1998年4月下旬至5月上旬地磁暴的日地事件认证

综合运用SOHO／LASCO、SOHO／EIT关于CME的观测结果和WIND飞船关于太阳风的观测记录，识别了1998年4月下旬至5月上旬发生的磁暴的CME源，分析了与5月初强磁暴群相联系的日地事件。结果表明，所用日地扰动事件关系认证的方法是可行的，本文就上述日地事件所涉及的磁暴群与活动区的关系、CME地磁效应的日面东西不对称性以及磁云与高速流的作用等问题进行了讨论。     

SOHO observations relating to the associationbetween flares and coronal mass ejections

Campaigns to investigate the solar coronal mass ejection (CME) onset have been run using the Solar andHeliospheric Observatory (SOHO) since 1996. These have included coronagraph and extreme-ultraviolet (EUV) disc imaging, along with magnetic mapping of the photosphere, in concert with EUV and UV spectroscopic observations. These campaigns have included co-ordination with ground-based observatories, and with other spacecraft, especially Yohkoh and the Transition Region and Corona Explorer (TRACE). This multi-instrument, multi-spacecraft effort has provided many rewards, with some spectacular observations of countless eruptions. It has included the discovery of unexpected phenomena such as EUV waves and groundbreaking work on coronal dimming, and the development of sigmoidal shaped structures. Much has been learnt about the CME onset yet the most basic questions still remain. We have an unprecedented view of CME eruptions, yet we are still unable to identify clearly the onset process and we do not fully understand the CME-flare relationship. With all of the campaigns producing excellent multi-wavelength observations of CMEs, how far have we progressed in the understanding of the CME onset and, in particular, the CME-flare relationship? Can we identify lines of research using the SOHO data, which will provide the answers we seek — or do we need fundamentally different observation scenarios? It is the author's opinion that we actually have the observational tools required to understand much about the onset process and the CME/flare links, and the emphasis should be on understanding the limitations of our instrumentation and on removing any preconceived ideas from our interpretations.     

Current and future activities in education and public outreach at the Observatoire de Haute Provence

The Haute Provence Observatory has for primary mission the operation of telescopes, up to two meters in diameter, for the astrophysics community, and the measurements of various upper atmosphere parameters for the geophysics community. An education and outreach program has been developed with several reached: from school pupils to post-doctorate students, teachers, and the general public. In the recent years we put emphasis on the formation of teachers and on the renewal of the general public visit. Given the wide range of education and outreach activities we cover, we had to develop a relation network with individuals, amateurs, teachers and institutions, amplifying our efforts. For the future, we will try to make an optimal use of the resources available in the St Michel l’Observatoire area, taking steps to reach an agreement with the neighbouring “Centre d’Astronomie”, a structure devoted to education and public outreach belonging to the local authorities.     

面向鱼眼图像的人群密度估计

针对传统人群密度估计方法在鱼眼图像畸变下不适用的问题,提出了一个面向鱼眼图像的人群密度估计方法,实现了在鱼眼镜头场景下对人流量的监控。在模型结构方面,引入了可变形卷积,提高了模型对鱼眼畸变的适应能力。在生成目标数据方面,利用鱼眼图像的畸变特点,基于高斯变换,对人群标注转换的密度图进行符合鱼眼畸变的分布匹配。在训练方面,对损失函数的计算进行了优化,避免了模型在训练中陷入局部最优解的问题。由于鱼眼人群计数的数据集比较匮乏,采集并标注了相应的数据集。通过主客观实验与经典方法进行了对比,所提方法在测试集中的平均绝对误差达3.78,低于对比方法,证明了面向鱼眼图像的人群密度估计方法的优越性。     

A statistical study of solar radio Type III bursts and space weather implication

Solar radio bursts (SRBs) are the signatures of various phenomenon that happen in the solar corona and interplanetary medium (IPM). In this article, we have studied occurrence of Type III bursts and their association with the Sunspot number. This study confirms that occurrence of Type III bursts correlate well with Sunspot number. Further, using the data obtained using e-CALLISTO network, we have investigated drift rates of isolated Type III bursts and duration of the group of Type III bursts. Since Type II, Type III and Type IV bursts are signatures of solar flares and/or CMEs, we can use the radio observations to predict space weather hazards. In this article, we have discussed two events that have caused near Earth radio blackouts. Since e-CALLISTO comprises more than 152 stations at different longitudes, we can use it to monitor the radio emissions from the solar corona 24 h a day. Such observations play a crucial role in monitoring and predicting space weather hazards within few minutes to hours of time.     

