Air-cooling mathematical analysis as inferred from the air-temperature observation during the 1st total occultation of the Sun of the 21st century at Lusaka, Zambia

Peñaloza-Murillo, Marcos A.; Pasachoff, Jay M.

doi:10.1016/j.jastp.2015.02.002

Cited by 11 publications

(28 citation statements)

References 53 publications

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“…It provided for solar and terrestrial observations under unusually extreme conditions [1,2], extending our measurements of the effect of solar eclipses on the terrestrial atmosphere [3].…”

Section: Introductionsupporting

confidence: 57%

Terrestrial atmospheric responses on Svalbard to the 20 March 2015 Arctic total solar eclipse under extreme conditions

Pasachoff

Peñaloza-Murillo

Carter

et al. 2016

Phil. Trans. R. Soc. A.

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“…It provided for solar and terrestrial observations under unusually extreme conditions [1,2], extending our measurements of the effect of solar eclipses on the terrestrial atmosphere [3].…”

Section: Introductionsupporting

confidence: 57%

Terrestrial atmospheric responses on Svalbard to the 20 March 2015 Arctic total solar eclipse under extreme conditions

Pasachoff

Peñaloza-Murillo

Carter

et al. 2016

Phil. Trans. R. Soc. A.

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“…In Peñaloza‐Murillo and Pasachoff (), astrometric and physical basic aspects of TSEs, like solar limb darkening, occultation, and obscuration functions, were explained and reviewed in depth, inferred from temperature observations during the first TSE of the 21st century on 21 June 2001, at Lusaka, Zambia. For the 2009 Chinese TSE, we will try to apply the same methodology and analysis, without repeating details.…”

Section: The Occultation and Obscuration Functionsmentioning

confidence: 99%

“…In our case we have taken the values b = 0.84 and c = −0.20. Using the notation of Tzanis (), and taking into account additional explanations in Peñaloza‐Murillo and Pasachoff (), this function is expressed as follows:

normalΓ ((), ν) = 1 - b - c + b {(1 - ν^{2})}^{1 / 2} + c ((), 1 - ν^{2}),

where ν = r / R s , cos ψ = (1 − ν 2 ) 1/2 , Γ( ν ) = I ( ν )/ I (0), and r is a radial integration variable taken on the solar disk which gives the distance from the apparent solar center to a ring or annulus of dr width partially intersected by the Moon at a given instant t ; thus, dr = R s dν . The apparently fractional lack of energy, corresponding to a particular area of the Sun being occulted at a given instant t by the Moon, is the integration of this annulus over the blocked solar area along with the solar limb darkening function

2 \int_{v_{\min}}^{1} normalΓ ((), v) ϕ {rR}_{s} normald v = 2 \int_{v_{\min}}^{1} normalΓ ((), v) ϕ R_{s}^{2} normald v,

where ϕ is given by this interception when one considers that it defines an aperture angle, 2 ϕ , subtended at the center of the solar disk by the partially occulted annulus.…”

Section: The Occultation and Obscuration Functionsmentioning

confidence: 99%

“…So far, this is the very useful scheme derived by Tzanis (), which was applied to ground‐based observations of ozone at Athens, Greece, during the solar partial eclipse of 11 August 1999, in that city. The second part (Moon exiting) proceeds in the same fashion but reversing the integration procedures, that is to say, inverting the integration limits; now the integration has a negative direction (−d ν ) and so on (see Peñaloza‐Murillo & Pasachoff, ).…”

Section: The Occultation and Obscuration Functionsmentioning

confidence: 99%

“…The next step is to account for the effect of the eclipse on these solar radiation profiles through the application of the obscuration function, calculated via equations – (for further details on how to proceed with this calculation, see Peñaloza‐Murillo & Pasachoff, ).…”

Section: Models Of the Solar Radiation Under Occultation Of The Sun Bmentioning

confidence: 99%

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Cloudiness and Solar Radiation During the Longest Total Solar Eclipse of the 21st Century at Tianhuangping (Zhejiang), China

Peñaloza-Murillo

Pasachoff

2018

JGR Atmospheres

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The lack of comprehensive solar radiation monitoring during the longest total solar eclipse of the 21st century at Tianhuangping (Zhejiang), China, on 22 July 2009, has led to this investigation in order to evaluate the cloudiness contribution in estimating the impact on global solar radiation throughout this phenomenon. In doing so, we applied a cloud cover empirical model to obtain the global solar radiation and, at the same time, we deduced a theoretical model to get the direct solar radiation in which both the occultation and obscuration functions of this eclipse are included. We took limb darkening and atmospheric transmission into account. Though the weather during our eclipse observations agreed with the forecasts for that day, clouds and some rain, we were nonetheless able to observe all phases of the eclipse from our observation site at Tianhuangping. This experience suggests that for coming eclipses a record of the in situ observation protocol of cloudiness is mandatory. Our results for comparing global solar radiation models indicate that our total solar eclipse radiation model is quite acceptable and representative of that which could have happened at that time.Plain Language Summary A total solar eclipse is a situation where the Sun is obscured by the Moon viewed from Earth. In this particular arrangement in space a shadow is cast over a particular region. Thus, the ideal circumstances to observe a total solar eclipse are those in which the sky is cloudless in that region or zone. Yet from time to time this phenomenon occurs in the presence of interfering clouds preventing a direct observation of the event. However, under these adverse circumstances effects over the environment can still be felt and measured as, for example, the rapid reduction of solar energy reaching the surface. In that case such measurements would be lacking, but with some information about cloudiness one can have an idea of how the variation of this energy during the eclipse took place. In the procedure a quantitative knowledge of how the Moon disk is going to progressively cut the Sun's brightness during the eclipse is necessary. From an environmental point of view it is shown that a scientific observation of a total solar eclipse matters even though it was made under the influence of blocking clouds.

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Environmental Effect of a Solar Eclipse: What Happens, When the Solar Radiation Changes?

Mitre

2019

International Climate Protection

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Air-cooling mathematical analysis as inferred from the air-temperature observation during the 1st total occultation of the Sun of the 21st century at Lusaka, Zambia

Cited by 11 publications

References 53 publications

Terrestrial atmospheric responses on Svalbard to the 20 March 2015 Arctic total solar eclipse under extreme conditions

Terrestrial atmospheric responses on Svalbard to the 20 March 2015 Arctic total solar eclipse under extreme conditions

Cloudiness and Solar Radiation During the Longest Total Solar Eclipse of the 21st Century at Tianhuangping (Zhejiang), China

Environmental Effect of a Solar Eclipse: What Happens, When the Solar Radiation Changes?

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