Stratospheric profiles of HCl and CH4 at 32°N obtained on PROJECT STRATOPROBE from 1978 to 1985

The most recent in the series of STRATOPROBE balloon flights were conducted in the Spring of 1985 from the National Scientific Balloon Facility in Texas. Altitude distributions of HCl and CH₄ were derived and compared with our results from flights in previous years. The HCl and CH₄ column integrated amounts show a trend towards higher concentrations, not inconsistent with other measurements and model calculations. The CH₄ was determined from emission spectra using a scanning radiometer as well as from absorption lines in the HCl spectral region recorded with the interferometer. There is good agreement between the two techniques and with a model simulation.     

Vertical profiles of source gases at tropical latitudes

A first ISRO-DFVLR collaborative balloon flight of the MPAE cryogenic sampler was conducted at Hyderabad, India (17.5°N), on March 27 1985, and 15 air samples were collected between 10 and 35 km altitude. Vertical profiles of source gases analysed from these samples, such as CCl₃F, CCl₂F₂, CBrClF₂, and CH₄ are presented. Due to tropical upwelling, mixing ratios of source gases decrease less rapidly with altitude than at mid-latitudes.     

Mass spectrometry in the stratosphere

During the last few years a gas expansion system, combined with a mass spectrometer has been developed and successfully flown in the stratosphere. Neutral gas particles are formed into a molecular beam which traverses the ion source of the mass spectrometer without wall interactions. Vertical profiles of constituents such as H₂O, CO₂ and O₃ have been measured in the altitude range of 20 to 40 km during balloon descents. Isotopes of major atmospheric gases (N₂, O₂, Ar) provided in-flight calibration standards.Before each flight the mass spectrometer system was calibrated in the laboratory for many gases of interest, including ozone. Mixing ratios of ozone determined from recent flights have accuracies of better than 5%. The sensitivity of the system was sufficiently high to detect, in addition, the heavy isotope of ozone at mass 50. A pronounced enhancement of heavy ozone in the upper stratosphere has been found. The mass spectrometer system provides the unique opportunity to perform in the stratospherein-situ measurements combined with isotopic studies.     

Measurement of stratospheric trace constituent distributions from balloon-borne far infrared observations

Far infrared limb thermal emission spectra obtained from balloon borne measurements made as a part of the Balloon Intercomparison Campaign (BIC) have been analyzed for retrieval of stratospheric trace constituent distributions. The measurements were made with a high resolution Michelson Interferometer and covered the 15–180 cm⁻¹ spectral range with an unapodized spectral resolution of 0.0033 cm⁻¹. The retrieved vertical profiles of O₃, H₂O, HDO, HCN, CO and isotopes of O₃ are presented. The results are compared with the BIC measurements for O₃ and H₂O made from the same balloon gondola and with other published data. A comparison of the simultaneously retrieved profiles for several gases with the published data shows good agreement and indicates the validity of the far infrared data, the retrieval techniques and the accuracy of the inferred profiles.     

H2O concentration in the middle atmosphere: Processing of LIMS radiance measurements with a research algorithm

Transmittance functions as well as inversion algorithms have been developed for deriving H₂O profiles from radiometer measurements. These computer programs have been applied to evaluate own stratospheric balloon occultation measurements and LIMS (Limb Infrared Monitor of the Stratosphere) radiance measurements in the H₂O channel. The results are compared with the H₂O profiles in the LIMS data archive. The differences between corresponding H₂O profiles are discussed in dependence of altitude and latitude.     

Solar UV and ozone balloon measurements

Absolute solar UV spectra were obtained with a $\text{1}\text{4}$m spectrometer on a balloon flight from Palestine, Texas on September 23, 1981. This balloon reached a float altitude of 39 km at solar noon. The ozone density profiles derived from these spectra are discussed. The measurements are compared with data obtained from the same calibrated instrument flown in 1976 at solar minimum.     