退火算法在电子元件位置优化上的应用

一块电路板上有电子元件，它们不仅有热源，而且相互和，另外与空气还交换热，对这类问题建立线性数学模型，从而算出温度稳态分布，因为许多集成电路系统可靠性很大程度上取愉于温度，所以温度的模拟显向很重要性，把温度模型与退火算法相结合可以获得元件最接近优化的布局，并用一个例子加以说明，通过优化能降低板子最高温度，从而提高系统的可靠性。     

A statistical study of post-flare-associated CME events

We present a statistical study of post-flare-associated CMEs (PFA-CMEs) during the period from 1996 to 2010. By investigating all CMEs and X-ray flares, respectively, in the LASCO and GOES archives, we found 15875 CMEs of which masses are well measured and 25112 X-ray flares of which positions are determined from their optical counterparts. Under certain temporal and spatial criteria of these CMEs and solar flare events, 291PFA-CMEs events have been selected. Linking the flare fluxes with CME speeds of these paired events, we found that there is a reasonable positive linear relation between the CME linear speed and associated flare flux. The results show also the CME width increases as the flux of its associated solar flare increases. Besides we found that there is a fine positive linear relation between the CME mass and its width. Matching the flare fluxes with CME masses of these paired events, we find the CME mass increases as the flux of its associated solar flare increases. Finally we find the PFA-CME events are in regular more decelerated than the other CMEs.     

X-ray source populations in nearby star-forming galaxies

We present results on the X-ray source populations of nearby star-forming galaxies based on Chandra observations. First we discuss the monitoring campaigns on the Antennae and M82 galaxies. In both cases we find that the majority of the X-ray sources exhibit intensity and/or spectral variability. However, despite of this variability, we do not find any statistically significant variations of their X-ray luminosity functions (XLFs). We also find that the majority of the X-ray sources are associated with star-forming regions, although we do not always identify optical counterparts to the X-ray sources. Especially in the case of M82 we find that the most luminous sources are clustered in the central region of the galaxy. Finally, we present the first results from a study of a sample of nearby star-forming galaxies which form a starburst age sequence: although their XLFs to first order are represented by power-laws with consistent slopes, there is an indication for small variations, suggesting a change of their X-ray binary populations.     

Are Boltzmann plots of hydrogen Balmer lines a tool for identifying a subclass of S1 AGN?

It is becoming clear that we can define two different types of nearby AGN belonging to the Seyfert 1 class (S1), on the basis of the match of the intensities of their Broad Balmer Lines (BBL) with the Boltzmann Plots (BP). These two types of S1 galaxies, that we call BP-S1 and NoBP-S1, are characterized, in first approximation, by Broad Line Regions (BLR) with different structural and physical properties. In this communication, we show that these features can be well pointed out by a multi-wavelength analysis of the continuum and of the broad recombination Hydrogen lines, that we carry out on a sample of objects detected at optical and X-ray frequencies. The investigation is addressed to verify whether BP-S1 are the ideal candidates for the study of the kinematical and structural properties of the BLR, in order to derive reliable estimates of the mass of their central engine and to constrain the properties of their nuclear continuum spectrum.     

Strategies for remote detection of life--DARWIN-IRSI and TPF missions.

Having selected a general definition of a living system, we wonder whether a remote detection of such systems can be made, at least in some cases. Quite fortunately, we find that this seems possible. We describe the present status of missions with this goal.     

