Vertical wavenumber spectra of atmospheric ozone measured from ozonesonde observations

Vertical profiles of ozone have been measured at balloon altitudes. Our purpose is to examine the character of vertical wavenumber spectra of ozone fluctuations, to assess the possible roles of gravity wave field in ozone fluctuations, and to determine dominant vertical wavelengths of ozone spectra. Vertical wavenumber spectra of 12 ozone fluctuations obtained during June–August 2003 are presented. Results indicate that mean spectral slopes in the wavenumber range from 4.69 × 10⁻⁴ to 2.50 × 10⁻³ cyc/m are about −2.91 in the troposphere and −2.87 in the lower stratosphere, which is close to the slope of −3 predicted by current gravity wave saturation models. The consistency of the observed spectral slopes with the value of −3 predicted by current gravity wave saturation models suggests that the observed ozone fluctuations are due primarily to atmospheric gravity waves. At m = 1/(1000 m) the mean spectral amplitude is over 30 times larger in the lower stratosphere than in the troposphere. Mean vertical wavenumber spectra in area-preserving form reveal dominant vertical wavelengths of ∼2.6 km in the troposphere and ∼2.7 km in the lower stratosphere, which is consistent with the values varying between 1.5 and 3.0 km estimated from the velocity field and temperature field at these heights.     

Ozone reference models for CIRA

The ozone reference model which is to be incorporated in the COSPAR International Reference Atmosphere (CIRA) is described and compared with other measurements of the Earth's ozone distribution. Ozone vertical structure models from approximately 25 to 90 km are provided combining data from five recent satellite experiments (Nimbus-7 LIMS, Nimbus-7 SBUV, AE-2 SAGE, Solar Mesosphere Explorer (SME) UVS, and SME IR). The results include the latest improvements in the SBUV algorithms using the most recent estimates of ozone cross sections. Also, the latest refinements in SME algorithms are incorporated. These algorithm improvements have improved agreement between the satellite data sets. Standard deviations are provided of monthly zonal means, and an estimate of the interannual variability is given. The models based on satallite data compare well with the Krueger and Minzner mid-latitude model incorporated into the U. S. Standard Atmosphere which is based on rocket and balloon measurements. Other comparisons are shown with Umkehr and more recent balloon data. Models are also provided of total columnar ozone reflecting recent improved estimates of ozone cross section. Information is provided on semiannual and annual variations. Other systematic variations including estimates of diurnal variations in the mesosphere will be included in the CIRA document.     

Meteorological variations in the middle clouds of Venus from VEGA balloon in situ measurements

Instruments aboard the gondolas of the two VEGA balloons obtained in situ measurements of pressure, temperature, vertical velocity relative to the balloon, cloud particle backscatter, lightning and the ambient light level. Atmospheric motions at the balloon float altitudes were also determined from Earth-based tracking results. To illustrate the history of the balloon flights and to facilitate comparisons between some of the different observed quantities, measurements of pressure, temperature and backscatter are presented as time series for the entire lifetime of each balloon. Both long and short period variations have been detected. In addition, the environmental entropy encountered by each balloon will be discussed.     

Sodium lidar measurements of mesopause region temperatures at 23° S

A sodium lidar, capable of measuring temperature in the 80–100 km region, has been in operation at São José dos Campos (23° S, 46 W) since March 2007. Good quality data have been obtained for late autumn, winter and spring, but weather conditions make it extremely difficult to make measurements from mid-November to mid- February. We find the temperature structure to be strongly modulated by tides and gravity waves, but average profiles typically show a primary mesopause height close to 100 km with temperatures around 180 K, and a tendency for a secondary minimum of about 185 K to occur close to 90 km. Vertical temperature gradients greater than 50 K/km are sometimes seen even on profiles averaged over several hours. The strongest gradients are always positive and are frequently associated with strong gradients in sodium concentration. On the other hand, we frequently see rapid changes in the temperature profile, suggesting that models and non-local temperature measurements, as made by satellite radiometers, for example, are of little use in applications such as the analysis of gravity wave propagation seen in airglow images.     

VHF radar observation of wave instability and turbulence in the mesosphere

At mesospheric heights, VHF radar measurements reveal strong signal power bursts which have the same period as simultaneously observed short-period velocity oscillations. Both the power bursts and the velocity oscillations occur in layers of maximum vertical wind shear generated by tidal or long-period gravity waves with apparent vertical wavelengths of the order of 10 km. A comparison with similar power bursts measured in the troposphere during a jet stream passage leads to the conclusion that the short-period velocity oscillations are due to a Kelvin-Helmholtz instability. This instability in turn generates superadiabatic lapse rates so that strong turbulence can occur which produces the observed signal power bursts.     

