Aspen Flare System Analyzer在火炬管网设计与分析中的具体应用

火炬气的排放系统设计是一个非常复杂的过程,涉及到各泄放点的背压与管路马赫数的计算。介绍了Aspen Flare System Analyzer模拟软件的特点及应用方法,该软件遵循API的规范要求,通过计算火炬管网中各管段始末点的压力、温度、流速等参数,可有效发现设计中的不合理管径并进行修改。以中东某油田地面工程项目为例,阐述了在工程实际中如何通过该软件进行火炬管网核算。高压火炬管网的核算结果显示,部分安全阀尾管背压和马赫数过大,经软件修改后的尺寸在实际运行中可满足火炬气的排放要求,保证了系统安全。表明了该软件在安全阀的选型和火炬管网的设计工作中的应用价值。

ASPEN FLARE SYSTEM ANALYZER在火炬系统设计中的应用

对Aspen Flare System Analyzer在天然气化工合成氨装置火炬管网设计中的应用进行了研究。首先阐述了化工装置火炬管网设计相关专业名词;其次介绍了Aspen Flare System Analyzer软件在火炬管网中计算方法、建模设计原则及应用范围;最后结合某合成氨装置火炬系统实际案例进行了分析。结果表明:工程师在应用Aspen Flare System Analyzer进行火炬管网设计时可优先根据工程经验预先给定管道尺寸,选择Rating模式计算,能够获得满足生产要求的且更为合理的火炬管网尺寸,同时可以提高火炬管网设计的效率。

Aspen Flare System Analyzer在火炬管网核算中的应用

火炬管网的核算是工厂设计中的一个重要环节,其核算过程十分复杂,涉及多个环节,如排放负荷测量、管网压降测量、泄流装置背压和马赫数测量等。本文简要介绍了Aspen Flare System Analyzer软件的计算模型,并将其应用到一改扩建项目的火炬管网核算,根据软件结果修改了部分火炬管网设计,满足了装置排放气泄放要求,保障了系统的安全运行。

Inverse Calculation and Regularization Process for the Solar Aspect System(SAS) of HXI Payload on ASO-S Spacecraft

For the ASO-S/HXI payload, the accuracy of the flare reconstruction is reliant on important factors such as the alignment of the dual grating and the precise measurement of observation orientation. To guarantee optimal functionality of the instrument throughout its life cycle, the Solar Aspect System (SAS) is imperative to ensure that measurements are accurate and reliable. This is achieved by capturing the target motion and utilizing a physical model-based inversion algorithm. However, the SAS optical system’s inversion model is a typical ill-posed inverse problem due to its optical parameters, which results in small target sampling errors triggering unacceptable shifts in the solution. To enhance inversion accuracy and make it more robust against observation errors, we suggest dividing the inversion operation into two stages based on the SAS spot motion model. First, the as-rigid-aspossible (ARAP) transformation algorithm calculates the relative rotations and an intermediate variable between the substrates. Second, we solve an inversion linear equation for the relative translation of the substrates, the offset of the optical axes, and the observation orientation. To address the ill-posed challenge, the Tikhonov method grounded on the discrepancy criterion and the maximum a posteriori (MAP) method founded on the Bayesian framework are utilized. The simulation results exhibit that the ARAP method achieves a solution with a rotational error of roughly±3 5 (1/2-quantile);both regularization techniques are successful in enhancing the stability of the solution, the variance of error in the MAP method is even smaller—it achieves a translational error of approximately±18μm (1/2-quantile) in comparison to the Tikhonov method’s error of around±24μm (1/2-quantile). Furthermore, the SAS practical application data indicates the method’s usability in this study. Lastly, this paper discusses the intrinsic interconnections between the regularization methods.

A Confined Two-peaked Solar Flare Observed by EAST and SDO

The solar flare is one of the most violent explosions,and can disturb the near-Earth space weather.Except for commonly single-peaked solar flares in soft X-ray,some special flares show intriguing a two-peak feature that is deserved much more attentions.Here,we reported a confined two-peaked solar flare and analyzed the associated eruptions using high-quality observations from Educational Adaptive-optics Solar Telescope and Solar Dynamics Observatory.Before the flare,a magnetic flux rope(MFR)formed through partially tether-cutting reconnection between two sheared arches.The flare occurred after the MFR eruption that was confined by the overlying strong field.Interestingly,a small underlying filament immediately erupted,which was possibly destabilized by the flare ribbon.The successive eruptions were confirmed by the analysis of the emission measure and the reconnection fluxes.Therefore,we suggest that the two peaks of the confined solar flare are corresponding to two episodes of magnetic reconnection during the successive eruptions of the MFR and the underlying filament.