A census of high-energy observations of Galactic supernova remnants

We present the first public database of high-energy observations of all known Galactic supernova remnants (SNRs). In Section 1 we introduce the rationale for this work motivated primarily by studying particle acceleration in SNRs, and which aims at bridging the already existing census of Galactic SNRs (primarily made at radio wavelengths) with the ever-growing but diverse observations of these objects at high-energies (in the X-ray and γ$\gamma$-ray regimes). In Section 2 we show how users can browse the database using a dedicated web front–end (http://www.physics.umanitoba.ca/snr/SNRcat). In Section 3 we give some basic statistics about the records we have collected so far, which provides a summary of our current view of Galactic SNRs. Finally, in Section 4, we discuss some possible extensions of this work. We believe that this catalogue will be useful to both observers and theorists, and timely with the synergy in radio/high-energy SNR studies as well as the upcoming new high-energy missions. A feedback form provided on the website will allow users to provide comments or input, thus helping us keep the database up-to-date with the latest observations.     

Planetary Protection and the astrobiological exploration of Mars: Proactive steps in moving forward

Future efforts towards Mars exploration should include a discussion about the effects that the strict application of Planetary Protection policies is having on the astrobiological exploration of Mars, which is resulting in a continued delay in the search for Martian life. As proactive steps in the path forward, here we propose advances in three areas. First, we suggest that a redefinition of Planetary Protection and Special Regions is required for the case of Mars. Particularly, we propose a definition for special places on Mars that we can get to in the next 10–20?years with rovers and landers, where try to address questions regarding whether there is present-day near-surface life on Mars or not, and crucially doing so before the arrival of manned missions. We propose to call those special places “Astrobiology Priority Exploration” regions (APEX regions). Second, we stress the need for the development of robotic tools for the characterization of complex organic compounds as unequivocal signs of life, and particularly new generations of complex organic chemistry and biosignature detection instruments, including advances in DNA sequencing. And third, we advocate for a change from the present generation of SUV-sized landers and rovers to new robotic assets that are much easier to decontaminate such as microlanders: they would be very small with limited sensing capabilities, but there would be many of them available for launch and coordination from an orbiting platform. Implementing these changes will help to move forward with an exploration approach that is much less risky to the potential Mars biosphere, while also being much more scientifically rigorous about the exploration of the “life on Mars” question – a question that needs to be answered both for astrobiological discovery and for learning more definitive lessons on Planetary Protection.     

Solar EUV energy budget of the thermosphere

Using the accumulation of experimental data and theoretical studies conducted on the terrestrial thermosphere since the mid seventies, we have re-evaluated the channels by which solar UV energy is transferred to the atmosphere. As an outcome of this evaluation we have redetermined the solar EUV heating efficiency for the thermosphere and find this to be considerably different from that established in earlier studies. The heating efficiency has strong altitude, solar cycle and diurnal dependencies. The values of this parameter vary from less than 10% to greater than 100%, with peak midday values of 50–55% In recent papers we have presented the results of this new UV heating efficiency determination using a steady state solution of the ionospheric model. In this paper we present the results obtained solving a time dependent model over a diurnal cycle. The time dependent effects are found to be significant, with certain longlived species acting as temporary reservoirs of latent heat that is released to the neutral atmosphere at later times.     

利用栅网控制空间等离子体环境效应模拟中的等离子体参数

通常采用ECR等离子体源产生的等离子体的温度和密度都比较大，通过附加适当目数的栅网，并在栅网上加一定的偏置电位来对等离子体参数，尤其是温度，密度进行调整，满足空间等离子体环境模拟要求，本文利用14目，25目的栅网，对已有的地面实验室空间等离子体环境进行了改进，得到了更加接近空间等离子体参数的一个地面模拟环境。     

Characterization of a novel gravitropic mutant of morning glory, weeping2

In higher plants, gravity is a major environmental cue that governs growth orientation, a phenomenon termed gravitropism. It has been suggested that gravity also affects other aspects of morphogenesis, such as circumnutation and winding movements. Previously, we showed that these aspects of plant growth morphology require amyloplast sedimentation inside gravisensing endodermal cells. However, the molecular mechanism of the graviresponse and its relationship to circumnutation and winding remains obscure. Here, we have characterized a novel shoot gravitropic mutant of morning glory, weeping2 (we2). In the we2 mutant, the gravitropic response of the stem was absent, and hypocotyls exhibited a severely reduced gravitropic response, whereas roots showed normal gravitropism. In agreement with our previous studies, we found that we2 mutant has defects in shoot circumnutation and winding. Histological analysis showed that we2 mutant forms abnormal endodermal cells. We identified a mutation in the morning glory homolog of SHORT-ROOT (PnSHR1) that was genetically linked to the agravitropic phenotype of we2 mutant, and which may underlie the abnormal differentiation of endodermal cells in this plant. These results suggest that the phenotype of we2 mutant is due to a mutation of PnSHR1, and that PnSHR1 regulates gravimorphogenesis, including circumnutation and winding movements, in morning glory.     

