Corrigendum to “The Sunlit lunar atmosphere: A Comprehensive study by CHACE on the Moon Impact Probe of Chandrayaan-1” [Planet. Space Sci. 58 (2010) 1567–1577]

Sridharan, R.; Ahmed, S.M.; Das, Tirtha Pratim; Sreelatha, P.; Kumar, P. Pradeep; Naik, Neha; Supriya, Gokulapati

doi:10.1016/j.pss.2014.12.021

Cited by 11 publications

(4 citation statements)

References 3 publications

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“…At a first cut it may appear that these values indicated a much denser atmosphere than previously presumed (e.g., Dollfus, 1956;Stern, 1999 and the references cited therein). It had been clarified through a note (Sridharan et al, 2014) that what has actually been recorded is without taking the velocity of the probe through the medium into account and when one wants to estimate the actual number density of any of the measured species this factor has to be accounted for. The volume correction factor turns out to be 10 4 implying that the actual pressure values were $5 Â 10 À 11 Torr ( $6.5 Â 10 À 9 Pa).…”

Section: Introductionmentioning

confidence: 99%

The spatial distribution of molecular Hydrogen in the lunar atmosphere—New results

Thampi

Sridharan

Das

et al. 2015

Planetary and Space Science

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Section: Introductionmentioning

confidence: 99%

The spatial distribution of molecular Hydrogen in the lunar atmosphere—New results

Thampi

Sridharan

Das

et al. 2015

Planetary and Space Science

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“…The number density of Ar-40 derived from CHACE-2 is about three orders of magnitude higher than that reported by previous observations in the near equatorial region. Such a discrepancy has been reported during CHACE/Chandrayaan-1 observations also and a correction factor of 4 10 E was applied subsequently (Sridharan et al, 2015) to account for the enhancement of signal due to the movement of the spacecraft. It is to be noted that CHACE was part of MIP, which was aimed to impact on the lunar surface and the measurements of the lunar exosphere happened during the course of travel toward the surface (  E 1 hr), before the impact.…”

Section: Instrumentation Data Sources and Methodologymentioning

confidence: 85%

Argon‐40 in Lunar Exosphere: Observations From CHACE‐2 on Chandrayaan‐2 Orbiter

Dhanya

Thampi

Das

et al. 2021

Geophysical Research Letters

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The Moon is known to possess a surface bounded exosphere (Killen & Ip, 1999;Stern, 1999). Characterization of the composition of lunar exosphere and its variability remains an outstanding problem. Noble gases serve as important tracers to understand different processes that contribute to the exosphere and their distribution in the high latitude regions remains poorly explored.Argon-40 (Ar-40) is one of the noble gas, whose presence in the lunar exosphere was first confirmed by Lunar Atmospheric composition Experiment (LACE) on Apollo-17 (Hodges & Hoffman, 1974;Hoffman et al., 1973). LACE detected Ar-40 at the landing site close to the equatorial region of the Moon. LACE observations, which lasted for nine lunations, were confined to the nightside of the Moon bounded by sunrise and sunset terminators, due to the detector saturation effects on the dayside. The observations showed that the surface number density of Ar-40 decrease through the nightside and peaks near the sunrise terminator, typical of a condensable gas that gets absorbed at the cold lunar nightside surface and gets desorbed during

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“…Chandra's Altitudinal Composition Explorer (ChACE), a mass spectrometer-based instrument, was a part of MIP aboard Chandrayaan-1. Results obtained from ChACE are described in series of papers [Sridharan et al, 2010a[Sridharan et al, , 2010b[Sridharan et al, , 2015Thampi et al, 2015;Das et al, 2016;Bhardwaj et al, 2015]. The surface densities of neutral species used in this model are the following: CO 2 = 6 × 10 5 cm −3 , CO = 7.1 × 10 2 cm −3 , H 2 O = 8 × 10 5 cm −3 , OH = 2 × 10 5 cm −3 , O = 2 × 10 2 cm −3 , Ar = 3 × 10 4 cm −3 , Ne = 2 × 10 4 cm −3 , He = 3 × 10 4 cm −3 , H 2 = 1 × 10 3 cm −3 , and CH 4 = 6 × 10 2 cm −3 .…”

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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Corrigendum to “The Sunlit lunar atmosphere: A Comprehensive study by CHACE on the Moon Impact Probe of Chandrayaan-1” [Planet. Space Sci. 58 (2010) 1567–1577]

Cited by 11 publications

References 3 publications

The spatial distribution of molecular Hydrogen in the lunar atmosphere—New results

The spatial distribution of molecular Hydrogen in the lunar atmosphere—New results

Argon‐40 in Lunar Exosphere: Observations From CHACE‐2 on Chandrayaan‐2 Orbiter

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

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