate coefficients increase slowly with the increase in temperature.     

DDO photometry and metallic abundances of E and SO galaxies and globular clusters of the LMC and SMC

Metallicity of 8 E and SO galaxies as well as that of red globulars of the LMC and SMC were obtained by means of DDO integrated photometry calibrated with galactic globular clusters (Bica and Pastoriza, 1983; hereafter referred to as Paper I). A correction was obtained in order to reduce the colors of the galaxies to zero redshift. The relation metallicity vsM _V for the galaxies is analyzed (adding to our sample the observations of McClure and Van den Bergh, 1968; and Faber, 1973a). For the Magellanic Clouds we found metallicity ranging from intermediate to poor.     

Substructure and the cusp and fold relations

Gravitational lensing of a background source by a foreground galaxy lens occasionally produces four images of the source. The cusp and the fold relations impose conditions on the ratios of magnifications of these four-image lenses. In this theoretical investigation, we explore the sensitivity of these relations to the presence of substructure in the lens. Starting with a smooth lens potential, we add varying amounts of substructure, while keeping the source position fixed, and find that the fold relation is a more robust indicator of substructure than the cusp relation for the images. This robustness is independent of the detailed spatial distribution of the substructure, as well as of the ellipticity of the lensing potential and the presence of external shear.     

Gravity and Topography of Moon and Planets

Planetology serves the understanding on the one hand of the solar system and on the other hand, for investigating similarities and differences, of our own planet. While observational evidence about the outer planets is very limited, substantial datasets exist for the terrestrial planets. Radar and optical images and detailed models of gravity and topography give an impressive insight into the history, composition and dynamics of moon and planets. However, there exists still significant lack of data. It is therefore recommended to equip all future satellite missions to the moon and to planets with full tensor gravity gradiometers and radar altimeters.     

Fragmentation and hydration of tektites and microtektites

Abstract— An examination of data collected over the last 30 years indicates that the percent of glass fragments vs. whole splash forms in the Cenozoic microtektite strewn fields increases towards the source crater (or source region). We propose that this is due to thermal stress produced when tektites and larger microtektites fall into water near the source crater while still relatively hot (>1150 °C). We also find evidence (low major oxide totals, frothing when melted) for hydration of most of the North American tektite fragments and microtektites found in marine sediments. High-temperature mass spectrometry indicates that these tektite fragments and microtektites contain up to 3.8 wt% H₂O. The H₂O-release behavior during the high-temperature mass-spectrometric analysis, plus high CI abundances (0.05 wt%), indicate that the North American tektite fragments and microtektites were hydrated in the marine environment (i.e., the H₂O was not trapped solely on quenching from a melt). The younger Ivory Coast and Australasian microtektites do not exhibit much evidence of hydration (at least not in excess of 0.5 wt% H₂O); this suggests that the degree of hydration increases with age. In addition, we find that some glass spherules (with <65 wt% SiO₂) from the upper Eocene clinopyroxene-bearing spherule layer in the Indian Ocean have palagonitized rims. These spherules appear to have been altered in a similar fashion to the splash form K/T boundary spherules. Thus, our data indicate that tektites and microtektites that generally contain >65 wt% SiO₂ can undergo simple hydration in the marine environment, while impact glasses (with <65 wt% SiO₂) can also undergo palagonitization.     

Radii and Albedos of four Trojan asteroids and Jovian satellites 6 and 7

Thermal radiation has been detected from four asteroids of the Trojan group, and J6 and J7, the brightest of the outer satellites of Jupiter. The six objects all have exceedingly low geometric albedos of 0.02 or 0.03 according to calculations based on their known visual brightness and the measured thermal fluxes. 624 Hektor, the largest object studied here, has a radius of 110 ± 20 km, though the exact shape of this body is in question. While the sample observed in this work is small (the total number of Trojans larger than 0.25 km in radius is about 1000), the fact that all four studied have similarly low albedos suggests that this property is characterisic of the Trojans and at least two of the outer members of Jupiter's retinue of satellites. The low surface albedo of the Trojans may preclude the proposed origin of the Jovian group of comets among these bodies according to E. Rabe. Updated tables of the dimensions of all the Jovian satellites are given.     

Uranus and Neptune: Shape and rotation

Both Uranus and Neptune are thought to have strong zonal winds with velocities of several 100 m s⁻¹. These wind velocities, however, assume solid-body rotation periods based on Voyager 2 measurements of periodic variations in the planets’ radio signals and of fits to the planets’ magnetic fields; 17.24 h and 16.11 h for Uranus and Neptune, respectively. The realization that the radio period of Saturn does not represent the planet’s deep interior rotation and the complexity of the magnetic fields of Uranus and Neptune raise the possibility that the Voyager 2 radio and magnetic periods might not represent the deep interior rotation periods of the ice giants. Moreover, if there is deep differential rotation within Uranus and Neptune no single solid-body rotation period could characterize the bulk rotation of the planets. We use wind and shape data to investigate the rotation of Uranus and Neptune. The shapes (flattening) of the ice giants are not measured, but only inferred from atmospheric wind speeds and radio occultation measurements at a single latitude. The inferred oblateness values of Uranus and Neptune do not correspond to bodies rotating with the Voyager rotation periods. Minimization of wind velocities or dynamic heights of the 1 bar isosurfaces, constrained by the single occultation radii and gravitational coefficients of the planets, leads to solid-body rotation periods of ∼16.58 h for Uranus and ∼17.46 h for Neptune. Uranus might be rotating faster and Neptune slower than Voyager rotation speeds. We derive shapes for the planets based on these rotation rates. Wind velocities with respect to these rotation periods are essentially identical on Uranus and Neptune and wind speeds are slower than previously thought. Alternatively, if we interpret wind measurements in terms of differential rotation on cylinders there are essentially no residual atmospheric winds.     

On universal elements,and conversion procedures to and from position and velocity

An element set is advocated that is familiar (in traditional terms), and yet applicable to every type of conic-section orbit without loss of accuracy. It is not free of singularity, but this is not a serious deficiency. Conversion procedures, to and from position and velocity, are outlined, with Fortran-77 listings appended. Tests have indicated that the errors in the pair of procedures are minimal, accuracy being limited only by computer precision and the (fixed) number of iterations used in the Kepler-equation solutions.