2021年空间科学热点回眸

 回顾了2021年全球空间科学重要进展、美欧俄中等国家和地区组织最新空间科学重大发展战略和规划、新发射的空间科学任务平台和新选定的未来任务。盘点了“帕克太阳探测器”首次飞越日冕，“洞察号”揭示火星内部结构，阿联酋、中国、美国探测器齐聚火星，美国绘制天文学和天体物理学发展路线图，欧洲确定2035-2050年大型空间科学任务科学主题，中俄发布国际月球科研站路线图，“詹姆斯·韦伯空间望远镜”成功发射，中国成功发射太阳探测科学技术试验卫星和可持续发展科学卫星，美欧批准新的金星探测任务等重大成果和事件。     

Magnetic fields at the solar wind termination shock

A transition between the supersonic solar wind and the subsonic heliosheath was observed by Voyager 1, but the expected termination shock was not seen owing to a gap in the telemetry. Here we report observations of the magnetic field structure and dynamics of the termination shock, made by Voyager 2 on 31 August-1 September 2007 at a distance of 83.7 au from the Sun (1 au is the Earth-Sun distance). A single crossing of the shock was expected, with a boundary that was stable on a timescale of several days. But the data reveal a complex, rippled, quasi-perpendicular supercritical magnetohydrodynamic shock of moderate strength undergoing reformation on a scale of a few hours. The observed structure suggests the importance of ionized interstellar atoms ('pickup protons') at the shock.     

Intense plasma waves at and near the solar wind termination shock

Plasma waves are a characteristic feature of shocks in plasmas, and are produced by non-thermal particle distributions that develop in the shock transition layer. The electric fields of these waves have a key role in dissipating energy in the shock and driving the particle distributions back towards thermal equilibrium. Here we report the detection of intense plasma-wave electric fields at the solar wind termination shock. The observations were obtained from the plasma-wave instrument on the Voyager 2 spacecraft. The first evidence of the approach to the shock was the detection of upstream electron plasma oscillations on 1 August 2007 at a heliocentric radial distance of 83.4 au (1 au is the Earth-Sun distance). These narrowband oscillations continued intermittently for about a month until, starting on 31 August 2007 and ending on 1 September 2007, a series of intense bursts of broadband electrostatic waves signalled a series of crossings of the termination shock at a heliocentric radial distance of 83.7 au. The spectrum of these waves is quantitatively similar to those observed at bow shocks upstream of Jupiter, Saturn, Uranus and Neptune.     

An asymmetric solar wind termination shock

Voyager 2 crossed the solar wind termination shock at 83.7 au in the southern hemisphere, approximately 10 au closer to the Sun than found by Voyager 1 in the north. This asymmetry could indicate an asymmetric pressure from an interstellar magnetic field, from transient-induced shock motion, or from the solar wind dynamic pressure. Here we report that the intensity of 4-5 MeV protons accelerated by the shock near Voyager 2 was three times that observed concurrently by Voyager 1, indicating differences in the shock at the two locations. (Companion papers report on the plasma, magnetic field, plasma-wave and lower energy particle observations at the shock.) Voyager 2 did not find the source of anomalous cosmic rays at the shock, suggesting that the source is elsewhere on the shock or in the heliosheath. The small intensity gradient of Galactic cosmic ray helium indicates that either the gradient is further out in the heliosheath or the local interstellar Galactic cosmic ray intensity is lower than expected.     

Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock

The solar wind blows outward from the Sun and forms a bubble of solar material in the interstellar medium. The termination shock occurs where the solar wind changes from being supersonic (with respect to the surrounding interstellar medium) to being subsonic. The shock was crossed by Voyager 1 at a heliocentric radius of 94 au (1 au is the Earth-Sun distance) in December 2004 (refs 1-3). The Voyager 2 plasma experiment observed a decrease in solar wind speed commencing on about 9 June 2007, which culminated in several crossings of the termination shock between 30 August and 1 September 2007 (refs 4-7). Since then, Voyager 2 has remained in the heliosheath, the region of shocked solar wind. Here we report observations of plasma at and near the termination shock and in the heliosheath. The heliosphere is asymmetric, pushed inward in the Voyager 2 direction relative to the Voyager 1 direction. The termination shock is a weak, quasi-perpendicular shock that heats the thermal plasma very little. An unexpected finding is that the flow is still supersonic with respect to the thermal ions downstream of the termination shock. Most of the solar wind energy is transferred to the pickup ions or other energetic particles both upstream of and at the termination shock.     

