HY-1C卫星影像中太阳耀斑区域的预测技术研究          下载免费PDF全文

《海洋技术学报》2023,(3)

对卫星影像太阳耀斑区域的预测是保障船-星同步观测有效实施的基础性工作。本文在对HY-1C卫星影像各像元观测几何分析的基础上,简化构建卫星影像各像元的网格化模型,介绍了利用卫星轨道报估算的卫星-太阳-像元位置的观测几何,进而估算卫星影像中太阳耀斑区域的技术方法。经与HY-1C实际卫星影像的应用比对,表明本文预测的像元位置、太阳位置以及卫星观测天底角/方位角均与实际影像数据具有很好的重合度,预测的太阳耀斑区域与实际影像耀斑掩码区重合度良好,验证了该方法能够预测影像中太阳耀斑区域,保障船-星同步观测的能力。  相似文献   

地球自转速度的年变化   总被引：11，自引：10，他引：1       下载免费PDF全文

宋贯一  曹志成  王吉易  杨同林 《地球物理学进展》2007,22(4):1225-1228

本文利用宋贯一等（2006）发表的“极移的成因及其移动特征”一文中的自转轴受迫摆动资料,从理论上推断出地球自转速度年变化的特征.结果证明,理论计算出的地球自转速度年变化曲线形态特征与观测曲线形态特征十分吻合.从而得出,太阳辐射光压在南、北半球的不平衡分布是引起地球自转速度年变化的主要原因.  相似文献   

A note on strong mass loss from early sun and warm and wet Mars     

J. Kar 《Earth, Moon, and Planets》1996,73(2):187-192

Recently, the possibility of strong mass loss from an early sun has been proposed in connection with the lithium depletion problem along with early solar system problems. However, the time scale for this enhanced mass loss is uncertain. Using an empirical relation for the dependence of the Martian surface temperature on solar luminosity and surface pressure, we find that the mass loss time scale for a 1.1 M sun should be about 1 × 10⁹ years or longer if Mars had liquid water on its surface 3.8 billion years ago. The minimum surface pressure on early Mars should be about 5 bars of CO₂.  相似文献   

Magnetic reconnection in solar flares     

T. G. Forbes 《地球物理与天体物理流体动力学》2013,107(1-4):15-36

Abstract

The magnetic energy stored in the corona is the only plausible source for the energy released during large solar flares. During the last 20 years most theoretical work has concentrated on models which store magnetic energy in the corona in the form of electrical currents, and a major goal of present day research is to understand how these currents are created, and then later dissipated during a flare. Another important goal is to find a flare model which can eject magnetic flux into interplanetary space. Although many flares do not eject magnetic flux, those which do are of special importance for solar-terrestrial relations since the ejected flux can have dramatic effects if it hits the Earth's magnetosphere. Three flare models which have been extensively investigated are the emerging-flux model, the sheared-arcade model, and the magnetic-flux-rope model. All of these models can store and release magnetic energy efficiently provided that rapid magnetic reconnection occurs. However, only the magnetic-flux-rope model appears to provide a plausible mechanism for ejecting magnetic flux into interplanetary space.  相似文献   

甘肃金塔地区大气对太阳射电辐射吸收的测量研究     

刘炎  李东  宋其武  孟璇  许富英  吴洪敖  宁宗军 《天文学报》2011,52(5):377-384

2008年8月1日,在我国西北的新疆、内蒙、甘肃等地区可以观测到一次日全食的天象,紫金山天文台太阳射电团组在甘肃省金塔用两架太阳射电望远镜对这次日全食进行了观测,并成功地取得了观测资料.为了科学分析观测资料,在日全食的前两天,实测了当地的大气吸收.着重分析这些观测数据,结合太阳射电方法,测得在λ=2.4 cm和λ=8....  相似文献   

日晕测量与日晕光度计外缘杂散光抑制试验     

刘念平  刘煜  申远灯  张雪飞  曹文达  Arnaud Jean 《天文学报》2011,52(2)

