Meteor Outburst Profiles and Cometary Ejection Models |
| |
| Authors: | D J Asher |
| |
| Institution: | (1) Armagh Observatory, College Hill, Armagh, BT61 9DG, UK |
| |
| Abstract: | The spatial structure of meteor streams, and the activity profiles of their corresponding meteor showers, depend firstly on
the distribution of meteoroid orbits soon after ejection from the parent comet nucleus, and secondly on the subsequent dynamical
evolution. The latter increases in importance as more time elapses. For younger structures within streams, notably the dust
trails that cause sharp meteor outbursts, it is the cometary ejection model (meteoroid production rate as a function of time
through the several months of the comet’s perihelion return, and velocity distribution of the meteoroids released) that primarily
determines the shape and width of the trail structure. This paper describes how a trail cross section can be calculated once
an ejection model has been assumed. Such calculations, if made for a range of ejection model parameters and compared with
observed parameters of storms and outbursts, can be used to constrain quantitatively the process of meteoroid ejection from
the nucleus, including the mass distribution of ejected meteoroids. |
| |
| Keywords: | Celestial mechanics Comets Dust trails Leonids Meteor outbursts Meteor streams |
| 本文献已被 SpringerLink 等数据库收录！ |
|