Detection of solar neutrons on a long duration balloon flight

The observation of large solar flares on high altitude balloons requires long duration balloon flights because large flares are infrequent and cannot be predicted with enough reliability and lead time to allow a conventional balloon to be launched and reach altitude before the flare occurs. With the many weeks at float altitude expected for a long duration flight, the probability of “catching” a large flare during solar maximum becomes reasonably high and the study of phenomena which heretofore have required a satellite become accessible to a balloon platform. One example of this type of experiment is the observation of neutrons produced by the interaction of flare accelerated nucleons with the solar atmosphere. Because the neutrons are produced immediately by the flare accelerated particles and are unaffected by their transmission through the upper solar atmosphere and the intervening magnetic fields, their observation at 1 A.U. will provide direct information on the flare acceleration process. Specifically, a measurement of the neutron energy and time spectra will yield the energy spectrum of the charged nucleons in the interval 50 to 500 MeV/amu, the charged particle anisotropy, the height of the acceleration region for limb flares, and information on the two-stage acceleration process. Because the γ-ray spectrum is also sensitive to these factors, a combined neutron and γ-ray measurement will provide a much more stringent test of flare models than either done separately. CWRU and the University of Melbourne have designed the EOSCOR (Extended Observation of Solar and Cosmic Radiation) detector to have the necessary sensitivity to detect neutrons from a flare 0.1 the size of the 4 Aug. 1972 event and to be compatible with the constraints of the long duration balloon system. The detector has been test flown on short duration balloon flights and calibrated at E_n = 38, 58, and 118 MeV. It is planned to launch it on a long duration balloon flight from Australia in December 1982 when simultaneous γ-ray observations will be possible with the SMM and/or HINTORI satellites.     

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.      

Development overview of the revised NASA Ultra Long Duration Balloon

The desire for longer duration stratospheric flights at constant float altitudes for heavy payloads has been the focus of the development of the National Aeronautics and Space Administration’s (NASA) Ultra Long Duration Balloon (ULDB) effort. Recent efforts have focused on ground testing and analysis to understand the previously observed issue of balloon deployment. A revised approach to the pumpkin balloon design has been tested through ground testing of model balloons and through two test flights. The design approach does not require foreshortening, and will significantly reduce the balloon handling during manufacture reducing the chances of inducing damage to the envelope. Successful ground testing of model balloons lead to the fabrication and test flight of a ∼176,000 m³ (∼6.2 MCF – Million Cubic Foot) balloon. Pre-flight analytical predictions predicted that the proposed flight balloon design to be stable and should fully deploy. This paper provides an overview of this first test flight of the revised Ultra Long Duration Balloon design which was a short domestic test flight from Ft. Sumner, NM, USA. This balloon fully deployed, but developed a leak under pressurization. After an extensive investigation to the cause of the leak, a second test flight balloon was fabricated. This ∼176,000 m³ (∼6.2 MCF) balloon was flown from Kiruna, Sweden in June of 2006. Flight results for both test flights, including flight performance are presented.     

Measurements of upper atmosphere wind and temperature from meteorological rocket experiments during winter 1979

This institute conducted a series of meteorological rocket experiments for the upper-atmospheric sounding in the winter of 1979. Within the overlap altitude range with balloon flights, a comparison of the results with the standard radiosonde data indicated that the rocket-borne system was reliable. The measurements from foru rocket flights for the region between 20 and 30 km showed a degree of compatibility to each other while those for above 30 km differed considerably from one another. At low latitude, the temperature profiles in the winter stratosphere in general showed a reasonably good agreement with the U.S. Standard Atmospheric Supplements, 1966 (USSAS 66). A temperature of 2–24°C lower than the USSAS 66, however, was recorded in the lower mesosphere. Above 30 km the maximum diurnal variation in temperature was 9°C or so. In the winter, the wind profile showed the westerlies and the maximum wind velocity of 92.1 Msec^?1 was obtained from these experiments at the height of 60 km.     

Development of balloon technology in China

The first stage in the development of the Chinese scientific balloon facility, commenced in 1979, has been completed successfully. The targets of the second stage, started in 1985 are: increasing balloon volume up to 4×10⁵M³ and payload carrying capacity 1000–1500 kg.; long duration flights from Beijing to the Gobi region in North west China; developing a new telemetry and telecommand system.In this paper we present the recent progress in China on balloon materials, balloon design and manufacture procedures, launch and recovery techniques, telemetry and telecommand facilities etc.     

