Ozone Measurements during Solar Eclipse

Stranz, D.

doi:10.1111/j.2153-3490.1961.tb00084.x

Cited by 12 publications

(3 citation statements)

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“…From the earliest days of atmospheric research, meteorological measurements have been stationed within predicted paths of eclipse shadows to investigate these sensitivities (for a brief historical review, see Aplin and Harrison [2003, section 2]). In the middle atmosphere, the earliest such measurements focused on ozone changes during eclipses, given evolving understanding of the role of solar ultraviolet photolysis in odd oxygen production in the stratosphere and mesosphere [ Kawabata , 1937; Jerlov et al , 1954; Stranz , 1961; Hunt , 1965; Randhawa , 1968]. Rocketsonde sounding experiments also searched for eclipse‐related changes to stratospheric and mesospheric winds and temperatures [ Ballard et al , 1969].…”

Section: Introductionmentioning

confidence: 99%

Atmospheric effects of the total solar eclipse of 4 December 2002 simulated with a high‐altitude global model

et al. 2007

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[1] The atmosphere's response to the total solar eclipse of 4 December 2002 is studied using a prototype high-altitude global numerical weather prediction model (NOGAPS-ALPHA). Local reductions in solar ultraviolet (UV) radiation during the eclipse are estimated using astronomical calculations of umbral and penumbral surface trajectories and observed solar limb darkening at $200-300 nm. In NOGAPS-ALPHA these UV eclipse shadows yield stratospheric radiative cooling rate footprints peaking near 27 K day À1 , a value 2-3 times larger than assumed in previous modeling. Difference fields between NOGAPS-ALPHA runs with and without this eclipse forcing reveal vertically deep middle atmospheric responses, with three-dimensional horizontal structures very similar to the large-scale ''bow-wave'' response first proposed by Chimonas (1970). Such structure appears clearly only at later times when total eclipses have abated and gravity waves generated in the stratosphere have had time to propagate vertically. Bow-wave amplitudes and direct thermal cooling responses are both small (]1 K for temperature and ]2-3 m s À1 for horizontal winds), contradicting some rocketsonde measurements that suggest much larger responses near 50-60 km altitude. We also find clear evidence of a bow-wave-like response in the model's surface pressure fields, with an amplitude $0.1-0.5 hPa, while surface air temperatures in NOGAPS-ALPHA show $4 K cooling over Africa during the eclipse. Both findings are consistent with surface atmospheric data acquired during previous eclipse passages.

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Section: Introductionmentioning

confidence: 99%

Atmospheric effects of the total solar eclipse of 4 December 2002 simulated with a high‐altitude global model

et al. 2007

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“…Although nine sets of ozone observations during eclipses have been reported (Bezverkhny et al, 1956;D'Albe & Rasool, 1956; Kawabata, 1937; Khrigian & Kuznezov, 1965;Jerlov et al, 1954;Pariisky & Chao, 1961;Steblova, 1962;Stranz, 1961;Svensson, 1956), results of only three can be compared with confidence. These three (D'Albe & Rasool, 1956;Svensson, 1958;Stranz, 1961) report observations made with Dobson ozoneepectrophotometers, which poss e~ the spectral accuracy needed for measurements of this type. The other six sets of observations vary widely and report from a 40 per cent ozone decrease (Jerlov et al, 1954) to a 20-30 per cent increase (Khrigian & Kuznezov, 1965; Steblova, 1962) and even a physically impossible increase of 300-400 per cent (Bezverkhny et al, 1956).…”

Section: Introductionmentioning

confidence: 99%

The ozone variations during the solar eclipse of 20 May 1966

Bojkov¹

1968

Tellus

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During the annular (87.6 %) solar eclipse of May 20, 1966, more than 60 measurements of total ozone were taken with the Dobson ozonespectrophotometer at the University of Sofia, Bulgaria. An analysis of data obtained shows an ozone increase of 26-30 m atm-cm (An > 2an) at the maximum phase of the eclipse. However, according to the photochemical theory, only -1 m atm-cm increase should occur during an eclipse such as this.The difference between the theoretical and observed increase of the total ozone may be partly due to the limb-darkening effect. The importance of this effect increases progressively to the maximum phase of the eclipse. When dark-limb correction is applied to observational data, the ozone increase is reduced to 14 m atm-cm (about 4 per cent of the total ozone amount). This increase is as yet unexplained.

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“…Several workers have studied the variation of ozone during a solar eclipse by a one-dimensional (l-D) photochemical model [Hunt, 1965;Doherty, 1969;Keneshea, 1969;Wuebbles and Chang, 1979]. Hunt [1965] was probably the first to make an attempt to explain the observations made by Stranz [1961] during the solar eclipse of October 2, 1959. He used a Chapman reactions scheme that assumed reactive species in the atmosphere as oxygen.…”

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confidence: 99%