On the basic trends of the upper atmosphere modeling: a review

Zamlutti, C. J.

doi:10.1590/s0102-261x1998000200005

Cited by 3 publications

(4 citation statements)

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“…Reactive collisions are the loss mechanism for the density equation ( 1) and elastic collisions prevail as the loss mechanism for the momentum equation (2). This result can be easily inferred from the modeling equations by Bristow & Watkins (1991) or Zamlutti (1998).…”

Section: Introductionmentioning

confidence: 65%

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The formal equations of the low latitude lower ionosphere and their applications

Zamlutti¹

2005

Rev. Bras. Geof.

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Section: Introductionmentioning

confidence: 65%

“…The ions also acquire energy from photoelectrons through collisional interaction storing it in the form of electronic excitation (Zamlutti, 1997). Then, from Zamlutti (1998), one can write for daylight hours the energy equation in the form:…”

Section: Fundamental Equationsmentioning

confidence: 99%

The formal equations of the low latitude lower ionosphere and their applications

Zamlutti¹

2005

Rev. Bras. Geof.

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“…The model considered production and loss reactions of 16 ions, namely, CO + 2 , CO + , C + , H 2 O + , H 3 O + , OH + , O + 2 , O + , Ar + , Ne + , He + , H + , H + 2 , CH + 3 , CH + 4 , and CH + 5 . Further details are given in the supporting information [Echim et al, 2011;Kallio et al, 2012;Baranov, 2006;Zamlutti, 1998]. We included all the reactions of primary ions, except the charge exchange reactions for secondary ions.…”

Section: Photochemical Modelmentioning

confidence: 99%

“…Like the lunar atmosphere, the atmosphere at a cometary coma is also very tenuous with neutral density of the order of 10 6 to 10 7 cm −3 at 30 km from comet. Further details are given in the supporting information [Echim et al, 2011;Kallio et al, 2012;Baranov, 2006;Zamlutti, 1998].…”

Section: Photochemical Modelmentioning

confidence: 99%

On the origin of the ionosphere at the Moon using results from Chandrayaan‐1 S band radio occultation experiment and a photochemical model

Choudhary

Ambili

Choudhury

et al. 2016

Geophysical Research Letters

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The origin of the Moon's ionosphere has been explored using Chandrayaan‐1 radio occultation (RO) measurements and a photochemical model. The electron density near the Moon's surface, obtained on 31 July 2009 (∼300 cm−3), is compared with results from a model which includes production and recombination of 16 ions, solar wind proton charge exchange, and the electron impact ionization. The model calculations suggest that in the absence of transport, inert ions, namely Ar+, Ne+, and He+, dominate lunar ionosphere (density ∼5 × 104 cm−3). Interaction with solar wind, however, leads to their complete removal (∼2–3 cm−3). Assuming the Moon's exosphere to have CO2, H2O, O, OH, H2, CH4, and CO molecules in addition to the inert gases, the model calculations suggest that the lunar ionosphere is dominated by molecular ions, namely H2O+, CO 2+, and H3O+, with near‐surface density ∼250 cm−3. We surmise that lunar ionosphere can be molecular in nature.

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Weather disturbances in the low latitude ionosphere and their low altitude modeling

Zamlutti

2003

Advances in Space Research

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On the basic trends of the upper atmosphere modeling: a review

Cited by 3 publications

References 0 publications

The formal equations of the low latitude lower ionosphere and their applications

The formal equations of the low latitude lower ionosphere and their applications

On the origin of the ionosphere at the Moon using results from Chandrayaan‐1 S band radio occultation experiment and a photochemical model

Weather disturbances in the low latitude ionosphere and their low altitude modeling

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