New upper limits for atmospheric constituents on Io

Uwe Fink; Harold P. Larson; Thomas N. Gautier

doi:10.1016/0019-1035(76)90022-1

New upper limits for atmospheric constituents on Io

Uwe Fink, Harold P. Larson, Thomas N. Gautier

Lunar and Planetary Lab

Research output: Contribution to journal › Article › peer-review

13 Scopus citations

Abstract

A spectrum of the satellite of Jupiter, Io, from 0.86 to 2.7 μm at a resolution of 3.36 cm^-1 and a signal to rms noise ratio of 120 is presented. No absorptions due to any atmospheric constituents on Io could be found on the spectrum. Upper limits of 0.12 cm-atm for NH₃, 0.12cm-atm for CH₄, 0.4cm-atm for N₂O, and 24cm-atm for H₂S were determined. Laboratory spectra of ammonia frosts as a function of temperature were compared with the spectrum of Io and showed as a frost not to be present at the surface of Io. A search for possible resonance lines of carbon, silicon, and sulfur as well as the 1.08μm line of helium proved negative and upper emission limits of 60, 18, 27, and 60 kilorayleighs, respectively, were established for these lines.

Original language	English (US)
Pages (from-to)	439-446
Number of pages	8
Journal	Icarus
Volume	27
Issue number	3
DOIs	https://doi.org/10.1016/0019-1035(76)90022-1
State	Published - Mar 1976

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1016/0019-1035(76)90022-1

Fingerprint Dive into the research topics of 'New upper limits for atmospheric constituents on Io'. Together they form a unique fingerprint.

Cite this

@article{cc1f728d3f6c4042af5a21695780a3e2,

title = "New upper limits for atmospheric constituents on Io",

abstract = "A spectrum of the satellite of Jupiter, Io, from 0.86 to 2.7 μm at a resolution of 3.36 cm-1 and a signal to rms noise ratio of 120 is presented. No absorptions due to any atmospheric constituents on Io could be found on the spectrum. Upper limits of 0.12 cm-atm for NH3, 0.12cm-atm for CH4, 0.4cm-atm for N2O, and 24cm-atm for H2S were determined. Laboratory spectra of ammonia frosts as a function of temperature were compared with the spectrum of Io and showed as a frost not to be present at the surface of Io. A search for possible resonance lines of carbon, silicon, and sulfur as well as the 1.08μm line of helium proved negative and upper emission limits of 60, 18, 27, and 60 kilorayleighs, respectively, were established for these lines.",

author = "Uwe Fink and Larson, {Harold P.} and Gautier, {Thomas N.}",

note = "Funding Information: We would like to thank W. M. Sinton for helpful discussion and comparison of his 10 spectrum with ours. We also thank K. Aksnes for providing us with precise coordinates for 10 so that 10 could be tracked during daytime. This research was supported by NASA Grant NSG 7070.",

year = "1976",

month = mar,

doi = "10.1016/0019-1035(76)90022-1",

language = "English (US)",

volume = "27",

pages = "439--446",

journal = "Icarus",

issn = "0019-1035",

publisher = "Academic Press Inc.",

number = "3",

}

TY - JOUR

T1 - New upper limits for atmospheric constituents on Io

AU - Fink, Uwe

AU - Larson, Harold P.

AU - Gautier, Thomas N.

N1 - Funding Information: We would like to thank W. M. Sinton for helpful discussion and comparison of his 10 spectrum with ours. We also thank K. Aksnes for providing us with precise coordinates for 10 so that 10 could be tracked during daytime. This research was supported by NASA Grant NSG 7070.

PY - 1976/3

Y1 - 1976/3

N2 - A spectrum of the satellite of Jupiter, Io, from 0.86 to 2.7 μm at a resolution of 3.36 cm-1 and a signal to rms noise ratio of 120 is presented. No absorptions due to any atmospheric constituents on Io could be found on the spectrum. Upper limits of 0.12 cm-atm for NH3, 0.12cm-atm for CH4, 0.4cm-atm for N2O, and 24cm-atm for H2S were determined. Laboratory spectra of ammonia frosts as a function of temperature were compared with the spectrum of Io and showed as a frost not to be present at the surface of Io. A search for possible resonance lines of carbon, silicon, and sulfur as well as the 1.08μm line of helium proved negative and upper emission limits of 60, 18, 27, and 60 kilorayleighs, respectively, were established for these lines.

AB - A spectrum of the satellite of Jupiter, Io, from 0.86 to 2.7 μm at a resolution of 3.36 cm-1 and a signal to rms noise ratio of 120 is presented. No absorptions due to any atmospheric constituents on Io could be found on the spectrum. Upper limits of 0.12 cm-atm for NH3, 0.12cm-atm for CH4, 0.4cm-atm for N2O, and 24cm-atm for H2S were determined. Laboratory spectra of ammonia frosts as a function of temperature were compared with the spectrum of Io and showed as a frost not to be present at the surface of Io. A search for possible resonance lines of carbon, silicon, and sulfur as well as the 1.08μm line of helium proved negative and upper emission limits of 60, 18, 27, and 60 kilorayleighs, respectively, were established for these lines.

UR - http://www.scopus.com/inward/record.url?scp=49549130881&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=49549130881&partnerID=8YFLogxK

U2 - 10.1016/0019-1035(76)90022-1

DO - 10.1016/0019-1035(76)90022-1

M3 - Article

AN - SCOPUS:49549130881

VL - 27

SP - 439

EP - 446

JO - Icarus

JF - Icarus

SN - 0019-1035

IS - 3

ER -