平流层上部负离子成分的直接测量和硫酸离子热化学分析

本文报道了在法国南部(44°N)上空进行的两次气球飞行实验的部分负离子成分探测结果.利用自然负离子谱计算了某些硫酸离子的热化学常数ΔG, ΔH和ΔS.讨论了上升段测量中气球表面放气造成的离子化学污染.     

极区夏季70—100km大气垂直速度扰动功率谱的观测

使用1987年夏季MAC/SINEcampaign期间在挪威北部的Andenes发射的5枚chaff火箭垂直速度数据研究了70—100km高度范围内大气垂直速度扰动垂直波数谱.发现垂直速度垂直波数谱在39×10^-4m^－1处有1个谱缺口.在大于这个谱缺口的垂直波数范围,垂直速度垂直波数谱与饱和谱模式有好的一致.在小于这个谱缺口的垂直波数范围,垂直速度垂直波数谱有谱斜率－1.87和谱振幅比饱和谱振幅低1个量级,认为在低波数,除重力波外的其它地球物理过程存在于垂直速度扰动中.     

Measuring atmospheric density using GPS–LEO tracking data

We present a method to estimate the total neutral atmospheric density from precise orbit determination of Low Earth Orbit (LEO) satellites. We derive the total atmospheric density by determining the drag force acting on the LEOs through centimeter-level reduced-dynamic precise orbit determination (POD) using onboard Global Positioning System (GPS) tracking data. The precision of the estimated drag accelerations is assessed using various metrics, including differences between estimated along-track accelerations from consecutive 30-h POD solutions which overlap by 6 h, comparison of the resulting accelerations with accelerometer measurements, and comparison against an existing atmospheric density model, DTM-2000. We apply the method to GPS tracking data from CHAMP, GRACE, SAC-C, Jason-2, TerraSAR-X and COSMIC satellites, spanning 12 years (2001–2012) and covering orbital heights from 400 km to 1300 km. Errors in the estimates, including those introduced by deficiencies in other modeled forces (such as solar radiation pressure and Earth radiation pressure), are evaluated and the signal and noise levels for each satellite are analyzed. The estimated density data from CHAMP, GRACE, SAC-C and TerraSAR-X are identified as having high signal and low noise levels. These data all have high correlations with anominal atmospheric density model and show common features in relative residuals with respect to the nominal model in related parameter space. On the contrary, the estimated density data from COSMIC and Jason-2 show errors larger than the actual signal at corresponding altitudes thus having little practical value for this study. The results demonstrate that this method is applicable to data from a variety of missions and can provide useful total neutral density measurements for atmospheric study up to altitude as high as 715 km, with precision and resolution between those derived from traditional special orbital perturbation analysis and those obtained from onboard accelerometers.     

Performance of GPS-based accelerometry: A simulation experiment

Recent studies have shown that with the availability of high-quality CHAMP and GRACE gravity field models, it is feasible to determine accurate non-gravitational accelerations for low Earth orbiting satellites indirectly from precise GPS satellite-to-satellite observations. Possible applications of this so-called GPS-based accelerometry approach consist of accelerometer calibration and atmospheric density and wind computations. With the growing number of high-quality space-borne GPS receivers, this method could be applied to a large range of satellites. In this paper an extensive simulation study has been carried out, based on real accelerometer data from the GRACE mission, in order to determine the optimal processing strategy and the resulting accuracy of the estimated non-gravitational accelerations. It is shown that the optimal processing strategy consists of a piecewise linear parameterization of the estimated empirical accelerations, together with short 6-h orbit arcs. The GPS-based accelerometry approach makes use of triple-differenced GPS observations and the impact of considering the correlated observation noise was found to be marginal in the presence of other error sources such as GPS ephemeris errors. Using a priori non-gravitational force models improves the recovery of low temporal resolution accelerations, except during huge geomagnetic storms. With this strategy, non-gravitational accelerations can be recovered during high solar activity with an accuracy of better than 10% of the total signal in along-track direction and around 25–40% in cross-track direction, at time resolutions of around 8–20 min. During solar minimum conditions, the relative recovery error will increase to approximately 50% in along-track direction and around 60–70% in cross-track direction, due to the reduced atmospheric drag signal. Unfortunately, GPS-based accelerometry is hardly sensitive in the radial direction.     

