Nodal and periastron precession of inclined orbits in the field of a rotating black hole

The inclination of low-eccentricity orbits is shown to significantly affect orbital parameters, in particular, the Keplerian, nodal precession, and periastron rotation frequencies, which are interpreted in terms of observable quantities. For the nodal precession and periastron rotation frequencies of low-eccentricity orbits in a Kerr field, we derive a Taylor expansion in terms of the Kerr parameter at arbitrary orbital inclinations to the black-hole spin axis and at arbitrary radial coordinates. The particle radius, energy, and angular momentum in the marginally stable circular orbits are calculated as functions of the Kerr parameter j and parameter s in the form of Taylor expansions in terms of j to within O[j ⁶]. By analyzing our numerical results, we give compact approximation formulas for the nodal precession frequency of the marginally stable circular orbits at various s in the entire range of the Kerr parameter.     

黑洞吸积盘内边缘半径的演化

本文用广义相对论讨论了黑洞吸积盘内边缘半径ｒ（ｍｓ）的演化规律。结果表明，吸积盘的中心黑洞在由Ｓｃｈｗａｒｚｓｃｈｉｌｄ型向极端Ｋｅｒｒ型演化的过程中，黑洞的角动量变化对ｒ（ｍｓ）的影响始终比黑洞的质量变化对ｒ（ｍｓ）的影响大。在此过程中ｒ（ｍｓ）始终是连续、单调减小的。本文得出ｒ（ｍｓ）对时间变化率的取值范围，并对其物理意义作了讨论。     

Observational signature of planet formation: The ALMA view

Protoplanetary disks are the most probable sites where planet formation takes place. According to theory, planet formation in protoplanetary disks should show remarkable signatures, such as a gap/hole or a spiral structure. In fact, recent high-angular and high-sensitivity observations in millimeter and submillimeter wavelengths, as well as optical/near-IR wavelengths, have shown such structures in protoplanetary disks. Two particular examples of such disks around AB Aurigae and HD 142527 are discussed here, with an emphasis on results obtained using the Submillimeter Array. These disks—and their probable planet formation—will be very important future targets for ALMA to study the physical process of planet formation in detail.     

A Study of the Scale Height of the Thin Galactic Disk in the Solar Neighborhood

An attempt is made to determine the scale height of the thin Galactic disk in the solar neighborhood using various stellar samples from the accurate astrometric data of the Hipparcos satellite. Using the Tycho color indices and considering the completeness of the samples, several samples were selected from the main sequence and the horizontal branch. Based on two rather complete samples, it is found that the scale height of the Galactic disk defined by the O-B type main sequence stars is 103.1 ± 3.0 pc and the Sun is located at height of 15.2 ± 7.3 pc above its mean plane; while the scale height of the Galactic disk defined by the horizontal branch stars is 144.0 the ±10.0 pc and the Sun is located at height 3.5 ± 5.4 pc above the mean plane. Owing to the incompleteness of observational samples, it is not possible to use the main sequence stars of spectral types A, F, G, K and M to make a reliable determination of the scale height.     

Bimodality of anomalous pulsars?

At present, it is widely believed that anomalous X-ray pulsars (AXPs), soft gamma-ray repeaters (SGRs), rotational radio transients (RRATs), compact central objects (CCOs) in supernova remnants, and X-ray dim isolated neutron stars (XDINSs) belong to different classes of anomalous objects in which the central bodies are isolated neutron stars. Previously, we have shown that AXPs and SGRs can be described in terms of the drift model for parameters of the central neutron star typical of radio pulsars (rotation periods P ～ 0.1–1 s and surface magnetic fields B ～ 10¹¹–10¹³ G). Here, we show that some of the peculiarities of the sources under consideration can be explained by their geometry (in particular, by the angle β between the rotation axis and the magnetic moment). If β ? 10° (an aligned rotator), the drift waves in the outer layers of the neutron star magnetosphere can account for the observed periodicity in the radiation. For large β (a nearly orthogonal rotator), the observed modulation of the radiation and its short bursts can be explained by mass accretion from the ambient medium (e.g., a relic disk).     

阿霉素性心肌病大鼠左心室肌纤维化程度与缝隙连接蛋白的变化

目的 探讨阿霉素性心肌病大鼠发生心律失常的发病机制。方法 健康wistar雄性大鼠20只,体重200g,适应周围环境1周后,随机将20只wistar雄性大鼠分为对照组（n=10）和阿霉素（ADR）组（n=10）。ADR组的大鼠在1周内进行3次腹腔注射ADR 2mg/kg;同时对照组则进行3次腹腔注射0.9%NaCl （2ml/kg）,停药后让两组大鼠自由饮食4周。7周后对两组大鼠行心脏彩超检测,左心室舒张末径（LVEDd）与左心室收缩末期内径（LVESd）及左心室射血分数（LVEF）,行VG染色观察各组大鼠心肌纤维化情况;扫描电镜染色观察左心室心肌细胞闰盘病理学变化;两组大鼠心肌结缔组织生长因子（CTGF）、转化生长因子β1（TGF-β1）、N型钙黏蛋白（N-cad）、桥粒芯糖蛋白（DSG2）表达应用ELISA法检测;采用Western blot法检测两组大鼠的心肌细胞Cx40 、Cx43、p-Cx43蛋白表达。结果 与对照组相比,阿霉素组大鼠明显出现心室重构,并易出现心律失常;电镜下观察ADR组大鼠心肌细胞闰盘破损严重,间隙增宽,VG染色显示ADR组大鼠病理积分明显高于对照组（P<0.05）;ADR组大鼠相较于对照组大鼠心室肌中CTGF、TGF-β1的表达升高显著,N-cad、DSG2、Cx40、Cx43及p-Cx43的表达明显减低（P<0.05）。结论 ADR组大鼠可能由于心室肌细胞纤维化、闰盘结构受损、缝隙连接重构等原因导致心律失常。