为配合大型太阳设备西部选址工作,研制了一架现代日晕光度计(Sky Brightness Monitor,SBM).前期实验对日晕光度计性能进行了测试,同时积累了云南部分址点的日晕数据.资料分析结果显示,轿子雪山正午前后的日晕水平最低可至日面中心强度百万分之几的量级(蓝波段).这表明该日晕光度计内部杂散光水平已达到了国际同类产品的标准.日晕光度计的内部杂散光源主要来自两部分:镜筒前端中性滤光片(ND4)固定套圈的边缘衍射(视场靠内区域)和镜筒内置光阑的边缘衍射(视场靠外区域).针对后者进行的变换光阑孔径大小试验结果证实,适当缩小光阑孔径可有效减小数据中视场靠外区域的衍射光干扰.  相似文献   

Two Sympathetic Homologous CMEs on 2002 May 22     

Jian-Xia Cheng  Cheng Fang  Peng-Fei Chen  Ming-De Ding Department of Astronomy  Nanjing University  Nanjing   《中国天文和天体物理学报》2005,5(3):265-272

Sympathetic coronal mass ejections (CMEs) usually occur in different active regions connected by interconnecting magnetic loops, while homologous CMEs occur within the same active region with an almost the same background magnetic field, and so are similar in shapes. Two sympathetic CMEs erupted within 3 hours on 2002 May 22, originating from the same active region, AR 9948. Their multi-wavelength data were collected and analyzed. It is suggested that emerging flux triggered the occurrence of the first CME and the corresponding flare, the reconnection inflow of which in turn triggered the eruption of the second CME. Based on the fact that the two sympathetic CMEs have many similarities, in their shapes, their low-lying dimming areas, etc., we tentatively propose, for the first time, the phenomenon of sympathetic homologous CMEs.  相似文献   

太阳分米波射电快速精细结构的观测分析     

段长春  汪敏  许春  谢瑞祥 《天文研究与技术》2002,(4):19-28

通过分析云南天文台(YNO)0.7～1.5GHz太阳射电频谱仪2000年9月至2001年9月取得的158个射电爆发,发现其中约有65%存在4类不同类型的快速精细结构(FFS):毫秒尖峰辐射、Ⅲ型爆发、准周期脉动、慢漂移结构。给出了其中6个典型精细结构的介绍和相关的初步解释。  相似文献   

Excitation of solar-like oscillations: From PMS to MS stellar models     

R. Samadi  M. -J. Goupil  E. Alecian  F. Baudin  D. Georgobiani  R. Trampedach  R. Stein  å. Nordlund 《Journal of Astrophysics and Astronomy》2005,26(2-3):171-184

The amplitude of solar-like oscillations results from a balance between excitation and damping. As in the sun, the excitation is attributed to turbulent motions that stochastically excite thep modes in the uppermost part of the convective zone. We present here a model for the excitation mechanism. Comparisons between modeled amplitudes and helio and stellar seismic constraints are presented and the discrepancies discussed. Finally the possibility and the interest of detecting such stochastically excited modes in pre-main sequence stars are also discussed.  相似文献   

太阳活动周期的小波分析   总被引：5，自引：0，他引：5  

占腊生  何娟美  叶艺林  赵海娟 《天文学报》2006,47(2):166-174

运用小波技术对太阳射电流量2800 MHz,太阳黑子数和太阳黑子面积数周期进行分析．其结果表明: (1)这3个系列的数据显示最显著的周期是10．69年,其他周期并不明显．(2)小波功率谱给出了全部时间-周期范围的功率谱变化,它显示了在某个周期处于某个时段的局部功率的变化,小波功率谱分析表明,小于1年的周期仅仅在太阳活动最大期附近比较明显．(3)太阳射电2800 MHz,太阳黑子数和太阳黑子面积数的几个周期(10．69年,5．11年, 155．5天)的小波功率谱比较相似,出现峰值的时间相同;曲线的起伏相似,周期越小,曲线起伏的频率越大．  相似文献