From solar nanoflares to stellar giant flares: Scaling laws and non-implications for coronal heating

In this study we explore physical scaling laws applied to solar nanoflares, microflares, and large flares, as well as to stellar giant flares. Solar flare phenomena exhibit a fractal volume scaling, V(L)  L^1.9, with L being the flare loop length scale, which explains the observed correlation between the total emission measure EM_p and flare peak temperature T_p in both solar and stellar flares. However, the detected stellar flares have higher emission measures EM_p than solar flares at the same flare peak temperature T_p, which can be explained by a higher electron density that is caused by shorter heating scale height ratios s_H/L ≈ 0.04–0.1. Using these scaling laws we calculate the total radiated flare energies E_X and thermal flare energies E_T and find that the total counts C are a good proxy for both parameters. Comparing the energies of solar and stellar flares we find that even the smallest observed stellar flares exceed the largest solar flares, and thus their observed frequency distributions are hypothetically affected by an upper cutoff caused by the maximum active region size limit. The powerlaw slopes fitted near the upper cutoff can then not reliably be extrapolated to the microflare regime to evaluate their contribution to coronal heating.     

绕大钝头短体外形跨音速大迎角湍流流动计算

采用数值模拟求解N-S方程方法计算与分析了绕大钝头短体外形的跨音速大迎角时的湍流流动.数值方法中选用Van Leer 分裂格式离散无粘通量项,并构造了一种Limiter函数以保证TVD(Total Variation Diminishing)性质,采用中心差分格式来离散粘性通量项.计算中采用了B-L湍流模型.算例定性地表明绕流的三维分离具有准周期性的非定常特性.     

管道截面的流速分布参数及其在涡街流量计标定中的应用

本文讨论了标定实验对涡街流量计所在截面流速分布的要求、拟合公式的选用和数据处理，以及使用标定结果时所要注意的问题。提出了一种以测试手段和分析办法相结合的关于标定涡街流量计的新的技术途径，以缩短标定装置的轴向尺寸，降低标定费用。对于充分湍流的圆管流动，根据Ｎｉｋｕｒａｄｓｅ的实验结果，给出了截面平均流速与最大流速之比随雷诺数变化的简洁计算公式。     

一种求解翼面类斜截面外形的简便方法

从飞机翼面外形设计的角度，利用顺气流截面弦长与任意斜截面弦长的相互关系，导出了一种求解翼面类斜截面外形的简便方法。本方法的优点是，可以方便地给出翼面类任意斜截面外形的相对坐标值。只要算出任意斜截面的弦长，就可以很快地得到对应外形的坐标值，而无需求解复杂的曲面方程。与传统的方法相比较，减少了计算量。这对于求解着于非顺气流方向的翼肋外形来说，尤其显得方便。文中以某型飞机机翼为例，分别用传统方法和简便方法进行计算，得到完全一致的结果。     

一个大挠度柱面弯曲板条的求解

本文应用付宝连的大挠度弯曲直梁的功的互等定理,求解一个柱面弯曲板条的挠曲面方程。     

“Oblique” Bernstein modes in solar preflare plasma: Generation of second harmonics

Process of second harmonics generation due to development of corresponding instability has been investigated for pure electron weakly oblique Bernstein mode. This mode was supposed to be modified by taking into account the influence of pair Coulomb collisions and weak large-scale electric field in flare loop. Investigated area was located near the loop foot-point in the “lower–middle” chromosphere of active region. It has been shown, that for the Fontenla–Avrett–Loeser model of solar atmosphere the investigated process of second harmonics generation starts at the extremely low threshold values of subdreicer electric field, well before the beginning of “preheating” phase of flare process.     

Gamma Astrometric Measurement Experiment (GAME) – Implementation and performance

The GAME mission concept is aimed at testing the General Relativity, through precise measurement of the gravitational deflection of light by the Sun, by means of an optimised telescope operating in the visible and launched in orbit on a small class satellite. We describe the proposed mission profile, the preliminary payload design and the expected performance. The targeted precision on the γ parameter of the PPN formulation of General Relativity is in the range 10⁻⁶ to 10⁻⁷. The measurement principle relies on the differential astrometric signature on the stellar positions. The instrument concept is based on a dual field, multiple aperture Fizeau interferometer, observing simultaneously two sky regions close to the solar limb. A beam combiner folds the telescope line of sight on two different directions on the sky, separated by a base angle of 4°. The diluted optics approach achieves an efficient rejection of the scattered solar radiation, while retaining an acceptable angular resolution on the science targets.     

Three-dimensional global simulation of multiple ICMEs’ interaction and propagation from the Sun to the heliosphere following the 25–28 October 2003 solar events

This study performs simulations of interplanetary coronal mass ejection (ICME) propagation in a realistic three-dimensional (3D) solar wind structure from the Sun to the Earth by using the newly developed hybrid code, HAFv.2+3DMHD. This model combines two simulation codes, Hakamada–Akasofu–Fry code version 2 (HAFv.2) and a fully 3D, time-dependent MHD simulation code. The solar wind structure is simulated out to 0.08 AU (18 Rs) from source surface maps using the HAFv.2 code. The outputs at 0.08 AU are then used to provide inputs for the lower boundary, at that location, of the 3D MHD code to calculate solar wind and its evolution to 1 AU and beyond. A dynamic disturbance, mimicking a particular flare’s energy output, is delivered to this non-uniform structure to model the evolution and interplanetary propagation of ICMEs (including their shocks). We then show the interaction between two ICMEs and the dynamic process during the overtaking of one shock by the other. The results show that both CMEs and heliosphere current sheet/plasma sheet were deformed by interacting with each other.     

FIP Effect in the Solar Upper Atmosphere: Spectroscopic Results

Recent spectroscopic measurements from instruments on the Solar and Heliospheric Observatory (SOHO) find that the coronal composition above a polar coronal hole is nearly photospheric. However, similar SOHO observations show that in coronal plasmas above quiet equatorial regions low-FIP elements are enhanced by a factor of ≈ 4. In addition, the process of elemental settling in coronal plasmas high above the solar surface was shown to exist. Measurements by the Ulysses spacecraft, which are based on non-spectroscopic particle counting techniques, show that, with the exception of He, the elemental composition of the fast speed solar wind is similar to within a factor of 1.5 to the composition of the photosphere. In contrast, similar measurements in the slow speed wind show that elements with low first ionization potential (FIP < 10 eV) are enhanced, relative to the photosphere, by a factor of 4-5. By combining the SOHO and Ulysses results, ideas related to the origin of the slow speed solar wind are presented. Using spectroscopic measurements by the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) instrument on SOHO the photospheric abundance of He was determined as 8.5 ± 1.3% (Y = 0.248). This revised version was published online in June 2006 with corrections to the Cover Date.     

一类垂足多边形的有向面积公式及其应用

给出圆内接多边形的垂足多边形的有向面积公式，并利用该公式获得圆内接多边形的垂足多边形和正多边形的垂足多边形的若干结果，从而推广了垂足三角形的一些结论。