Statistical Study of the Geoeffectivity of Halo Coronal Mass Ejections Associated with X-Class Flares during Solar Cycles 23 and 24

By analysing a long series of data (1996-2019), we show that solar cycle 23 was more marked by violent solar flares and coronal mass ejections (CMEs) compared to solar cycle 24. In particular, the halo coronal mass ejections associated with X-class flares appear to be among the most energetic events in solar activity given the size of the flares, the speed of the CMEs and the intense geomagnetic storms they produce. Out of eighty-six (86) X-class halo CMEs, thirty-seven (37) or 43% are highly geoeffective;twenty-four (24) or approximately 28% are moderately geoeffective and twenty-five (25) or 29% are not geoeffective. Over the two solar cycles (1996 to 2019), 71% of storms were geoeffective and 29% were not. For solar cycle 23, about 78% of storms were geoeffective, while for solar cycle 24, about 56% were geoeffective. For the statistical study based on speed, 85 halo CMEs associated with X-class flares were selected because the CME of 6 December 2006 has no recorded speed value. For both solar cycles, 75.29% of the halo CMEs associated with X-class flares have a speed greater than 1000 km/s. The study showed that 42.18% of halo (X) CMEs with speeds above 1000 km/s could cause intense geomagnetic disturbances. These results show the contribution (in terms of speed) of each class of halo (X) CMEs to the perturbation of the Earth’s magnetic field. Coronal mass ejections then become one of the key indicators of solar activity, especially as they affect the Earth.

A Computation on Velocity Field of the Post-flare Loop System of August 17, 1989

The observational line of sight velocity fields of a large post flare loop(PFL) system on August 17,1989 were derived based on “multi cloud model” (MCM) method from the Hβ spectral data obtained with the two dimensional Multi Waveband Spectra Spectro Helio Graph (MW SSHG) at Yunnan Observatory. In order to explain the fundamental features of the velocity fields observed,an assumption and approximation to be taken into account that the matter within a loop system rises up from the loop foot to the loop top along the loop leg in a helical magnetic line under the combined action of solar gravity, magnetic stress and a gradient of atmospheric pressure in the loop system, and a theoretical velocity field of the loop system was calcuated with the aid of MHD theory. From a comparison of both velocity fields, it is found that the computed velocity field is basically similar with the observed one. It indicates that the assumption and approximation mentioned above are suitable basically.

Observation and Research on the Twisting Characteristics of Flare Loop System

We analyze the evolution of Hβ monochromatic images and Hβ velocity fields of the flare loops system on June 4, 1991. It is the first time to demonstrate directly the dynamic process of the energy storage, transportation and release of the twisting magnetic fields in the flare process.

New Cases of Superflares on Slowly Rotating Solar-type Stars and Large Amplitude Superflares in G-and M-type Main Sequence Stars

In our previous work,we searched for superflares on different types of stars while focusing on G-type dwarfs using entire Kepler data to study statistical properties of the occurrence rate of superflares.Using these new data,as a byproduct,we found 14 cases of superflare detection on 13 slowly rotating Sun-like stars with rotation periods of24.5–44 days.This result supports the earlier conclusion by others that the Sun may possibly undergo a surprise superflare.Moreover,we found 12 and seven new cases of detection of exceptionally large amplitude superflares on six and four main sequence stars of G-and M-type,respectively.No large-amplitude flares were detected in A,F or K main sequence stars.Here we present preliminary analysis of these cases.The superflare detection,i.e.,an estimation of flare energy,is based on a more accurate method compared to previous studies.We fit an exponential decay function to flare light curves and study the relation between e-folding decay time,τ,versus flare amplitude and flare energy.We find that for slowly rotating Sun-like stars,large values ofτcorrespond to small flare energies and small values ofτcorrespond to high flare energies considered.Similarly,τis large for small flare amplitudes andτis small for large amplitudes considered.However,there is no clear relation between these parameters for large amplitude superflares in the main sequence G-and M-type stars,as we could not establish clear functional dependence between the parameters via standard fitting algorithms.

