Astronomy and Astrophysics – Astrophysics – Earth and Planetary Astrophysics
Scientific paper
2010-09-29
Astronomy and Astrophysics
Astrophysics
Earth and Planetary Astrophysics
6 pages, 1 table
Scientific paper
Orbital evolution of spherical interplanetary dust particles in the Edgeworth-Kuiper belt zone is treated for semimajor axes 30-50 AU. Besides solar gravity, also solar electromagnetic and corpuscular radiation, and, fast interstellar gas flow are important forces influencing motion of the particles. The solar electromagnetic radiation is represented by the Poynting-Robertson effect and the solar corpuscular radiation corresponds to the solar wind. Time-variability of the non-radial solar wind can significantly increase dust lifetime in the zone. The average time for the particle stay in the zone is more than 30-times greater than the conventional case of constant (time independent) radial solar wind offers, for the particles of tens micrometers in size. This holds for the most realistic material properties of the particles: $\bar{Q}'_{pr} =$ 1, where $\bar{Q}'_{pr}$ is the dimensionless efficiency factor for electromagnetic radiation pressure. If $\bar{Q}'_{pr} =$ 1/2, then the average time of the particle stay in the zone is only 4-times the conventional value. The approach used in the paper illustrates the relevance of the solar wind action in comparison with the Poynting-Robertson effect. The results have an important consequence for our understanding of the structure of dust distribution in the Edgeworth-Kuiper belt zone, and, also, of dust belts in other stellar systems.
Klacka Jozef
Komar Ladislav
Pastor P.
No associations
LandOfFree
Dust in the Edgeworth-Kuiper belt zone does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Dust in the Edgeworth-Kuiper belt zone, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Dust in the Edgeworth-Kuiper belt zone will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-523611