Further evidence of total ozone variation during the solar eclipse of 1995

Chakrabarty, D.; Peshin, S. K.; Srivastav, S. K.; Shah, Neera; Pandya, K. V.

doi:10.1029/2000jd900522

Cited by 8 publications

(8 citation statements)

References 16 publications

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“…The undulations observed in columnar ozone concentration are of significant amplitude. The similar kinds of undulations were also reported in literature [ Mims and Mims , 1993; Chakrabarty et al , 1997, 2001]. The similar variation in ground‐reaching UV radiation is expected due to increase and decrease in total columnar ozone.…”

Section: Resultssupporting

confidence: 88%

“…In fact, the most efficient reactions involving ozone are driven by solar radiation [ Finlayson‐Pitts and Pitts , 2000; Seinfeld and Pandis , 2006]. The effects of a solar eclipse on the total ozone column have been widely studied by various groups [ Bojkov , 1968; Mims and Mims , 1993; Chakrabarty et al , 1997, 2001; Zerefos et al , 2000; Kazadzis et al , 2007; Zerefos et al , 2000 and references therein]. A series of fluctuations in the column ozone was observed following the totality of eclipse preceded with reduced amplitude [ Mims and Mims , 1993].…”

Section: Introductionmentioning

confidence: 99%

“…Column ozone measurements during the eclipse on August 11, 1999 showed positive and negative fluctuations of 2% in the column ozone within a period of two hours [ Tzanis , 2005]. During the same eclipse, at the maximum obscuration, the ozone column has decreased by about 25 Dobson units (DU) from its pre‐eclipse value over New Delhi (28.4N 77.1E) [ Chakrabarty et al , 1997, 2001]. Wavelike fluctuations were observed in total columnar ozone over Ahmedabad, India (23N, 72E).…”

Section: Introductionmentioning

confidence: 99%

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The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

et al. 2012

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[1] Studies on the solar eclipse-induced changes in near-surface ozone and its precursors NO x and CO were carried out at two nearby tropical coastal locations, Thumba (very close to the sea) and the Centre for Earth Science Studies (CESS), which is 4.5 km off the Thumba coast and with varying topography, during the annular eclipse of 15 January 2010. The surface ozone decreased by 12 and 13 ppb (35% and 52%) over Thumba and CESS, with the time lag of 40 min and 25 min from the maximum phase of eclipse, respectively, and at CESS, post-eclipse recovery was faster compared to Thumba. No pronounced change was observed in NO x , but CO showed an enhancement toward the ending phase of the eclipse. The diurnal patterns of ozone and their differences at the two sites were strongly dependent on local meteorology, in particular, the mesoscale dynamics and topography. While the temperature decreased by 1.2°C at Thumba, the decrease was almost double ($2.1°C) at CESS. The early fall in temperature caused the early setting in of land-breeze (post-eclipse effect), which in turn triggered an early evening decrease in near-surface ozone compared to the control conditions. The present study points to the role of mesoscale meteorology/dynamics in controlling the evolution of solar eclipse-induced changes in ozone in a relatively clean environment. The chemical box model simulations reproduced these broad features: a percentage decrease and the time lag in surface ozone. The observation of total column ozone showed a decrease and fluctuations, after the eclipse maximum.

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Section: Resultssupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

et al. 2012

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“…Winkler et al (2001) reported contradicting results from Brewer and Microtops ozone measurements at Hohenpeissenberg during the total solar eclipse of 11 August 1999. Chakrabarty et al (2001) suggested that the observed ozone variability over India during the eclipse of 24 October 1995 could not be explained by the variations in the rates of conventional photochemical and dynamical processes or by the formation of gravity waves during the eclipse.…”

Section: Introductionmentioning

confidence: 99%

Attenuation of global ultraviolet and visible irradiance over Greece during the total solar eclipse of 29 March 2006