LyαEmission Enhancement Associated with Soft X-Ray Microflares

Lyα(Lyα,1216 A)is the strongest emission line in the solar ultraviolet spectrum.In the present work,we obtained a Lyαenhancement catalog covering flares larger than B1 class from the GOES/EUVS data during 2010-2016.We focused on the 242 B-class events which are less investigated,however,show non-negligible Lyαemission enhancement.We found that on average the Lyαpeak of B-class flares is 0.85%stronger than the background.For the flare energetics,it is found that the weaker the soft X-ray(SXR)flare,the larger the ratio of the radiated energy in Lyαto SXR.Using the RHESSI data and multi-wavelength observations taken by SDO-AIA,we diagnose the thermal and non-thermal properties of several flares.Three case studies show that the coincidence of the Lyαpeak with the SXR time-derivative peak is not a sufficient condition of the nonthermal property of a Lyαmicroflare.The Lyαenhancement in the microflares may be caused by the nonthermal electron beams or/and thermal conduction.However for typeⅢevents,we found that the delay of the Lyαpeak with respect to the SXR peak can be attributed to either the Lyαemission from a filament erupted or the cooling of the thermal plasma in flare loops.Furthermore,interestingly the Lyαemission from filaments can not only occur in the decay phase of the flare,but also in the preflare phase.In this case,the Lyαemission was originated from an erupted filament which probably initiated the flare.

Flare Forecast Model Based on DS-SMOTE and SVM with Optimized Regular Term

The research of flare forecast based on the machine learning algorithm is an important content of space science.In order to improve the reliability of the data-driven model and weaken the impact of imbalanced data set on its forecast performance,we proposes a resampling method suitable for flare forecasting and a Particle Swarm Optimization(PSO)-based Support Vector Machine(SVM)regular term optimization method.Considering the problem of intra-class imbalance and inter-class imbalance in flare samples,we adopt the density clustering method combined with the Synthetic Minority Over-sampling Technique(SMOTE)oversampling method,and performs the interpolation operation based on Euclidean distance on the basis of analyzing the clustering space in the minority class.At the same time,for the problem that the objective function used for strong classification in SVM cannot adapt to the sample noise,In this research,on the basis of adding regularization parameters,the PSO algorithm is used to optimize the hyperparameters,which can maximize the performance of the classifier.Finally,through a comprehensive comparison test,it is proved that the method designed can be well applied to the flare forecast problem,and the effectiveness of the method is proved.

Research Progress on Solar Flare Forecast Methods Based on Data-driven Models

Eruption of solar flares is a complex nonlinear process,and the rays and high-energy particles generated by such an eruption are detrimental to the reliability of space-based or ground-based systems.So far,there are not reliable physical models to accurately account for the flare outburst mechanism,but a lot of data-driven models have been built to study a solar flare and forecast it.In the paper,the status of solar-flare forecasting is reviewed,with emphasis on the machine learning methods and data-processing techniques used in the models.At first,the essential forecast factors strongly relevant to solar flare outbursts,such as classification information of the sunspots and evolution pattern of the magnetic field,are reviewed and analyzed.Subsequently,methods of resampling for data preprocessing are introduced to solve the problems of class imbalance in the solar flare samples.Afterwards,typical model structures adopted for flare forecasting are reviewed from the aspects of the single and fusion models,and the forecast performances of the different models are analyzed.Finally,we herein summarize the current research on solar flare forecasting and outline its development trends.

醋酸阿比特龙治疗去势抵抗性前列腺癌早期出现PSA Flare现象的初步分析

目的分析我院泌尿外科治疗中心确诊为去势抵抗型前列腺癌(CRPC)患者、应用醋酸阿比特龙联合泼尼松治疗早期出现PSA Flare现象后对其前列腺特异抗原(PSA)缓解率的影响及部分基线值对PSA Flare出现概率的影响,为后续治疗提供经验。方法本研究共纳入2015年10月至2017年10月接受醋酸阿比特龙联合泼尼松治疗的CRPC患者共计86例,分析其中用药12周以上的55例有效病例的PSA基线值及其变化。结果 55例患者PSA总体缓解为56.4%,其中27.2%(15/55例)的患者出现了PSA Flare现象;PSA再次下降至基线值水平以下的中位时间为3.1(2~6)月。CRPC患者的年龄、PSA基线值、Gleason评分和患者出现PSA Flare现象无明确关联。结论对于醋酸阿比特龙联合泼尼松治疗CRPC患者来说,PSA Flare现象的发生比较常见,和患者年龄、PSA基线值、Gleason评分并无明确关联。在治疗早期药物暴露时间要足够,部分患者可能≥12周,个别患者PSA Flare持续时间达到24周,因此出现PSA Flare并不能说明疾病进展,对疾病进展的预估要结合影像学等多方面证据。

Observation and Analysis of VLF Nocturnal Multimode Interference Phenomenon based on Waveguide Mode Theory

Very low frequency(VLF)signals are propagated between the ground-ionosphere.Multimode interference will cause the phase to show oscillatory changes with distance while propagating at night,leading to abnormalities in the received VLF signal.This study uses the VLF signal received in Qingdao City,Shandong Province,from the Russian Alpha navigation system to explore the multimode interference problem of VLF signal propagation.The characteristics of the effect of multimode interference phenomena on the phase are analyzed according to the variation of the phase of the VLF signal.However,the phase of VLF signals will also be affected by the X-ray and energetic particles that are released during the eruption of solar flares,therefore the two phenomena are studied in this work.It is concluded that the X-ray will not affect the phase of VLF signals at night,but the energetic particles will affect the phase change,and the influence of energetic particles should be excluded in the study of multimode interference phenomena.Using VLF signals for navigation positioning in degraded or unavailable GPS conditions is of great practical significance for VLF navigation systems as it can avoid the influence of multimode interference and improve positioning accuracy.

