Volume 435, Number 1, May III 2005
|Page(s)||341 - 351|
|Section||Planets and planetary systems|
|Published online||25 April 2005|
Metallic abundances of the 2002 Leonid meteor deduced from high-definition TV spectra
Department of Astronomical Science, School of Physical Science, The Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181–8588, Japan e-mail: firstname.lastname@example.org
2 National Astronomical Observatory of the Japan (NAOJ), National Institute of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181–8588, Japan e-mail: email@example.com
3 Institute of Low Temperature Science, Department of Earth and Planetary Sciences, Hokkaido University, Kita-19, Nishi-8, Kita-ku, Sapporo, Hokkaido 060–0819, Japan
4 Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464–8602, Japan e-mail: firstname.lastname@example.org
5 V-CAD High Speed Computer System Team, The Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351–0198, Japan e-mail: email@example.com
6 Gunma Astronomical Observatory, 6860-86 Nakayama, Takayama, Agatsuma, Gunma 377–0702, Japan e-mail: firstname.lastname@example.org
7 Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229–8510, Japan e-mail: email@example.com
Accepted: 28 December 2004
High-definition TV spectra in the ultraviolet–visible region were obtained during the 2002 Leonid aircraft campaign. We analyze the spectra of the brightest fireball that appeared at UT on Nov. 19, 2002 and identify the neutral atoms, mainly MgI, FeI, CaI, and NaI in the observed wavelengths between 300–650 nm. The singly ionized atomic emissions, CaII and MgII lines, also appeared in the spectrum in several epochs during the series of video frames. From analysis of the spectra, time variation in the abundances of metallic atoms, along with their electronic excitation and blackbody temperatures, were obtained assuming the Local Thermal Equilibrium (LTE) condition. Both Fe and Ca abundances relative to Mg are lower than the solar abundance, while Na is slightly higher. We found correlation between the excitation temperature and the abundance of Ca, which suggests incomplete evaporation of the Ca due to intrinsic refractoriness. A search for bands of CHON–related molecules, such as OH and CN, is not successful in the brightest fireball in this study.
Key words: meteors, meteroids
© ESO, 2005
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