电热破膜激波管及其PLIF测量系统的研制

探讨了用Nd:YAG脉冲激光器作为泵浦光源对激波管内瞬态非定常流场进行平面激光诱导荧光(Planar laser induced fluorescence,PLIF)测量的时序同步问题.由于该激光器需要预热以获得稳定的倍频输出,作者研制了低压大电流的电热破膜装置,实现对激波产生时机的控制.在大尺寸矩形截面的激波管上搭建了PLIF测量平台,并在此平台上进行了丙酮示踪流场显示和氢氧基分布测量.     

平面激光诱导荧光显示火焰中OH的分布图像

用平面激光诱导荧光技术测量了平面火焰炉、原子气化炉和超声速燃烧室的单脉冲激光诱导OH荧光。由平面荧光图可得到氢氧基相对浓度分布和它的厚度。由超声速燃烧室的OH荧光测量 ,可以看出不同时间OH分布的差别。氢氧基的PLIF图像是研究火焰结构和流场的有力工具。     

The hydroxyl radical as an indicator of SEP fluxes in the high-latitude terrestrial atmosphere

The low background values at nighttime of the mesospheric hydroxyl (OH) radical make it easier to single out the atmospheric response to the external solar forcing in Polar Regions. Because of the short lifetime of HO_x, it is possible to follow the trails of Solar Energetic Particle (SEP) events in the terrestrial atmosphere, as shown by Storini and Damiani (2008). The sensitivity of this indicator makes discernible not only extreme particle events with a flux peak of several thousand pfu [1 pfu = 1 particle/(cm² s sr)] at energies >10 MeV, but also those with lower flux up to about 300 pfu. Using data from the Microwave Limb Sounder (MLS) on board the EOS AURA satellite, we examined the correlation of OH abundance vs. solar proton flux for almost all the identified SEP events spanning from November 2004 to December 2006 (later on no more SEP events occurred during Solar Cycle no. 23). The channels at energies greater than 5 MeV and 10 MeV showed the best correlation values (r ∼ 0.90–0.95) at altitudes around 65–75 km whereas, as expected, the most energetic channels were most highly correlated at lower altitudes. Therefore, it is reasonably possible to estimate the solar proton flux from values of mesospheric OH (and viceversa) and it could be useful in studying periods with gaps in the records of solar particles.     

3D Imaging of the OH mesospheric emissive layer

A new and original stereo imaging method is introduced to measure the altitude of the OH nightglow layer and provide a 3D perspective map of the altitude of the layer centroid. Near-IR photographs of the OH layer are taken at two sites separated by a 645 km distance. Each photograph is processed in order to provide a satellite view of the layer. When superposed, the two views present a common diamond-shaped area. Pairs of matched points that correspond to a physical emissive point in the common area are identified in calculating a normalized cross-correlation coefficient (NCC). This method is suitable for obtaining 3D representations in the case of low-contrast objects. An observational campaign was conducted in July 2006 in Peru. The images were taken simultaneously at Cerro Cosmos (12°09′08.2″ S, 75°33′49.3″ W, altitude 4630 m) close to Huancayo and Cerro Verde Tellolo (16°33′17.6″ S, 71°39′59.4″ W, altitude 2272 m) close to Arequipa. 3D maps of the layer surface were retrieved and compared with pseudo-relief intensity maps of the same region. The mean altitude of the emission barycenter is located at 86.3 km on July 26. Comparable relief wavy features appear in the 3D and intensity maps. It is shown that the vertical amplitude of the wave system varies as exp (Δz/2H) within the altitude range Δz = 83.5–88.0 km, H being the scale height. The oscillatory kinetic energy at the altitude of the OH layer is comprised between 3 × 10⁻⁴ and 5.4 × 10⁻⁴ J/m³, which is 2–3 times smaller than the values derived from partial radio wave at 52°N latitude.     

基于OH-PLIF技术的环形燃烧室预混火焰结构实验

针对微型燃气轮机环形燃烧室中的燃烧特性,利用平面激光诱导荧光(PLIF)技术,对环形燃烧室内甲烷/空气预混湍流多束火焰燃烧开展实验研究,得到OH自由基物质的量浓度分布,并研究雷诺数和当量比对火焰结构特征参数的影响。结果表明:OH自由基浓度分布呈现环形结构,并有火焰托举和分叉现象,OH-PLIF瞬时和平均图像揭示了火焰具有湍流和层流预混结构共同特征。火焰结构特征参数的定量分析表明,雷诺数升高,拉伸火焰预混锥形结构,促进射流之间相互作用;康达效应使内焰向内壁面弯曲,火焰张角增大;适当调节预混火焰的当量比,有利于火焰结构的稳定。      

