Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data
Some results of study for high-resolution spectra of Jupiter and Saturn atmospheres are presented. The spectral data are derived with the help of the coude echelle spectrometer installed on the 2-m telescope at the Terskol Observatory (the Northern Caucasus). The investigations are carried out with...
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| Дата: | 2005 |
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Головна астрономічна обсерваторія НАН України
2005
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| Назва видання: | Кинематика и физика небесных тел |
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| Цитувати: | Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data / Yu.G. Kuznyetsova, A.P. Vid'machenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 480-482. — Бібліогр.: 5 назв. — англ. |
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nasplib_isofts_kiev_ua-123456789-797032025-02-10T01:08:22Z Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data Kuznyetsova, Yu.G. Vid'machenko, A.P. MS5: Dynamics and Physics of Solar System Bodies Some results of study for high-resolution spectra of Jupiter and Saturn atmospheres are presented. The spectral data are derived with the help of the coude echelle spectrometer installed on the 2-m telescope at the Terskol Observatory (the Northern Caucasus). The investigations are carried out with consideration for Raman light scattering. Calculations for molecular scattering effect in the atmospheres of giant planets are made for visible part of the spectrum. Wavelengths of Fraunhofer lines and their strongest ghosts caused by the rotational S(0), S(1), O(2) and the vibrational Q₁(1) transitions are used. 2005 Article Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data / Yu.G. Kuznyetsova, A.P. Vid'machenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 480-482. — Бібліогр.: 5 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79703 en Кинематика и физика небесных тел application/pdf Головна астрономічна обсерваторія НАН України |
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English |
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MS5: Dynamics and Physics of Solar System Bodies MS5: Dynamics and Physics of Solar System Bodies |
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MS5: Dynamics and Physics of Solar System Bodies MS5: Dynamics and Physics of Solar System Bodies Kuznyetsova, Yu.G. Vid'machenko, A.P. Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data Кинематика и физика небесных тел |
| description |
Some results of study for high-resolution spectra of Jupiter and Saturn atmospheres are presented. The spectral data are derived with the help of the coude echelle spectrometer installed on the 2-m telescope at the Terskol Observatory (the Northern Caucasus). The investigations are carried out with consideration for Raman light scattering. Calculations for molecular scattering effect in the atmospheres of giant planets are made for visible part of the spectrum. Wavelengths of Fraunhofer lines and their strongest ghosts caused by the rotational S(0), S(1), O(2) and the vibrational Q₁(1) transitions are used. |
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Article |
| author |
Kuznyetsova, Yu.G. Vid'machenko, A.P. |
| author_facet |
Kuznyetsova, Yu.G. Vid'machenko, A.P. |
| author_sort |
Kuznyetsova, Yu.G. |
| title |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data |
| title_short |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data |
| title_full |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data |
| title_fullStr |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data |
| title_full_unstemmed |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data |
| title_sort |
raman scattering effect in atmospheres of giant planets of the solar system from high-resolution spectral data |
| publisher |
Головна астрономічна обсерваторія НАН України |
| publishDate |
2005 |
| topic_facet |
MS5: Dynamics and Physics of Solar System Bodies |
| url |
https://nasplib.isofts.kiev.ua/handle/123456789/79703 |
| citation_txt |
Raman scattering effect in atmospheres of giant planets of the Solar System from high-resolution spectral data / Yu.G. Kuznyetsova, A.P. Vid'machenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 480-482. — Бібліогр.: 5 назв. — англ. |
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Кинематика и физика небесных тел |
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2025-12-02T09:40:18Z |
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| fulltext |
RAMAN SCATTERING EFFECT IN ATMOSPHERES OF GIANT PLANETS
OF THE SOLAR SYSTEM FROM HIGH-RESOLUTION SPECTRAL DATA
Yu. G. Kuznyetsova, A. P. Vid’machenko
Main Astronomical Observatory, NAS of Ukraine
27 Akademika Zabolotnoho Str., 03680 Kyiv, Ukraine
e-mail: juliana@mao.kiev.ua
Some results of study for high-resolution spectra of Jupiter and Saturn atmospheres are pre-
sented. The spectral data are derived with the help of the coude echelle spectrometer installed
on the 2-m telescope at the Terskol Observatory (the Northern Caucasus). The investigations are
carried out with consideration for Raman light scattering. Calculations for molecular scattering
effect in the atmospheres of giant planets are made for visible part of the spectrum. Wavelengths
of Fraunhofer lines and their strongest ghosts caused by the rotational S(0), S(1), O(2) and the vi-
brational Q1(1) transitions are used.
INTRODUCTION
During a molecular scattering process, the photon may loose energy according to certain molecular transitions.
Theoretical description of Raman scattering is presented by Cochran and Trafton [1]. Raman scattering causes
emission features in the planetary albedo spectrum at each solar line and several absorption features, Raman
“ghosts”, longward of each solar line. The emission features at solar lines are quite obvious in the ultraviolet.
Because of the multitude of solar lines, emission and absorption features superposed at almost every wavelength.
