The Open UniversitySkip to content
 

Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity

Pagomenos, George (2019). Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity. PhD thesis The Open University.

Full text available as:
[img]
Preview
PDF (Version of Record) - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (12MB) | Preview
URL: https://drive.google.com/file/d/1wKDTzpp87LQPAbsS0...
Google Scholar: Look up in Google Scholar

Abstract

Planetary nebulae are the final phases of evolution for low- to intermediate-mass stars (∼ 0.8– 8 M⊙). They consist of a central star surrounded predominantly by a circumstellar envelope containing the products of nuclear processing, and a photodissociation region containing dust and molecules. These include silicates and large organic molecules such as polycyclic aromatic hydrocarbons (PAHs), which are ubiquitous throughout the Universe, and fullerenes, which are the largest molecules to be firmly detected in space. All of this material coasts away from the central star, causing enrichment of the interstellar medium.

Although there have been significant advances in studies of this circumstellar material, we still do not fully understand how the metallicity (i.e. the abundance of elements heavier than helium) of the local environment affects the dust composition around these stars, or the processes that govern the formation and evolution of these large organic molecules.

This thesis presents a series of studies in which the abundances and dust composition around planetary nebulae are characterised in the low metallicity regions of the Milky Way, with use of data from the Spitzer Space Telescope and SOFIA. These include investigations into the metallicity and dust content of planetary nebulae in the outer thin disk and the halo of the Galaxy, and the physical conditions in which large organic molecules form.

I find that the outer regions of the Galactic disk have a lower metallicity than the solar neighbourhood, and that regions of low metallicity favour carbon-rich dust production over oxygen-rich dust (i.e. silicates), except for within the Galactic halo. These regions show a greater diversity of carbonaceous material than observed towards the Galactic bulge and in the solar neighbourhood. Fullerenes are preferentially formed in environments with low hydrogen density.

Item Type: Thesis (PhD)
Copyright Holders: 2018 The Author
Project Funding Details:
Funded Project NameProject IDFunding Body
FEASTFUL, FP7 CIG grant630861European Comission
Keywords: astronomy; astrochemistry; planetary nebulae; dust; fullerenes; PAHs; anti-centre; Galactic; Spitzer; SOFIA; spectroscopy
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM)
Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Research Group: Astronomy
Space
Item ID: 58530
Depositing User: George Pagomenos
Date Deposited: 08 Jan 2019 17:04
Last Modified: 19 Nov 2019 22:09
URI: http://oro.open.ac.uk/id/eprint/58530
Share this page:

Download history for this item

These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.

Actions (login may be required)

Policies | Disclaimer

© The Open University   contact the OU