Vertical density and temperature structure over Northern Europe

During the Energy Budget Campaign, several profiles of the density and temperature of the upper atmosphere were obtained. The measurements were made using rocket-borne instrumentation launched from ESRANGE, Sweden and Andoya Rocket Range, Norway during November and December, 1980. The techniques included meteorological temperature sondes, passive falling spheres, accelerometer instrumented falling spheres, density gauges, mass spectrometers and infrared emission experiments. The instruments provided data within the altitude range from 20 km to 150 km. The measurements were made during periods which have been grouped into three categories by level of geomagnetic activity. Analysis has been made to compare the results and to examine the oscillations and fluctuations in the vertical profiles for scales ranging between hundreds of meters and tens of kilometers. Most of the features observed fit qualitatively within the range expected for internal gravity waves. The geomagnetic storm conditions may be associated with enhanced wave activity and heating observed in the lower thermosphere.     

Mapping the earth's magnetic and gravity fields from space: Current status and future prospects

Orbital potential field measurements are sensitive to regional variations in earth density and magnetization that occur over scales of a few hundred kilometers or greater. Global field models currently available are able to distinguish gravity variations of ±5 milligal over distances of ～1,000 km and magnetic variations of ±6 gamma over distances of ～300 km at the earth's surface. Regional variations in field strength have been detected in orbital measurements that are not apparent in higher resolution, low altitude surveys. NASA is presently studying a spacecraft mission known as GRAVSAT/MAGSAT, which would be the first satellite mission to perform a simultaneous survey of the earth's gravity and magnetic fields at low orbital altitudes. GRAVSAT/MAGSAT has been proposed for launch during the latter nineteen-eighties, and it would measure gravity field strength to an accuracy of 1 milligal and magnetic field strength to an accuracy of 2 gamma (scalar)/5 gamma (vector components) over a distance of roughly 100 km. Even greater improvements in the accuracy and spatial resolution of orbital surveys are anticipated during the nineteen-nineties with the development of potential field gradiometers and a tethered satellite system that can be deployed from the Space Shuttle to altitudes of 120 km above the earth's surface.     

Estimates of convective heat fluxes and gravity wave amplitudes in the Venus middle cloud layer from VEGA balloon measurements

Atmospheric temperatures and vertical velocities obtained from the VEGA balloon measurements indicate that the dynamical heat flux is upward and has an amplitude that ranges from 0 to 360 W m⁻² in the middle cloud region. The static stability is positive and ranges from 0 to 2.0 K km⁻¹. Time series analysis of these results indicates that convection is the principal mechanism for generating the large vertical motions. Gravity waves were also detected at these levels and account for about 15% of the covariance between temperature and vertical velocity.     

80-100km高度范围高分辨率大气水平速度扰动谱

使用1989/1990年冬季在DYANA试验中从5枚Chaff火箭测量获得的高分辨率水平速度数据,讨论80-100km高度范围内水平速度垂直波数谱与饱和重力波谱的一致性,并决定特征垂直尺度.     

International comparison of satellite winds — An update

Winds obtained from geostationary satellites are compared with each other and with rawinsondes. These comparisons serve as a periodic quality check of satellite cloud motions (or winds) set up by the CGMS (Coordination for Geostationary Meteorological Satellites). Differences are taken between colocated cloud motions observed by adjacent satellites in areas of overlapping coverage (Type 1) and between colocated rawinsondes and cloud motions within the field of view of each individual satellite (Type 2).Among colocated satellite winds (Type 1) RMS vector difference of high clouds rarely exceed 10 mps and of low clouds, 6 mps. But, among colocated cloud and balloon vectors (Type 2), RMS vector differences are large. At high levels, differences range from 12 to 40 mps for GMS (Geostationary Meteorological Satellite) winds and from 10 to 18 mps for GOES (Geostationary Operational Environmental Satellite) winds. The greater disagreement of satellite winds with rawinsonde winds than with each other is attributed in large part to error in the assignment of cloud height especially in the presence of strong vertical shear and to a lesser extent on time differences between cloud and balloon measurements. Both Type 1 and 2 comparisons suffer from separations in distance (tolerated for purposes of establishing “colocation”) between cloud and balloon in the presence of strong horizontal shear. The discrepancy existing between GMS and GOES differences with rawinsondes is attributed primarily to differing techniques of height assignment.At low levels satellite winds departed from balloon winds by a RMS vector difference of about 6 to 9 mps which approached or exceeded the mean wind speed itself. This problem is attributed chiefly to the uncertainty of wind levels controlling the motion of the various low cloud types.     