现役泄压设备和火炬系统安全核算的系统化方法及应用

介绍了对现役装置的泄压设备和火炬系统的可靠性进行严谨校核的必要性。指出石化企业现役泄压设备(安全阀、爆破片等)和火炬系统存在的主要问题,并对原因进行了分析。基于美国石油学会标准规范API Standard 521—2020的原则和要求,提出了现役泄压设备和火炬系统安全核算的系统化方法,并在两个石化企业取得成功应用。通过系统化核算,发现部分现役安全阀存在流道面积不足、背压不能满足要求以及火炬系统处理能力不能满足实际排放需求等安全隐患,并提出了针对性的整改措施。该方法有效保障了石化企业的安全生产。

焦炉气制甲醇生产火炬系统技术改造及安全防护分析

为进一步提升焦炉气制甲醇生产效率和安全性,以某化工企业甲醇生产线火炬系统的现存问题作为研究案例,基于自动控制原理和方法,利用PLC技术对焦炉气制甲醇生产过程中的火炬系统进行全方位的技术改造,并探究其安全防护措施。预计,本次技术改造将进一步提升该企业火炬系统的运行质量,有助于进一步推动焦炉气制甲醇生产线的稳定高效运行。

气田火炬系统安全运行控制技术研究

某净化厂具有30×10^(8)m^(3)的高含硫天然气(H2S的体积分数为5.55%,有机硫含量362.4mg/m3,CO_(2)的体积分数为6.57%)处理能力。为了保障火炬系统连续长周期安全平稳运行,集中梳理了火炬系统连续运行出现的典型问题,重点从高温热辐射、SO_(2)中毒、高空坠落等方面分析了火炬系统在生产装置不停工检修时的风险,并就火炬系统安全运行从4个方面提出安全对策,旨在保证事故工况时高含硫天然气的安全泄放。

活塞环润滑理论的发展及美国FLARE软件包

1 前言 活塞环的润滑状况一直是人们关心的重要课题,因为发动机约60%的摩擦损失消耗在活塞环与缺套的摩擦上。不仅如此,发动机的寿命也是以这对摩擦副的磨损程度为依据的。因此要想提高发动机的工作性能和延长发动机的使用寿命就必须对这对摩擦副的润滑状况进行深入细致的研究。 50年代末期,专家预测活塞环寿命只有2万km。

基于动态仿真的火炬气回收系统超压保护措施

油气田火炬气回收是碳减排的重要手段,但目前针对火炬气回收系统(FGRS)尤其是超压保护方面还缺乏系统性研究。以文昌9-7海上钻井生产平台为例,采用K-Spice软件搭建了火炬气回收系统动态仿真模型,研究确定火炬气回收系统在不同放空工况下的超压保护措施。结果表明:火炬气回收系统分液罐的压力高高关断(PAHH)设定值应根据连续放空气量变化确定,参照现行规范设定的PAHH值(210 kPa)明显偏高,应调至38.5 kPa,以确保超压值不高于分液罐设计压力又满足平台低压设备的泄放背压要求;应急放空工况下,为确保一级保护和二级保护相互独立,火炬支路快速开关阀(ESD)的开阀时间应小于27 s;火炬支路ESD故障时,为确保应急放空过程中分液罐内压力不超过设计压力,同时考虑爆破膜泄压对上游设备泄放背压的影响,最终选择Z型爆破膜。目前该平台已结合上述关键参数形成了一套完整的火炬气回收方案,预期回收火炬气可达13万立方米/年以上,碳减排效果显著。本研究为火炬气回收系统超压保护措施关键参数确定提供了定量分析手段,为火炬气回收系统的设计提供了参考。

FLARENET在乙烯装置火炬管网设计中的应用

介绍了一种利用模拟软件进行乙烯装置火炬系统设计计算的方法。首先对火炬系统设计中容易混淆的概念进行了澄清,随后对FLARENET模型的建立和计算原则进行了说明。并以天津百万吨乙烯项目的计算结果为例,通过与已建成装置的安全阀型式和火炬总管尺寸进行比较,证明采用该软件可以更加准确的进行安全阀的选型和火炬管网的设计工作。