Auroral and photoelectron fluxes in cometary ionospheres

Bhardwaj, Anil; Haider, S. A.; Singhal, R. P.

doi:10.1016/0019-1035(90)90112-m

Cited by 43 publications

(64 citation statements)

References 48 publications

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“…The degradation of the solar UV-EUV radiation and solar EUV-generated photoelectrons in the coma is modeled using the method of Bhardwaj et al (1990Bhardwaj et al ( , 1996 and further developed by Bhardwaj (2003). The electron impact production rates are calculated using the Analytical Yield Spectrum (AYS) approach, which is based on the Monte Carlo method.…”

Section: Chemistry-transport Model Of O Atomsmentioning

confidence: 99%

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O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

Capria¹,

Cremonese

Bhardwaj

et al. 2005

A&A

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High resolution spectroscopy observation of comet 153P/2002 C1 Ikeya-Zhang was performed on April 20, 2002 with the echelle spectrograph SARG on the 3.5 m Telescopio Nazionale Galileo in La Palma. The atomic O emission lines at 5577, 6360 and 6363 Å are clearly visible in the spectrum. We determined the intensity ratio of the green line to the sum of the red lines. In order to verify the hypothesis that water is the main parent species of these emissions, the result was compared with the value obtained from a coupled chemistry-transport model. The measured value for the green to red ratio, 0.12 ± 0.1, agrees quite well with the value obtained from the model. This led us to conclude that during the observation water was the parent species of atomic O lines.

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Section: Chemistry-transport Model Of O Atomsmentioning

confidence: 99%

“…The electron impact production rates are calculated using the Analytical Yield Spectrum (AYS) approach, which is based on the Monte Carlo method. Details of AYS approach are given in several of the previous cited papers (Bhardwaj et al 1990(Bhardwaj et al , 1996Bhardwaj & Michael 1999a,b;Bhardwaj 1999 …”

Section: Chemistry-transport Model Of O Atomsmentioning

confidence: 99%

O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

Capria¹,

Cremonese

Bhardwaj

et al. 2005

A&A

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“…In this region, the solar wind electrons may also contribute to the total emission intensity (Bhardwaj et al 1990(Bhardwaj et al , 1996Bhardwaj 1999). However, the dissociative recombination CObearing ions to the total emission intensity contribute little (<5%), whereas the formation of atomic oxygen contributes significantly (50%), because of charge exchange between O + and OH + with H 2 O.…”

Section: Parameters That Can Influence the Predicted Emission Intensimentioning

confidence: 99%

“…The coupled-chemistry-emission model has been used in the present study, which accounts for main production and loss processes for CO(a 3 Π), O( 3 P), O( 1 D), O( 1 S), C( 3 P), and C( 1 D) species in the inner cometary coma, as described in earlier works (Bhardwaj et al 1990(Bhardwaj et al , 1996Bhardwaj 1999Bhardwaj , 2003Bhardwaj & Raghuram 2011. Calculations are done at a perihelion distance (1.29 AU).…”

Section: Model Input Parametersmentioning

confidence: 99%

Prediction of Forbidden Ultraviolet and Visible Emissions in Comet 67p/Churyumov–gerasimenko

Raghuram

Bhardwaj

Galand

2016

ApJ

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Remote observation of spectroscopic emissions is a potential tool for the identification and quantification of various species in comets. The CO Cameron band (to trace CO 2 ) and atomic oxygen emissions (to trace H 2 O and/ or CO 2 , CO) have been used to probe neutral composition in the cometary coma. Using a coupled-chemistryemission model, various excitation processes controlling the CO Cameron band and different atomic oxygen and atomic carbon emissions have been modeled in comet 67P/Churyumov-Gerasimenko at 1.29 AU (perihelion) and at 3 AU heliocentric distances, which is being explored by ESAʼs Rosetta mission. The intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines as a function of projected distance are calculated for different CO and CO 2 volume mixing ratios relative to water. Contributions of different excitation processes controlling these emissions are quantified. We assess how CO 2 and/or CO volume mixing ratios with respect to H 2 O can be derived based on the observed intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines. The results presented in this work serve as baseline calculations to understand the behavior of low out-gassing cometary coma and compare them with the higher gas production rate cases (e.g., comet Halley). Quantitative analysis of different excitation processes governing the spectroscopic emissions is essential to study the chemistry of inner coma and to derive neutral gas composition.

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“…The photoelectron and auroral electron impact ionization and dissociative ionization rates are calculated using the Analytical Yield Spectrum approach (Bhardwaj et al, 1990(Bhardwaj et al, , 1996Bhardwaj, 1999Bhardwaj, , 2003, and references therein). The auroral electron impact production rates are calculated using solar wind electron spectrum measured by the plasma spectrometer (PLASMAG) experiment onboard VEGA 2 spacecraft on March 11, 1986 (Gringauz et al, 1986;Haider et al, 1993).…”

Section: Calculation and Input Parametersmentioning

confidence: 99%

Radial distribution of production rates, loss rates and densities corresponding to ion masses ⩽40 amu in the inner coma of Comet Halley: Composition and chemistry

Haider

Bhardwaj

2005

Icarus

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Auroral and photoelectron fluxes in cometary ionospheres

Cited by 43 publications

References 48 publications

O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

Prediction of Forbidden Ultraviolet and Visible Emissions in Comet 67p/Churyumov–gerasimenko

Radial distribution of production rates, loss rates and densities corresponding to ion masses ⩽40 amu in the inner coma of Comet Halley: Composition and chemistry

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