et al. 2007

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Abstract. The variability of ultraviolet and photosynthetically active radiation (PAR) during the total solar eclipse of 29 March 2006 was examined in this study. The measurements from NILU-UV multichannel radiometers at 7 stations of the Greek UV Network were used, where the maximum eclipse percentage ranged from 73.1% to 94.8%. In addition, an extra instrument was established at a remote Greek island, Kastelorizo, which was within the Moon's umbral shadow. The reduction of irradiance at 305 and 312 nm relative to non-eclipse conditions at all sites was almost 1.5 times more than the corresponding decrease in the UVA and visible part of the spectrum and reached 98% for eclipse percentage equal to 94%. The availability of several instruments in close proximity to the path of the umbral shadow provided a challenging test for the models. The measured changes in UV and visible irradiance were compared with 1-D model calculations accounting for the limb darkening effect. The agreement between measurements and modeled values at all sites is within 3% for eclipse percentages of less than 30% and becomes worse as the eclipse progresses. The 1-D model reproduced the spectral effect of the eclipse in UVA and PAR wavelength regions within 3% for eclipse percentages up to 50%, but only the half of the observed change was captured as the eclipse progressed. At three sites, where the eclipse maximum was more than 94%, the measured irradiance at 305 nm for eclipse percentages of more than 85% decreased with slower rates than for longer wavelengths. As a result, the total ozone values, derived from the 305/320 nm ratios, apparently decreased significantly for high eclipse percentages. The effect is similar at all three sites, but the interpretation of this observation remains a challenge. Comparison results with 3-D model calculations shortly before, during and shortly after totality were performed for the first time and revealed an agreement with measurements within 20% in the Correspondence to: A. Kazantzidis (akaza@auth.gr) UV-A region. However, the modeled estimates of irradiance at 312 nm are three times lower than measured values.

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“…During another eclipse of 87% totality, Elansky and Elokhov [1993] measured a 55% ± 6% increase in NO 2 VCD using zenith‐sky visible spectroscopy. Chakrabarty et al [2001] found that NO 2 slant column densities (SCDs) measured by a visible spectrometer approximately doubled and identified a wavelike structure in the NO 2 measurements. They suggested that the latter effect was related to eclipse‐induced gravity waves.…”

Section: Introductionmentioning

confidence: 99%

Ozone and NO₂ variations measured during the 1 August 2008 solar eclipse above Eureka, Canada with a UV‐visible spectrometer

Adams¹,

McLinden²,

Strong³

et al. 2010

J. Geophys. Res.

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[1] On 1 August 2008, a solar eclipse of 98% totality passed over the Polar Environment Atmospheric Research Laboratory at Eureka, Canada (80.05°N, 86.42°W), which is run by the Canadian Network for the Detection of Atmospheric Change. During the eclipse, a zenith-sky UV-visible spectrometer measured slant column densities (SCDs) and vertical column densities (VCDs) of ozone up to 82% occultation and NO 2 up to 96% occultation, beyond which low light intensities and changes in the solar spectrum due to limb darkening compromised data quality. Ozone VCDs during the eclipse remained within natural variability, and this study is inconclusive regarding ozone oscillations due to limited temporal resolution and measurement errors toward eclipse maximum. Measured NO 2 SCDs increased and decreased symmetrically around the eclipse maximum. NO 2 SCDs were also calculated using a photochemical box model and a one-dimensional radiative transfer model. The modeled ratio of eclipse day SCDs to the previous day's SCDs was compared to the measurements. They agreed within error bars leading up to maximum occultation, but the model ratio was systematically larger than the measured ratio for the second half of the eclipse, perhaps due to changing cloud conditions throughout the eclipse. The measured NO 2 SCD ratio of 1.84 −0.43 +0.12 at 96% totality is larger than observed in past studies and agrees with modeled ratio of 1.91. Therefore our current understanding of stratospheric photochemistry is sufficient to predict the evolution of NO x chemistry through a solar eclipse.

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Further evidence of total ozone variation during the solar eclipse of 1995

Cited by 8 publications

References 16 publications

The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

Attenuation of global ultraviolet and visible irradiance over Greece during the total solar eclipse of 29 March 2006

Ozone and NO₂ variations measured during the 1 August 2008 solar eclipse above Eureka, Canada with a UV‐visible spectrometer

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Further evidence of total ozone variation during the solar eclipse of 1995

Cited by 8 publications

References 16 publications

The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

The changes in near‐surface ozone and precursors at two nearby tropical sites during annular solar eclipse of 15 January 2010

Attenuation of global ultraviolet and visible irradiance over Greece during the total solar eclipse of 29 March 2006

Ozone and NO2 variations measured during the 1 August 2008 solar eclipse above Eureka, Canada with a UV‐visible spectrometer

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Ozone and NO₂ variations measured during the 1 August 2008 solar eclipse above Eureka, Canada with a UV‐visible spectrometer