Voyager 1 exited the solar wind at a distance of approximately 85 Au from the Sun

The outer limit of the Solar System is often considered to be at the distance from the Sun where the solar wind changes from supersonic to subsonic flow. Theory predicts that a termination shock marks this boundary, with locations ranging from a few to over 100 au (1 Au approximately 1.5 x 10(8) km, the distance from Earth to the Sun). 'Pick-up ions' that originate as interstellar neutral atoms should be accelerated to tens of MeV at the termination shock, generating anomalous cosmic rays. Here we report a large increase in the intensity of energetic particles in the outer heliosphere, as measured by an instrument on the Voyager 1 spacecraft. We argue that the spacecraft exited the supersonic solar wind and passed into the subsonic region (possibly beyond the termination shock) on about 1 August 2002 at a distance of approximately 85 Au (heliolatitude approximately 34 degrees N), then re-entered the supersonic solar wind about 200 days later at approximately 87 au from the Sun. We show that the composition of the ions accelerated at the putative termination shock is that of anomalous cosmic rays and of interstellar pick-up ions.     

太阳活动峰年和谷年期间黑子群与耀斑的统计分析

基于NOAA/SWPC公布的太阳活动数据,我们选取第24太阳活动峰年附近的12个连续月份(2011年7月至2012年6月)和第23太阳活动周谷年附近的12个连续月份(2005年7月至2006年6月),统计了这两段时间中太阳黑子群和耀斑的活动规律,并根据时间、黑子群分布纬度、寿命和磁场类型等对峰年和谷年进行了详细分析和比较,主要结论如下所述.(1)黑子群数随时间的变化在峰年和谷年均比较随机,峰年期间黑子数比谷年增多1.5倍左右.耀斑爆发与黑子群活动具有良好的相关性,但峰年期间存在某个月份耀斑数很少的现象,而谷年期间存在某个月份耀斑数集中增多的现象.(2)无论峰年还是谷年,δ类型黑子群的耀斑产率(耀斑总数与黑子群总数之比)最大,但β型黑子群产生的耀斑爆发最多.耀斑产率与磁场类型有密切关系,但与其所处太阳活动周中的阶段无关.(3)黑子群和耀斑的纬度分布的南北不对称性,以X级耀斑最为显著.峰年较谷年的耀斑数增加主要集中在C级和M级.(4)耀斑产率同黑子群寿命具有良好的相关性,但黑子群的数目同它们的寿命之间没有明显的规律.     

Transport of solar wind into Earth's magnetosphere through rolled-up Kelvin-Helmholtz vortices

Establishing the mechanisms by which the solar wind enters Earth's magnetosphere is one of the biggest goals of magnetospheric physics, as it forms the basis of space weather phenomena such as magnetic storms and aurorae. It is generally believed that magnetic reconnection is the dominant process, especially during southward solar-wind magnetic field conditions when the solar-wind and geomagnetic fields are antiparallel at the low-latitude magnetopause. But the plasma content in the outer magnetosphere increases during northward solar-wind magnetic field conditions, contrary to expectation if reconnection is dominant. Here we show that during northward solar-wind magnetic field conditions-in the absence of active reconnection at low latitudes-there is a solar-wind transport mechanism associated with the nonlinear phase of the Kelvin-Helmholtz instability. This can supply plasma sources for various space weather phenomena.     

基于临时加固策略的日光温室极端风雪灾害对策

为研究极端风雪灾害下日光温室结构的加固对策,利用ANSYS有限元分析软件,考虑材料非线性、几何大变形以及结构非线性条件,建立日光温室单榀骨架模型.分别模拟风荷载、雪荷载、风主导风雪荷载、雪主导风雪荷载4种荷载工况下日光温室结构失稳破坏的全过程,得到了其失稳模式与结构荷载位移关系曲线,并根据失稳模式提出相应临时加固办法.结果表明:临时加固对日光温室抗风雪灾害能力提升明显,加固后日光温室结构对风荷载承载能力提升154%～300%,对雪荷载承载能力提升11%～129%,对风主导风雪荷载承载能力提升245%～273%,对雪主导风雪荷载承载能力提升203%～264%.     

