The role of ice in planet formation
(2024)- Abstract
- As stars form, they are surrounded by a disc composed of gas, dust and ice – the protoplanetary disc, where solids grow from micrometre-sized dust to planets. Small dust grows readily by collisions. However, it is challenging to reach high enough particle sizes and dust-to-gas-ratios for continued growth to planetesimals – kilometre-sized and larger planetary building blocks. In this thesis I explore the effect of ice on the growth towards pebbles, in order to investigate if the water ice line – the radial distance from the star where water undergoes a phase change from
vapour to solid form – can be a favourable location for the initiation of growth towards planetesimals. In a series of papers, I numerically and experimentally... (More) - As stars form, they are surrounded by a disc composed of gas, dust and ice – the protoplanetary disc, where solids grow from micrometre-sized dust to planets. Small dust grows readily by collisions. However, it is challenging to reach high enough particle sizes and dust-to-gas-ratios for continued growth to planetesimals – kilometre-sized and larger planetary building blocks. In this thesis I explore the effect of ice on the growth towards pebbles, in order to investigate if the water ice line – the radial distance from the star where water undergoes a phase change from
vapour to solid form – can be a favourable location for the initiation of growth towards planetesimals. In a series of papers, I numerically and experimentally investigate condensation and sublimation at the water ice line. I find that micrometre-sized dust particles can grow quickly to icy pebbles through condensation. This confirms that the water ice line can be a favourable location for further growth towards planetesimals and planets. (Less) - Abstract (Swedish)
- När stjärnor bildas omges de av en skiva bestående av gas, stoft och is. Detta är den protoplanetära skivan där de fasta beståndsdelarna växer från mikrometerstora dammpartiklar till planeter. Små stoftpartiklar kan växa genom kollisioner, men att nå tillräckliga partikelstorlekar och tillräckligt hög partikelkoncentration är utmanande. I denna avhandling undersöker jag om den så kallade islinjen – avståndet från stjärnan där vattenånga övergår till is - kan bidra till gynnsamma förhållanden för planetbildning. Genom numeriska simulationer och laboratorieexperiment undersöker jag kondensation och sublimering av vatten vid islinjen. Resultaten visar att mikrometerstora stoftpartiklar snabbt kan växa till centimeterstora isiga partiklar... (More)
- När stjärnor bildas omges de av en skiva bestående av gas, stoft och is. Detta är den protoplanetära skivan där de fasta beståndsdelarna växer från mikrometerstora dammpartiklar till planeter. Små stoftpartiklar kan växa genom kollisioner, men att nå tillräckliga partikelstorlekar och tillräckligt hög partikelkoncentration är utmanande. I denna avhandling undersöker jag om den så kallade islinjen – avståndet från stjärnan där vattenånga övergår till is - kan bidra till gynnsamma förhållanden för planetbildning. Genom numeriska simulationer och laboratorieexperiment undersöker jag kondensation och sublimering av vatten vid islinjen. Resultaten visar att mikrometerstora stoftpartiklar snabbt kan växa till centimeterstora isiga partiklar genom kondensation. Detta bekräftar att islinjen kan vara en gynnsam plats där planetbildning kan initieras. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/3a96c556-35d2-4b21-82e8-50921a03e9a1
- author
- Ros, Katrin LU
- supervisor
-
- Anders Johansen LU
- Nils Ryde LU
- opponent
-
- Dr. Krijt, Sebastian, University of Exeter
- organization
- publishing date
- 2024
- type
- Thesis
- publication status
- published
- subject
- keywords
- Planetbildning, Protoplanetära skivor, Planet formation, Protoplanetary discs
- pages
- 110 pages
- publisher
- Lund University
- defense location
- Lundmarksalen, Sölvegatan 27, Lund.
- defense date
- 2024-04-26 13:00:00
- ISBN
- 978-91-8104-020-3
- 978-91-8104-019-7
- language
- English
- LU publication?
- yes
- id
- 3a96c556-35d2-4b21-82e8-50921a03e9a1
- date added to LUP
- 2024-04-02 14:36:09
- date last changed
- 2024-04-03 12:01:31
@phdthesis{3a96c556-35d2-4b21-82e8-50921a03e9a1,
abstract = {{As stars form, they are surrounded by a disc composed of gas, dust and ice – the protoplanetary disc, where solids grow from micrometre-sized dust to planets. Small dust grows readily by collisions. However, it is challenging to reach high enough particle sizes and dust-to-gas-ratios for continued growth to planetesimals – kilometre-sized and larger planetary building blocks. In this thesis I explore the effect of ice on the growth towards pebbles, in order to investigate if the water ice line – the radial distance from the star where water undergoes a phase change from<br/>vapour to solid form – can be a favourable location for the initiation of growth towards planetesimals. In a series of papers, I numerically and experimentally investigate condensation and sublimation at the water ice line. I find that micrometre-sized dust particles can grow quickly to icy pebbles through condensation. This confirms that the water ice line can be a favourable location for further growth towards planetesimals and planets.}},
author = {{Ros, Katrin}},
isbn = {{978-91-8104-020-3}},
keywords = {{Planetbildning; Protoplanetära skivor; Planet formation; Protoplanetary discs}},
language = {{eng}},
publisher = {{Lund University}},
school = {{Lund University}},
title = {{The role of ice in planet formation}},
url = {{https://lup.lub.lu.se/search/files/178506716/Avhandling_Katrin_Ros_utan_papers_till_Lucris.pdf}},
year = {{2024}},
}