SCIAMACHY limb measurements of NO2, BrO and OClO. Retrieval of vertical profiles: Algorithm,first results,sensitivity and comparison studies

The Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) measures scattered sun light also in limb viewing mode (i.e. tangential to Earth’s surface and its atmosphere), which allows determining vertical profiles of atmospheric trace gases. First results on the retrieval of NO₂, BrO and OClO profiles from the SCIAMACHY Limb measurements are presented and compared to independent satellite and balloon borne observations.     

Scientific ballooning in Japan

Activities in scientific ballooning in Japan during 1998–1999 are reported. The total number of scientific balloons flown in Japan in 1998 and 1999 was sixteen, eight flights in each year. The scientific objectives were observations of high energy cosmic electrons, air samplings at various altitudes, monitoring of atmospheric ozone density, Galactic infrared observations, and test flights of new type balloons. Balloon expeditions were conducted in Antarctica by the National Institute of Polar Research, in Russia, in Canada and in India in collaboration with foreign countries' institutes to investigate cosmic rays, Galactic infrared radiation, and Earth's atmosphere. There were three flights in Antarctica, four flights in Russia, three flights in Canada and two flights in India. Four test balloons were flown for balloon technology, which included pumpkin-type super-pressure balloon and a balloon made with ultra-thin polyethylene film of 3.4 μm thickness.     

Atomic oxygen concentrations in the lower auroral thermosphere

Atomic oxygen concentrations derived from the nightglow components of O₂(b¹Σ_g⁺ ? X³Σ_g^?) (0-0) Atmospheric Band emission profiles obtained during two rocket-borne photometer measurements of aurora are presented. The peak atomic oxygen concentrations of 2–3 × 10¹¹ cm^?3 are in better agreement with those of the MSIS-83 model than the CIRA 1972 mean reference atmosphere, although the shapes of the two derived profiles differ considerably from that of MSIS-83. The derived concentrations do not contradict the suggestion made by some investigators that the atomic oxygen concentrations in the auroral zone are depleted relative to their mid-latitude values.     

Simultaneous observations of Pc 1 micropulsation activity and stratospheric electrodynamic perturbations on 27 January 2003

The 2nd Polar Patrol Balloon campaign (2nd-PPB) was carried out at Syowa Station in Antarctica during 2002–2003. Identical stratospheric balloon payloads were launched as close together in time as allowed by weather conditions to constitute a cluster of balloons during their flights. A very pronounced negative ion conductivity enhancement was observed at 32 km in the stratosphere below the auroral zone on 27 January 2003 from 1500 to 2200 UT. During this event, the conductivity doubled for an interval of about 7 h. This perturbation was associated with an extensive Pc 1 or Pi 1 wave event that was observed by several Antarctic ground stations, balloon PPB 10, and the Polar spacecraft. No appreciable X-ray precipitation was observed in association with this event, which would point to >60 Mev proton precipitation as a possible magnetosphere–stratosphere coupling mechanism responsible for the conductivity enhancement. Such precipitation is consistent with the wave data. During the latter half of the event, E_z was briefly positive. There was a tropospheric Southern Ocean storm system underneath the balloon during this interval. If the event was associated with this storm system and not energetic proton precipitation, the observations imply an electrified Southern Ocean storm and major perturbations in stratospheric conductivity driven by a tropospheric disturbance. This event represents a poorly understood source for global circuit current. Precipitating energetic proton data from Akebono and NOAA POES spacecraft show significant >16 MeV precipitation was occurring at the location of PPB 8 but not PPB 10, suggesting that proton precipitation was, in fact, the responsible coupling mechanism.     

Comparing topside and bottomside-measured characteristics of the F2 layer peak

The ionospheric characteristics of the F2 layer peak have been measured with ionosondes from the ground or with satellites from space. The most common characteristics are the F2-peak density NmF2 and peak height hmF2. In addition to these two parameters this paper studies the F2-peak scale height. Comparing the median values of hmF2 and NmF2 obtained from topside and bottomside sounding shows good agreement in general. The Chapman scale height values for the F2 layer peak derived from topside profiles, H_m,top, are generally several times larger than H_m,bot derived from bottomside profiles.     

