Laboratory spectra of hot water and methane for modeling late-type stars and brown dwarfs

R  Nassar; P  Bernath

Laboratory spectra of hot water and methane for modeling late-type stars and brown dwarfs

Chemistry

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

Absorption bands from water and methane are prominent in the infrared spectra of many late-type stars and brown dwarfs, and are expected to be observed in the infrared spectra of hot extrasolar giant planets. In a continuing project, laboratory high resolution Fourier transform spectra of water emission were recorded from 40013,000 cm(-1) using two sources, a tube furnace at 1800 K and an oxyacetylene torch at 3000 K. These spectra have been used for the identification of water lines in sunspots. We have also recorded laboratory high resolution Fourier transform spectra of methane emission using a tube furnace at 1273, 1000, and 800 K, spanning the region of 2000-6400 cm(-1). Spectra of water and methane at high temperatures differ significantly from room temperature spectra; therefore, modelers have shown an interest in our laboratory data for interpreting the spectra of late-type stars and brown dwarfs, and modeling the atmospheres of hot extrasolar giant planets.

Original language	English
Title of host publication	CHEMISTRY AS A DIAGNOSTIC OF STAR FORMATION
Place of Publication	OTTAWA
Publisher	NATL RESEARCH COUNCIL CANADA
Pages	366-367
Number of pages	2
ISBN (Print)	0-660-19089-3
Publication status	Published - 2003

Keywords

stars : low-mass, brown dwarfs
infrared : stars
molecular data
methods : laboratory
techniques : spectroscopic
SPECTROSCOPY
SUNSPOT

Cite this

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title = "Laboratory spectra of hot water and methane for modeling late-type stars and brown dwarfs",

abstract = "Absorption bands from water and methane are prominent in the infrared spectra of many late-type stars and brown dwarfs, and are expected to be observed in the infrared spectra of hot extrasolar giant planets. In a continuing project, laboratory high resolution Fourier transform spectra of water emission were recorded from 40013,000 cm(-1) using two sources, a tube furnace at 1800 K and an oxyacetylene torch at 3000 K. These spectra have been used for the identification of water lines in sunspots. We have also recorded laboratory high resolution Fourier transform spectra of methane emission using a tube furnace at 1273, 1000, and 800 K, spanning the region of 2000-6400 cm(-1). Spectra of water and methane at high temperatures differ significantly from room temperature spectra; therefore, modelers have shown an interest in our laboratory data for interpreting the spectra of late-type stars and brown dwarfs, and modeling the atmospheres of hot extrasolar giant planets.",

keywords = "stars : low-mass, brown dwarfs, infrared : stars, molecular data, methods : laboratory, techniques : spectroscopic, SPECTROSCOPY, SUNSPOT",

author = "R Nassar and P Bernath",

year = "2003",

language = "English",

isbn = "0-660-19089-3",

pages = "366--367",

booktitle = "CHEMISTRY AS A DIAGNOSTIC OF STAR FORMATION",

publisher = "NATL RESEARCH COUNCIL CANADA",

}

TY - GEN

T1 - Laboratory spectra of hot water and methane for modeling late-type stars and brown dwarfs

AU - Nassar, R

AU - Bernath, P

PY - 2003

Y1 - 2003

N2 - Absorption bands from water and methane are prominent in the infrared spectra of many late-type stars and brown dwarfs, and are expected to be observed in the infrared spectra of hot extrasolar giant planets. In a continuing project, laboratory high resolution Fourier transform spectra of water emission were recorded from 40013,000 cm(-1) using two sources, a tube furnace at 1800 K and an oxyacetylene torch at 3000 K. These spectra have been used for the identification of water lines in sunspots. We have also recorded laboratory high resolution Fourier transform spectra of methane emission using a tube furnace at 1273, 1000, and 800 K, spanning the region of 2000-6400 cm(-1). Spectra of water and methane at high temperatures differ significantly from room temperature spectra; therefore, modelers have shown an interest in our laboratory data for interpreting the spectra of late-type stars and brown dwarfs, and modeling the atmospheres of hot extrasolar giant planets.

AB - Absorption bands from water and methane are prominent in the infrared spectra of many late-type stars and brown dwarfs, and are expected to be observed in the infrared spectra of hot extrasolar giant planets. In a continuing project, laboratory high resolution Fourier transform spectra of water emission were recorded from 40013,000 cm(-1) using two sources, a tube furnace at 1800 K and an oxyacetylene torch at 3000 K. These spectra have been used for the identification of water lines in sunspots. We have also recorded laboratory high resolution Fourier transform spectra of methane emission using a tube furnace at 1273, 1000, and 800 K, spanning the region of 2000-6400 cm(-1). Spectra of water and methane at high temperatures differ significantly from room temperature spectra; therefore, modelers have shown an interest in our laboratory data for interpreting the spectra of late-type stars and brown dwarfs, and modeling the atmospheres of hot extrasolar giant planets.

KW - stars : low-mass, brown dwarfs

KW - infrared : stars

KW - molecular data

KW - methods : laboratory

KW - techniques : spectroscopic

KW - SPECTROSCOPY

KW - SUNSPOT

M3 - Conference contribution

SN - 0-660-19089-3

SP - 366

EP - 367

BT - CHEMISTRY AS A DIAGNOSTIC OF STAR FORMATION

PB - NATL RESEARCH COUNCIL CANADA

CY - OTTAWA

ER -