利用COSMIC数据构建的全球垂直TEC图的验证研究

在日固坐标系(地磁纬度和地方时)下, 累积地方时过去24h的COSMIC(Constellation Observing System for Meteorology Ionosphere andClimate)观测资料, 通过对110$sim$750km高度范围内的电子密度进行数值积分得到各掩星点的垂直TEC值, 进而利用Kriging方法插值产生近实时的全球地方时MAGLat2.5°×2h的COSMIC TEC图. 利用2008年1月1日至2010年6月30日共30个月的COSMIC数据, 逐日构建COSMICTEC图, 将其与全球导航卫星系统服务组织(International GNSS Service,IGS)发布的全球电离层TEC图(Global Ionospheric Maps, GIMs)以及OSTM/JASON-2卫星高度计观测值分别进行比对,证明利用COSMIC掩星资料构建全球电离层垂直TEC图是可行的.     

武汉上空中层顶大气重力波活动的钠层荧光激光雷达观测研究

从中国科学院武汉物理与数学研究所钠荧光激光雷达自1999年至今的观测数据中选取了分布于全年26天的数据进行重力波活动的分析研究.统计结果表明,武汉中层顶区的重力波活动非常频繁:26天总观测时间累计约为185.5 h,总共观测到124个重力波活动,平均发生频度为每小时0.7个波,且波的出现频度与地方时有一定关系.这些波的垂直波长主要分布在3-7km,垂直相速主要位于0.1-0.5 m/s.与国外报道的结果相比较,波长数值与分布较为一致,但相速明显较低.武汉中层顶区重力波活动的另一特点是多波过程很频繁,多、单波过程的出现比例约为3:2.利用钠层相对密度扰动时空图方法,给出了武汉中层顶区重力波传播和破碎现象的典型结果.还利用单色波模型对部分钠层数据进行了单色波相关参数的提取.     

冬季中层顶区域重力波谱特性

使用DYANA试验期间19枚(Chaff火箭在81-105km高度范围测量的高分辨率水平速度数据,研究标量水平速度垂直波数谱在冬季的谱特性.分析结果显示冬季平均垂直波数谱有-3.02的谱斜率,这与各种饱和理论预测的-3谱斜率很一致,提供了饱和重力波谱在冬季的观测证据.与各种饱和理论比较表明,这个冬季谱的谱振幅与线性饱和理论预测的谱振幅完全一致,但是总是小于非线性饱和理论预期的、激光雷达测量的谱振幅.这个冬季谱与最近得到的夏季饱和重力波谱一道,共同表明我们的观测结果支持了线性饱和理论,而不管季节,地理位置和高度范围的不同.由这个冬季谱估计的盛行垂直波长为15km,它比夏季的12.8km盛行垂直波长稍大.     

Middle atmosphere models and comparison with shuttle reentry density data

Several middle atmosphere models will be reviewed, including a new set of models produced by Groves in 1985. The latter models are based on rocket and rawinsonde in situ measurements and satellite remote sounding temperature data. The models are compared with measurements made with instruments on board U. S. Shuttles during their reentry. Very useful atmospheric density data have been obtained in the altitude region from 50 to 80 km. The measurements are unique in that they are made by a vehicle travelling almost horizontally through the atmosphere at a velocity of 6 to 7 km/sec. This results in measurements along a path of approximately 8,000 km in a time interval of about 20 minutes. The results show some unique features.     

Importance of electric field measurement over low latitudes at stratospheric heights by balloons

The vertical field in the stratosphere around 35 km is predominantly of atmospheric origin whereas the horizontal electric field at these altitude is mainly of ionospheric origin. The electrical coupling between ionosphere and atmosphere is not known for low latitudes. Balloon borne electric field measurements are planned from Hyderabad, India (geographic latitude 17.5° N) to understand this coupling. Measurement of stratospheric electric fields are also important from the point of view of the sun-weather relationship. It si suggested that the balloon borne electric field measurements are important to understand the electrodynamics of the middle atmosphere.     

北京上空高分辨率气球探空观测的温度垂直波数谱

使用分辨率为10 m的温度剖面检查2.90～8.01 km和14.65～19.76 km高度范围内归一化温度扰动谱的谱特性,并且将它们与模式谱比较.结果表明,在波数9.8×10-4～2.5×10-2m-1范围内,对流层的垂直波数谱有约-1.9的平均谱斜率;低平流层的垂直波数谱有约-2.2的平均谱斜率.这两个平均谱斜率大大偏离了目前饱和谱模式和普适大气谱模式表示的-3.0和-2.4谱斜率,并且认为是目前气球测量中曾经观测到的最平谱斜率.在波数9.8×10-4～2.5×10-2m-1范围内,对流层和低平流层的平均谱振幅比饱和谱模式的谱振幅分别大24倍和5倍,这也与饱和谱模式以及目前文献中的观测结果有很大不同.这些较大平均谱振幅与最平的平均谱斜率一道共同表明,观测的温度谱并不遵循目前的饱和谱模式和普适大气谱模式.