Migrating Dust Particles
(2014) In Lund Observatory Examensarbeten ASTK01 20141Lund Observatory - Has been reorganised
Department of Astronomy and Theoretical Physics - Has been reorganised
- Abstract
- Where the dust in a protoplanetary disk is as the disk evolves over time is essential to know for further studies of the planet formation process. A new star is created alongside a stellar nebula. The nebula contains rock, ice and gas which are not accreted to the star. Our nebula is constructed using the Minimum Mass Solar Nebula model and the column density is studied as the protoplanetary disk evolves over time. The Minimum Mass Solar Nebula model takes the mass of dust from the planets we see today in our solar system and spreads it out between the planets. To estimate the gas column density, simply multiply by about a hundred.
The dust in a protoplanetary disk will feel a head wind from the more slowly orbiting gas and start to drift... (More) - Where the dust in a protoplanetary disk is as the disk evolves over time is essential to know for further studies of the planet formation process. A new star is created alongside a stellar nebula. The nebula contains rock, ice and gas which are not accreted to the star. Our nebula is constructed using the Minimum Mass Solar Nebula model and the column density is studied as the protoplanetary disk evolves over time. The Minimum Mass Solar Nebula model takes the mass of dust from the planets we see today in our solar system and spreads it out between the planets. To estimate the gas column density, simply multiply by about a hundred.
The dust in a protoplanetary disk will feel a head wind from the more slowly orbiting gas and start to drift towards the star. The ice particles sublime inside 2.7 AU as the temperature rises. A computer model is used here to simulate the changes in the column density over time. Micron-sized particles are simulated as they grow and drift towards the star. The ice-line at 2.7 AU results in a slight buildup of dust inside this radius. When a pebble grows it is due to how much dust it collides with and how much of it that sticks to the pebble. If the disk is less turbulent the pebbles grow slower due to fewer collisions and the column density changes more slowly. The same happens when the sticking factor is lowered. But with low turbulence (α = 10^(−4)) the disk becomes thinner and more dense, which can increase the growth somewhat. When the pebbles grow slowly there is a tendency for dust buildup when the drift speed decreases with orbital distance (for St < 1, St is a measurement of how particles behave in fluids). When the pebble density is closely varied around 2 g cm^(−3) no big difference in the column density is shown. One can only see that the disk shrinks slightly faster with heavier pebbles. (Less)
Please use this url to cite or link to this publication:
http://lup.lub.lu.se/student-papers/record/4530447
- author
- Eriksson, Joakim LU
- supervisor
- organization
- course
- ASTK01 20141
- year
- 2014
- type
- M2 - Bachelor Degree
- subject
- publication/series
- Lund Observatory Examensarbeten
- report number
- 2014-EXA87
- language
- English
- id
- 4530447
- date added to LUP
- 2014-07-04 11:57:27
- date last changed
- 2014-07-04 11:57:27
@misc{4530447,
abstract = {{Where the dust in a protoplanetary disk is as the disk evolves over time is essential to know for further studies of the planet formation process. A new star is created alongside a stellar nebula. The nebula contains rock, ice and gas which are not accreted to the star. Our nebula is constructed using the Minimum Mass Solar Nebula model and the column density is studied as the protoplanetary disk evolves over time. The Minimum Mass Solar Nebula model takes the mass of dust from the planets we see today in our solar system and spreads it out between the planets. To estimate the gas column density, simply multiply by about a hundred.
The dust in a protoplanetary disk will feel a head wind from the more slowly orbiting gas and start to drift towards the star. The ice particles sublime inside 2.7 AU as the temperature rises. A computer model is used here to simulate the changes in the column density over time. Micron-sized particles are simulated as they grow and drift towards the star. The ice-line at 2.7 AU results in a slight buildup of dust inside this radius. When a pebble grows it is due to how much dust it collides with and how much of it that sticks to the pebble. If the disk is less turbulent the pebbles grow slower due to fewer collisions and the column density changes more slowly. The same happens when the sticking factor is lowered. But with low turbulence (α = 10^(−4)) the disk becomes thinner and more dense, which can increase the growth somewhat. When the pebbles grow slowly there is a tendency for dust buildup when the drift speed decreases with orbital distance (for St < 1, St is a measurement of how particles behave in fluids). When the pebble density is closely varied around 2 g cm^(−3) no big difference in the column density is shown. One can only see that the disk shrinks slightly faster with heavier pebbles.}},
author = {{Eriksson, Joakim}},
language = {{eng}},
note = {{Student Paper}},
series = {{Lund Observatory Examensarbeten}},
title = {{Migrating Dust Particles}},
year = {{2014}},
}