多孔镁基板上纳米厚度Mg(OH)_2层片的常压水热合成

利用开放式常压水热合成工艺在烧结多孔镁基板表面制备了纳米厚度的氢氧化镁(Mg(OH)2)层片。采用扫描电子显微镜(SEM)和X射线衍射分析(XRD)研究了水热处理时间对Mg(OH)2形态的影响,并讨论了多孔镁基板表面纳米厚度Mg(OH)2层片的生成机理。实验结果表明,多孔镁基板中相邻镁颗粒之间的孔隙处是Mg(OH)2层片的优先形成区域,通过超声处理可以使基板上的Mg(OH)2层片脱落。制备的Mg(OH)2样品在123℃的饱和水蒸气中的吸水率在较长时间内会逐步增加。     

Chemical heating rates derived from SCIAMACHY vibrationally excited OH limb emission spectra

The SCIAMACHY instrument on board Envisat is able to measure nearly all vibrational transitions of mesospheric hydroxyl – from the ultraviolet to the near infrared spectral region.

In this paper, we analyze SCIAMACHY limb emission data in the 1000–1750 nm spectral region by means of a new vibrational non-LTE model of OH. Several hydroxyl hotbands are identified. Vibrational non-LTE model calculations applying different collisional relaxation models are able to reproduce the measured spectra. Best agreement between model calculations and measured spectra is obtained, if a combination of multiquantum and step ladder single-quantum relaxation model is applied. Emissions from the OH(v = 9) vibrational state are used to derive chemical heating rates from the SCIAMACHY spectra. Instantaneous heating rates are in the order of 10 K/day.     

Gravity wave mixing effects on the OH*-layer

Based on an advanced numerical model for excited hydroxyl (OH*) we simulate the effects of gravity waves (GWs) on the OH*-layer in the upper mesosphere. The OH* model takes into account (1) production by the reaction of atomic hydrogen (H) with ozone (O₃), (2) deactivation by atomic oxygen (O), molecular oxygen (O₂), and molecular nitrogen (N₂), (3) spontaneous emission, and (4) loss due to chemical reaction with O. This OH* model is part of a chemistry-transport model (CTM) which is driven by the high-resolution dynamics from the KMCM (Kühlungsborn Mechanistic general Circulation Model) which simulates mid-frequency GWs and their effects on the mean flow in the MLT explicitly. We find that the maximum number density and the height of the OH*-layer peak are strongly determined by the distribution of atomic oxygen and by the temperature. As a results, there are two ways how GWs influence the OH*-layer: (1) through the instantaneous modulation by O and T on short time scales (a few hours), and (2) through vertical mixing of O (days to weeks). The instantaneous variations of the OH*-layer peak altitude due to GWs amount to 5–10 km. Such variations would introduce significant biases in the GW parameters derived from airglow when assuming a constant pressure level of the emission height. Performing a sensitivity experiment we find that on average, the vertical mixing by GWs moves the OH*-layer down by ~2 to 7 km and increases its number density by more than 50%. This effect is strongest at middle and high latitudes during winter where secondary GWs generated in the stratopause region account for large GW amplitudes.     

雾化激波管研制和煤油点火延时测量

为测量雾化煤油点火延时和得到火焰自发辐射光强分布,研制了雾化激波管和燃料雾化、进气系统。采用“管外预混”思想形成煤油气溶胶,通过连续进气和抽吸方法使气溶胶均匀分布,未出现明显的液滴沉降和壁面吸附。当点火温度为1000K,缝合接触面运行的实验时间大于10ms。由压电传感器PCB和光电倍增管PMT测量指定点压力、OH基光强时间曲线。利用Mie散射测量煤油气溶胶散射光分布,采用ICCD拍摄自点火发射光强。结果表明：该雾化系统可形成粒径为2～5μm煤油气溶胶。当压力为0．1MPa、温度为1300K～1700K,测得化学计量比≠=1．0煤油气溶胶点火延时τig为0．07—6ms,In（τig）和10000／τig近似呈线性关系。与气态煤油相比,该文高温点火延时和已有文献数据接近,但低温点火延时偏大,表明了低温下煤油点火的两相效应。     

Investigation of infrasound signatures from microbaroms using OH airglow and ground-based microbarometers

In the frame of the European H2020 project ARISE, a short wave infrared (SWIR) InGaAs camera has been operated at the Haute-Provence Observatory, during a night that corresponds to the peak of Geminid meteor shower to investigate infrasound associated with meteor arrivals. This camera allows continuous observations during clear-sky nighttime of the OH airglow layer centered at 87 km. These observations were collocated with Rayleigh lidar measurements providing vertical temperature profiles from the lower stratosphere to the altitude of the OH layer around the mesopause. Spectral analysis of OH images did not allow to detect infrasound associated with meteor trails, however it reveals a peak corresponding to infrasound signals in the frequency band of those produced by ocean swell. Infrasound wave activity observed from ground-based microbarometers as well as the OH camera, appear to be modified with the presence of a temperature inversion described by Rayleigh lidar. Indeed, there is a difference in energy related to infrasonic activity between the first part of the night during the temperature inversion and after the inversion.