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Material properties of transition objects 3200 Phaethon and 2003 EH1

Published online by Cambridge University Press:  06 April 2010

J. Borovička ,
P. Koten ,
P. Spurný ,
D. Čapek ,
L. Shrbený  and
R. Štork
J. Borovička
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
P. Koten
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
P. Spurný
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
D. Čapek
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
L. Shrbený
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
R. Štork
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: borovic@asu.cas.cz
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Abstract

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Asteroids 3200 Phaethon and 196256 (2003 EH1) are connected with two major meteoroid streams, Geminids and Quadrantids, respectively. We have modeled the observed light curves and decelerations of Geminid and Quadrantid meteors and studied their spectra. In both cases, we have found typical bulk densities of about 2600 kg m−3, much larger than in cometary meteoroids. Sodium was partially lost from Geminids and Quadrantids due to solar heating. The Quadrantid material was therefore not hidden deep inside the parent body 1500 years ago, when the perihelion was low enough for sodium loss to occur.

Keywords

meteorsmeteoroidsminor planetsasteroids
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 218 - 222
Copyright
Copyright © International Astronomical Union 2010

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