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Brune, W. H.

Publications and source records attributed to Brune, W. H..

30 records · Page 2

Kinetics of O3 destruction by ClO and BrO within the Antarctic vortex - An analysis based on in situ ER-2 data

The kinetics of ozone destruction within the Antarctic polar vortex are studied via simultaneous in situ observations of ClO, BrO, O3, N2O, pressure, and temperature. It is found that the chlorine dimer mechanism rate, limited by the reaction ClO + ClO + M yields ClOOCl + M, contributes the most to the integrated rate of ozone destruction within the vortex on isentropic surfaces between altitudes of 14 and 18.3 km.

Anderson, J. G.↗

In situ northern mid-latitude observations of ClO, O3, and BrO in the wintertime lower stratosphere

In order to test photochemical theories linking chlorofluorocarbon derivatives to O3 depletion at high latitudes in the springtime, several related atmospheric species, including O3, ClO, and BrO were measured in the lower stratosphere. The flight path extended to the center of the polar jet associated with but outside of the Arctic vortex, in which the abundance of O3 was twice its midlatitude value, whereas BrO levels were five parts per trillion (pptv) by volume between 18 and 21 km, and 2.4 pptv below that altitude. The ClO mixing ratio was as much as 65 pptv at 60 N latitude at an altitude of 20 km, and was enhanced over midlatitude values by a factor of three to five at altitudes above 18 km and by as much as a factor of 40 at altitudes below 17 km. Levels of ClO and O3 were highly correlated on all measured distance scales, and both showed an abrupt change in character at 54 N latitude. The ClO abundance north of 54 N was probably caused by low NO2 levels in the flight path.

Brune, W. H.↗

In situ observations of ClO in the Antarctic: Evidence for chlorine catalyzed destruction of ozone

Results from a series of 12 ER-2 aircraft flights into the Antarctic polar vortex are summarized. These in situ data define the spatial and temporal distribution of ClO as the aircraft flew at an altitude of approx. 18 km from Punta Arenas (54 deg S latitude) to the base of the Palmer Peninsula (72 deg S latitude), executed a rapid descent to approx. 13 km, turned north and climbed bach to approximately 18 km, returning to Punta Arenas. A general pattern in the ClO distribution is reported: mixing ratios of approximately 10 ppt are found at altitude in the vicinity of 55 deg S increasing to 50 ppt at 60 degrees S. In the vicinity of 65 deg S latitude a steep gradient in the ClO mixing ratio is observed. At a fixed potential temperature, the ClO mixing ratio through this sharp transition increases by an order of magnitude within a very few degrees of latitude, thus defining the edge of the chemical containment vessel. From the edge of that containment vessel to the southern extension of the flights, 72 deg S, a dome of slowly increasing ClO best describes the distribution. Conclusion are drawn from the data.

Anderson, J. G.↗

In situ observations of ClO in the wintertime Northern Hemisphere: ER-2 aircraft results from 21 N to 61 N latitude

Measurements of lower stratospheric ClO taken during a NASA ER-2 flight between Moffett Field, CA (37 N, 122 W) and Great Slave Lake, Canada (61 N, 116 W) on 13 February 1988 are reported. Northbound, the aircraft was flown at about 20 km altitude from 39 N to 56 N, at 18 km from there to 58 N, in a descent to 15 km at 60 N, and in a rise and turn at the northernmost point. The southbound leg was flown in a gradual climb from 20 km to 21.5 km. On this day, the central position of the Arctic polar vortex, as determined by an NMC analysis of heights and temperatures at the 50 mb and 70 mb levels, was approximately 79 N, 100 W. Because the vortex was located on the North American side of the pole, the aircraft was able to reach a point slightly inside the maximum horizontal wind region where wind speeds were 80 to 90 knots. The general pattern for the observed ClO is that it increased with both latitude and altitude, and attained a maximum of about 55 pptv at 61 N latitude and 20.5 km altitude. This value is about 20 times smaller than the maxima observed over Antarctica, but is comparable to those seen just outside the chemical containment vessel located inside the Antarctic Polar vortex. On the other hand, in a comparison with northern midlatitude data taken on this and three other February flights, ClO mixing ratios observed north of 55 N latitude are 2 to 5 times larger at all flight altitudes (15 to 20 km). Possible reasons are discussed for this enhancement over midlatitude and the evidence is considered for whether or not the instruments sampled Arctic polar vortex air. A second feature of the data is the strong positive correlation between ClO and O3 during the entire flight.

Brune, W. H.↗

In situ observations of BrO over Antarctica: ER-2 aircraft results from 54 S to 72 S latitude

Bromine monoxide was observed in situ at approximately 18 km altitude during nine flights of the NASA ER-2 aircraft from Punta Arenas, Chile (54 altitude) to 72 S latitude over the Palmer Peninsula, Antarctica. The first flight for the BrO detection system was on 28 August. Here, the results from the flights over Antarctica and from the ferry flights from Punta Arenas to Moffett Field, CA (37 N latitude are reported. A key question concerning BrO, then, is how it is distributed with respect to the chemical containment vessel defined by elevated ClO mixing ratios. This question is answered with greatest statistical significance if the data are averaged into five regions: outside the vessel, aircraft heading south; inside the vessel on the same potential temperature surface; in the dive region; inside the vessel on a given potential temperature surface, aircraft heading north; and outside the vessel on the same surface. The result is that the BrO distribution inside the chemical containment vessel was different from that found outside. Inside, the BrO mixing ratio was (5.0 plus or minus 1.1) pptv between the 400 K and 460 K potential temperature surfaces, decreasing only slightly with potential temperature, and was less than 3.6 pptv below the 4 00 K surface. The abundance of BrO inside the chemical containment vessel showed no discernible temporal trend during the course of the nine flights. Outside the vessel, the BrO mixing ratio was (4.7 plus or minus 1.3) pptv near the 450 K surface, but decreased to (2.8 plus or minus 1.0) pptv near the 420 K surface.