机器人机构灵活度研究

首次提出并研究了六自由度机器人机构灵活度的定量计算方法,编制了相应的应用软件,以各种典型关节型机器人为例,在ＳＧＩ工作站上实现了机构灵活度的定量分析计算及其三维图形显示,绘出了工作空间内平行于子午面的任意切面上的机构等灵活度曲线,本研究成果为机器人的性能分析、避障、轨迹规划等研究提供了有力的手段。     

Flows and obstacles in the solar wind

Understanding the physics of the various disturbances in the solar wind is critical to successful forecasts of space weather. The STEREO mission promises to bring us new and deeper understanding of these disturbances. As we stand on the threshold of the first results from this mission, it is appropriate to review what we know about solar wind disturbances. Because of their complementary nature we discuss both the disturbances that arise within the solar wind due to the stream structure and coronal mass ejecta and the disturbances that arise when the solar wind collides with planetary obstacles, such as magnetospheres.     

Chaos and multifractals in the solar wind

By using the false-nearest-neighbours method, we have argued that the deterministic component of solar wind plasma dynamics should be low-dimensional. In fact, the results we have obtained using the method of topological embedding indicate that the behaviour of the solar wind can be approximately described by a low-dimensional chaotic attractor in the inertial manifold, which is a subspace of system phase space. We have also shown that the multifractal spectrum of the solar wind attractor is consistent with that for the multifractal measure of the self-similar generalized weighted Cantor set with two different scaling parameters and one probability measure parameter responsible for nonuniform compression in phase space and multifractality. The values of the parameters fitted also demonstrate that the complex solar wind system could only be weakly non-conservative (small dissipation) and quantify nonlinear dynamics; some parts of the attractor in phase space are visited much more frequently than other parts. In addition, to quantify the multifractality of space plasma intermittent turbulence, we consider that generalized Cantor set also in the context of scaling properties of solar wind turbulence. We investigate the resulting multifractal spectrum of a one-dimensional phenomenological model of turbulence cascade depending on its parameters, especially for asymmetric scaling. In particular, we have shown that intermittent pulses are stronger for the cascade model with two different scaling parameters. Even thought solar wind turbulence appears to be rather space filling, a better agreement with the data is obtained, especially for the negative index of generalized dimensions. Therefore we argue that there is a need to use a two-scale asymmetric cascade model. We hope that this generalized multifractal model will be a useful tool for analysis of intermittent turbulence in space plasmas. We thus believe that fractal analysis of chaotic systems could lead us to a deeper understanding of their nature, and maybe even to predict their seemingly unpredictable behaviour.     

On the station keeping of a solar sail in the elliptic Sun–Earth system

In this work we focus on the dynamics of a solar sail in the Sun–Earth Elliptic Restricted Three-Body Problem with solar radiation pressure. The considered situation is the motion of a sail close to the L₁ point, but displacing the equilibrium point with the sail so that it is possible to have continuous communication with the Earth. In previous works we derived a station keeping strategy for this situation but using the Circular RTBP as a model.     

Spatial variation of the supersonic thermal plasma flow downstream of the termination shock

In this paper we start from the most recently observed fact that the solar wind plasma after passage over the termination shock is still supersonic with a Mach number of about 2. To explain this unexpected phenomenon and to predict the evolution of properties of the downstream plasma flow we here consider a two-fluid proton plasma with pick-up protons as a separate suprathermal, second proton fluid. We then formulate a self-consistent system of hydrodynamical conservation equations coupling the two fluids by dynamical and thermodynamical coupling terms and taking into account the effects of newly incorporated protons due to charge exchange with the H-atoms in the heliosheath. This then allows us to predict that in the most probable case the solar wind protons will become subsonic over a distance of about 30 AU downstream of the shock. As we can also show, it may, however, happen that the plasma mixture later again reconverts to a supersonic signature and has to undergo a second shock before meeting the heliopause.