Latitude migration of solar activity at high latitudes

Utilized here is the Carte Synoptique solar filament archive, namely the catalogue of solar filaments from March 1919 to December 1989, corresponding to solar rotation numbers 876 to 1823 to study latitudinal migration of solar activity at high latitudes. Except the well-known poleward migration of solar activity from middle latitudes to the poles, an equatorward migration is found from the solar poles toward middle latitudes （about 40°） within a normal cycle, which is neglected before, and the time interval for the former migration （4.4 years） is about 2.2 years shorter than that for the latter （6.6 years）, indicating that the change from one migration to the other takes place around the maximum time of a normal cycle. In the future, a dynamo model should represent the migration from the poles toward middle latitudes of the Sun, besides the migration in ＂butterfly diagrams＂ and the ＂rush to the poles＂. The traditional extended activity cycle is actually a part of the period of the successive migration from the poles toward the solar equator.     

考虑设备风险和风光不确定性的园区综合能源随机优化运行

综合能源系统因其能源梯级利用的高效性被广泛应用,而在运行过程中各设备的潜在故障风险与风光出力波动会成为系统供能稳定性的安全隐患。为此本文首先基于设备负载率建立了故障概率模型与设备风险模型。其次针对风光出力的不确定性采取蒙特卡洛采样法生成典型场景,建立了考虑设备风险与风光不确定性的综合能源多目标随机优化模型,运用分段线性化、宽容分层序列法将该模型处理为混合整数模型。最后通过算例仿真表明所提优化模型能够兼顾运行风险与经济成本,相较于传统经济调度,在总成本仅上升了9.6%时、设备风险降低了79.3%,证明了模型的经济性与安全性。     

障碍物对孤立山丘三维风场的影响

采用数值计算软件FLUENT研究障碍物的尺寸、障碍物与山坡坡底的距离对山丘风场的影响.根据计算结果绘制山顶上方50m处的湍流强度和速度变化图,山丘表面风速值线图以及来流方向分风速等值线图.分析结果表明:障碍物越高,距离山坡坡底越近,山顶风速减小幅度越大,越不稳定;山丘上游存在障碍物时,迎风坡和背风坡均出现低速区;障碍物距离山坡坡底较近时,迎风面上还出现了回流现象.迎风面、背风面的速度变化较大,不适合安装风力机;山丘两侧风速一直变化不大,比较适合安装风力机.     

渤海海峡风浪特征统计分析

利用最新相关海洋气象资料分析渤海海峡风、浪、流等分布特征和变化规律.研究表明,进入20世纪90年代,渤海海域的年大风日数明显减少;在同等风力条件下,秋冬季节容易激发波浪的形成和波高增大;在秋冬季波浪形成延迟时间短,在春夏季延迟时间长.偏北风起浪慢,延迟时间长;偏南风起浪快,延迟时间短.研究结果对客滚船驾驶人员保障船舶的安全航行具有实际应用价值.     

"一次就业率"不宜提倡

剖析了“一次就业率”的弊端     

基于CuPc的反式钙钛矿太阳能电池低温制备

引入一种典型的p型半导体材料CuPc,采用反式钙钛矿太阳能电池结构,利用热蒸发沉积方法将其作为电池的空穴传输层,在低温条件下制备电池器件.对不同厚度CuPc膜对钙钛矿电池性能的影响进行了优化,采用电流-电压测试、扫描电镜、原子力显微镜和X-射线衍射等方法分析了电池的光电性能和薄膜质量.研究结果表明:热蒸发沉积的CuPc层具有良好的平整性和覆盖性,当其厚度为10 nm时,器件在刚性基底上取得了15.37%的最高光电转化效率,在柔性基底上取得了12.66%的最高光电转化效率.该电池制备过程简单、成本低且重复性高,为进一步制备大面积、高效率以及柔性化的钙钛矿太阳能电池提供了参考.