Reconstruction of topside density profile by using the topside sounder model profiler and digisonde data

To improve the accuracy of the real time topside electron density profiles given by the Digisonde software a new model-assisted technique is used. This technique uses the Topside Sounder Model (TSM), which provides the plasma scale height (H_s), O⁺–H⁺ transition height (H_T), and their ratio Rt = H_s/H_T, derived from topside sounder data of Alouette and ISIS satellites. The Topside Sounder Model Profiler (TSMP) incorporates TSM and uses the model quantities as anchor points in construction of topside density (Ne) profiles. For any particular location, TSMP calculates topside Ne profiles by specifying the values of foF2 and hmF2. In the present version, TSMP takes the F2 peak characteristics – foF2, hmF2, and the scale height at hmF2 – from the Digisonde measurements. The paper shows results for the Digisonde stations Athens and Juliusruh. It is found that the topside scale height used in Digisonde reconstruction is less than that extracted from topside sounder profiles. Rough comparison of their bulk distributions showed that they differ by an average factor of 1.25 for locations of Athens and Juliusruh. When the Digisonde scale heights are adjusted by this factor, the reconstructed topside profiles are close to those provided by TSM. Compared with CHAMP reconstruction profiles in two cases, TSMP/Digisonde profiles show lower density between 400 and 2000 km.     

Scientific ballooning in India – Recent developments

Established in 1971, the National Balloon Facility operated by TIFR in Hyderabad, India, is a unique facility in the country, which provides a complete solution in scientific ballooning. It is also one of its kind in the world since it combines both, the in-house balloon production and a complete flight support for scientific ballooning. With a large team working through out the year to design, fabricate and launch scientific balloons, the Hyderabad Facility is a unique centre of expertise where the balloon design, research and development, the production and launch facilities are located under one roof. Our balloons are manufactured from 100% indigenous components. The mission specific balloon design, high reliability control and support instrumentation, in-house competence in tracking, telemetry, telecommand, data processing, system design and mechanics is its hallmark. In the past few years, we have executed a major programme of upgradation of different components of balloon production, telemetry and telecommand hardware and various support facilities. This paper focuses on our increased capability of balloon production of large sizes up to 780,000 m³ using Antrix film, development of high strength balloon load tapes with the breaking strength of 182 kg, and the recent introduction of S-band telemetry and a commandable timer cut-off unit in the flight hardware. A summary of the various flights conducted in recent years will be presented along with the plans for new facilities.     

Fabrication and flight performance of a large area balloon borne hard X-ray telescope

We describe the fabrication and flight performance of a balloon-borne large area hard X-ray (20–100 keV) telescope for spectral studies of discrete cosmic X-ray sources. The telescope consists of two multi-wire Xenon filled proportional counters of effective area 1200 cm² each, mounted on an orientable platform. It can be pre-programmed to track any celestial source with a pointing accuracy of 0.5 degrees. For one hour of observation the telescope has a 5 σ detection sensitivity of 10⁻⁵ ph cm⁻² s⁻¹. The laboratory test results and the performance in a series of balloon flights conducted in 1984–1986 period is discussed and the preliminary results obtained for some X-ray sources are presented.     

Power supplies for long duration balloon flights

Long duration balloon flights require more electrical power than can be carried in primary batteries. This paper provides design information for selecting rechargeable batteries and charging systems. Solar panels for recharging batteries are discussed, with particular emphasis on cells mounting suitable for balloon flights and panel orientation for maximum power collection. Since efficient utilization of power is so important, modern DC to DC power conversion techniques are presented.On short flights of 1 day or less, system designers have not been greatly concerned with battery weight. But, with the advent of long duration balloon flights using superpressure balloons, anchor balloon systems, and RACOON balloon techniques, power supplies and their weight become of prime importance. The criteria for evaluating power systems for long duration balloon flights is performance per unit weight. Instrumented balloon systems have flown 44 days. For these very long duration flights, batteries recharged from solar cells are the only solution. For intermediate flight duration, say less than 10 days, the system designer should seriously consider using primary cells.