Brune, W. H.↗

Possible detection of far-ultraviolet line emission from a hot galactic corona

The presence of an emission-line component to the radiation field is suggested by rocket observations, at low resolution, of the spectrum of the diffuse, far-ultraviolet background near the north galactic pole. Removal of the line emission leaves a residual uniform cosmic ultraviolet background radiation of only 150 + or - 50 photons/sq cm s sr A, or about half that previously reported. The lines, which are at the wavelengths of the collisionally-excited atom emissions that have been predicted to arise from a hot galactic corona, suggest that there is no need to explain observed high-ionization states at high galactic latitudes as being due to photoionization caused by neutrino decay.

Feldman, P. D.↗

Far-ultraviolet studies. V - Rocket observation of the diffuse cosmic background

A far-ultraviolet spectrometer and several far-ultraviolet photometers have been carried to an altitude of 347 km to measure the spectrum of three regions at high galactic latitudes. After correction for O I airglow and for stars in the field of view, a nearly uniform residual intensity of 285 plus or minus 32 photons per (sq cm s sr A) is found over the spectral range 1230-1680 A, along with some evidence for a sharp rise in intensity longward of 1680 A. It is argued that the signal is not likely to be due to light scattering from interstellar dust. The flat spectrum could represent the integrated light of distance galaxies. The sharp rise must be due to some other phenomenon.

Anderson, R. C.↗

The spectrum of the diffuse cosmic ultraviolet background

A far-ultraviolet spectrometer and several far-ultraviolet photometers were carried to an altitude of 347 km and used to measure the spectrum of three regions at high galactic latitudes. After correction for O I airglow and for stars in the field of view, a nearly uniform residual intensity of 285 + or - 32 photons (per sq cm s sr A) over the spectral range 1230-1680 A is found, along with some evidence for a sharp rise in intensity longward of 1680 A. It is believed that the signal is not likely to be due to light scattering from interstellar dust. The flat spectrum is perhaps the integrated light of distant galaxies. The sharp rise must be due to some other phenomenon.

Anderson, R. C.↗

Vacuum ultraviolet spectrophotometry and effective temperatures of hot stars

Absolutely calibrated ultraviolet stellar spectra from 3100 A to the hydrogen absorption edge at 912 A were obtained on 1977 February 17 by rocket observations above Woomera, Australia. Spectra taken at 15 A resolution have been compared with the observed fluxes from OAO 2 and with recent model-atmosphere fluxes of Kurucz for five hot stars: Gamma (2) Vel, Zeta Pup, Alpha Eri, Beta Cen, and Alpha Vir. The present data give fluxes which are generally lower than those obtained from OAO 2, with the largest deviations of about 20% between 1400 and 1700 A. Agreement with the models is good, although the model fluxes are substantially larger than the observed values below 1200 A. This discrepancy is greater for the higher-temperature stars. Effective temperatures are also determined and are in good agreement with previous results.

Brune, W. H.↗

A search for far-ultraviolet emission from Sirius B

A rocket observation of Sirius in the far-UV region from 912 to 1240 A is reported. It is found that only a few counts were detected which can possibly be attributed to the hydrogen-rich white dwarf Sirius B. An upper limit of 2.0 by 10 to the -10th power erg/sq cm per sec/A on the Sirius B flux in the range from 1000 to 1080 A is established with 99.3% confidence. This upper limit is shown to constrain the model-dependent effective temperature of Sirius B to be less than or approximately 27,000 K. It is concluded that the observed X-ray flux from Sirius cannot be emitted by the photosphere of Sirius B.

Brune, W. H.↗

Midlatitude oxygen ultraviolet nightglow

A rocket-borne spectrometer measured the weak UV nightglow from 1240 to 1670 A in the altitude range 180-345 km above White Sands, New Mexico. Detection of nightglow emissions at the atomic oxygen lines (1304 and 1356 A) confirmed the existence of a weak midlatitude oxygen nightglow similar to the tropical airglow. Radiative recombination appeared to be the principal cause of the peak observed intensities of the atomic oxygen line emissions, though a maximum 25% contribution from mutual neutralization of O(+) and O(-) could also be contemplated. Partial radiative recombination coefficients are derived from the data.

Brune, W. H.↗

Carbon production in comet West 1975n

Rocket-ultraviolet spectra of comet West 1975n are reported which were obtained with scanning spectrophotometers in the wavelength range from 1200 to 1300 A. The principal emission features observed include lines of C, O, and C(+), as well as bands of OH, CO, CO(+). The estimated fluxes of the C, O, H, CO, and OH features are found to be consistent with a photodissociation source in which the CO evaporation rate is about one-third that of water. The presence of a large number of carbon atoms in the metastable 1D state is indicated and taken to suggest that dissociative recombination is important near the cometary nucleus, that CO must originate in the nucleus, and that CO is the primary carbon constituent of the comet.

Feldman, P. D.↗