Usually, Raman scattering is considered for three major hydrogen transitions, the rotational S(0) and S(1) as
well as the vibrational Q1(1) transitions, which produce significant Raman ghosts. Raman scattering due
to all other transitions, including multiple Raman scattering, is too small to be observable by their ghosts,
but their combined effect may significantly increase the emission features. The corresponding emission peaks
in the planetary spectra are easily visible and accurately measurable. This provides the amount of Raman
scattering due to all transitions combined [2].
OBSERVATIONS
The spectra presented were obtained with the use of 1024×1024 pixel CCD-matrix in the coude echelle spec-
trometer of the 2-m telescope of the Terskol Observatory (the Northern Caucasus) on March 11 and 13, 2001.
Optical scheme of the coude echelle spectrometer is described in [5]. We obtained four separate data sets:
one for the Jovian equatorial region, one for the Jovian north equatorial band, one for the Saturnian equatorial
region, and one for the Saturnian north polar cap. To take into account contribution of solar spectrum to planet
spectra, we used observational data for the Sun analogue HD89010 (35 Leo). Parameters of objects at the ob-
servation moment are listed in Table 1. Technical characteristics of observation apparatus and the procedure
used for data processing are described in [3].
Table 1. Observational characteristics of objects
Object Magnitude Exposure, s Signal-to-noise ratio
Jupiter −2.2 300 200
Saturn 0.2 900 100
35 Leo 5.9 3600 185
c© Yu. G. Kuznyetsova, A. P. Vid’machenko, 2004
480
RESULTS
The aims of our investigations are:
1. To detect the presence of Raman scattering by H2 in the atmospheres of Jupiter and Saturn using spectra
of these planets.
2. To find values of the relative contribution of Raman light scattering to separate morphological details of
Jovian and Saturnian discs.
We consider the spectral region from 3938 Å to 8743 Å. Unfortunately, the solar line Ca II K is located out
of this spectral region. An example of the primary Saturnian equatorial region spectrum in the vicinity
of the solar Ca II H line is presented in Fig. 1.
Figure 1. Saturnian equatorial region spectrum in the vicinity of the solar Ca II H line
On subtracting the solar contribution from the planet spectra with the help of a spectrum of the Sun analog
35 Leo, numerous pseudoemission peaks were detected in the obtained planet spectra. This is evidence of
Raman light scattering presence in the Jovian and Saturnian atmospheres. Figure 2 shows a small part of
the resulting spectrum of the Jovian equatorial region including the Ca II H line. The lower half of the figure
displays the spectrum, while the upper half shows the Jupiter / 35 Leo ratio spectrum. The ratio spectrum
has a peak arising as a result of Raman scattering of photons. Well visible Stoks ghosts are detected for both
lines Ca II H and K but are more significant for hydrogen transitions, namely, S(0) and S(1) corresponding to
354 and 587 cm−1 removals. Further, we find the values of relative contribution of Raman light scattering for
Jupiter and Saturn using pseudoemission peak in the field of the Ca II H line. It is made by means of division of
light field spectrum by the dark field spectrum for single planet disc. It is noted that, for giant planets, aerosol
layer in dark fields is located lower than in light fields. Accordingly, in the dark fields, there is a larger quantity
of gas (H2) and a larger contribution of Raman light scattering takes place than in the light fields. This fact
is confirmed by obtained values of relative contribution of Raman light scattering to spectra of Jupiter and
Saturn. The above-mentioned values are presented in Table 2.
Table 2. Values of relative contribution of Raman light scattering to spectra of Jupiter and Saturn
Object Light field / dark field Relative contribution of Raman
light scattering, percent
Jupiter equatorial region / north equatorial band 7.6
Saturn equatorial region / north polar cap 39.0
481
Figure 2. A small part of the resulting spectrum of the Jovian equatorial region in the vicinity of the Ca II H solar line.
The lower half of the figure displays the spectrum, while the upper half shows Jupiter / 35 Leo ratio spectrum
Our calculations of absolute values of Raman light scattering contribution to spectra of separate morpho-
logical details of the Jovian and Saturnian discs are made with the help of Morozhenko’s methods [4].
[1] Cochran W. D., Trafton L. M., et al. Raman scattering in the atmospheres of the major planets // Astrophys. J.–
1978.–219.–P. 756–762.
[2] Karkoschka E. Spectrophotometry of the Jovian Planets and Titan at 300- to 1000-nm wavelength: the methane
spectrum // Icarus.–1994.–111, N 1.–P. 174–192.
[3] Kuznyetsova Y. G., Bondar A. V. The results of extensive object observations obtained with aid of coude echelle
spectrometer fed by the 2-m telescope at the Terskol Observatory (Northern Caucasus) // J. Phys. Studies.–2002.–6,
N 4.–P. 411–413.
[4] Morozhenko A. V. Raman scattering in the atmospheres of giant planets and optical properties of atmospheric
aerosol // Kinematics and Physics of Celestial Bodies.–1997.–13, N 4.–P. 22–33.
[5] Musaev F. A., Galazutdinov G. A., Sergeev A. V., et al. Coude echelle spectrometer for the Terskol 2-meter
telescope // Kinematics and Physics of Celestial Bodies.–1999.–15, N 3.–P. 282–287.
482
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