Ewch i’r prif gynnwys
Freeke van de Voort

Dr Freeke van de Voort

(hi/ei)

Uwch Ddarlithydd
STFC Ernest Rutherford Cymrawd
Grŵp Seryddiaeth
Canolfan Caerdydd ar gyfer Ymchwil a Thechnoleg Astroffiseg

Ysgol Ffiseg a Seryddiaeth

Users
Ar gael fel goruchwyliwr ôl-raddedig

Trosolwyg

Ym mis Mawrth 2020 dechreuais ym Mhrifysgol Caerdydd fel Cymrawd Ymchwil a darlithydd Prifysgol y Gymdeithas Frenhinol a chefais fy nyrchafu yn uwch ddarlithydd yn 2023. I'r rhai ohonoch sy'n pendroni: mae fy enw cyntaf yn cael ei ynganu yn debyg i Frey-ka ac mae fy enw olaf yn golygu "o'r Ford", a dyna pam mae'r pwyslais ar "Voort" ac nid ar "fan". Cyn hynny, gweithiais yn MPA fel ymchwilydd ôl-ddoethurol, yn HITS ac Iâl fel cymrawd Tschira, ac yn UC Berkeley ac Academia Sinica fel cymrawd TAC-ASIAA. Derbyniais fy PhD o Brifysgol Leiden yn 2012.

Mae fy ymchwil yn canolbwyntio ar yr astudiaeth o ffurfio galaethau yr wyf yn gyffredinol yn defnyddio efelychiadau cosmolegol, magnetohydrodynamig. Mae gen i ddiddordeb yn esblygiad galaethau a'r cyfrwng amgylchynol a rhyng-galasig. Rwy'n astudio'r llif nwy rhwng y gwahanol ranbarthau hyn a sut mae eu heiddo yn newid pan fyddwn yn cynnwys modelau newydd yn ein efelychiadau. Rwyf hefyd yn mwynhau gweithio ar effaith ffurfio galaethau a mewnlifiadau cosmolegol ar ddosbarthu elfennau trwm ledled y bydysawd.

Cyhoeddiad

2024

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2010

Adrannau llyfrau

Erthyglau

Ymchwil

Galaxy formation

My research focuses on understanding galaxy formation and evolution. For this purpose, I primarily use cosmological, (magneto)hydrodynamical simulations, but I have worked with observational data as well. I study the interplay between gas accretion and feedback and thus how galaxies grow. Within this field of research, I have worked on a range of topics (see also my publications). Below I describe the two areas to which I am currently devoting most of my time.

Circumgalactic medium

Galaxies are intimately connected to the environments they live in. The gaseous haloes arounds galaxies, the circumgalactic medium, is both the reservoir of gas that provides the fuel for galaxy growth and the repository of enriched gas expelled from galaxies by galactic outflows. Most cosmological, hydrodynamical simulations focus their computational effort on the galaxies themselves and treat the CGM more coarsely, which means small-scale structure cannot be resolved. We have therefore developed a new technique that adds uniform spatial refinement within the halo, increasing the resolution by 2 orders of magnitude for without a prohibitive increase in computational cost (van de Voort et al. 2019). The improved spatial resolution results in smaller dense clumps and more pronounced underdensities. It does not impact the central galaxy or the average density of the CGM. However, it drastically changes the radial profile of the neutral hydrogen column density. Simulating the circumgalactic medium accurately is vital for correctly interpreting at least some of its observational properties. I am currently exploring physical processes such as magnetic field in a new suite of simulations. These topics are still only the tip of the iceberg for what can be studied with these groundbreaking simulations, so stay tuned or feel free to contact me if you would like to get involved.

Chemical evolution

The flow of gas throughout cosmic time is responsible for setting the elemental abundances in present-day stars, together with the elemental yields from various production sites. Stellar abundances observed in the present-day universe (e.g. in the Milky Way and its satellites) can therefore be used to probe the metal production sites as well as the distribution and mixing of these metals throughout the universe at earlier times. Observations have revealed a large spread in rapid neutron capture (r-process) elements at low metallicity as well as striking differences between Milky Way satellites. To help figure out the origin of these elements, we have added 10 r-process production models to high-resolution simulations of Milky Way-like galaxies (van de Voort et al. 2020). Current (sparse and potentially biased) observations of metal-poor stars in the Milky Way seem to prefer rare core-collapse supernovae over neutron star mergers as the dominant source of r-process elements. I am planning to explore the effects of neutron star kicks, which will impact the distribution of these elements. An improved multi-phase model for the ISM may also change how efficiently metal mixing occurs. Please let me know if you have a favourite r-process enrichment model you would like to test in a cosmological context or if you would like to work with the available data.

Bywgraffiad

Cyflogaeth

 

 

Rwy'n Gymrawd Ymchwil Prifysgol y Gymdeithas Frenhinol ac yn Uwch-ddarlithydd ym Mhrifysgol Caerdydd. Ymunais â'r Ysgol Ffiseg a Seryddiaeth yn 2020. Cyn hyn, gwnes i bost byr yn Sefydliad Max Planck ar gyfer Astroffiseg yn Garching, yr Almaen. Symudais i Garching o Heidelberg lle roeddwn i'n gweithio fel cymrawd Tschira yn Sefydliad Astudiaethau Damcaniaethol Heidelberg, swydd a oedd ar y cyd â Phrifysgol Yale yn New Haven, UDA. Cyn hynny treuliais 4 blynedd yn UC Berkeley yng Nghaliffornia ac yn Academia Sinica yn Taipei, Taiwan.

Cefais fy PhD ar dwf galaethau a'u halos nwyol yn 2012 o Brifysgol Leiden yn Yr Iseldiroedd, lle bûm yn gweithio gyda Joop Schaye. Cyn hyn, fe wnes i fy MSc (mewn seryddiaeth) a BSc (mewn seryddiaeth ac mewn ffiseg) hefyd ym Mhrifysgol Leiden. 

Meysydd goruchwyliaeth

Areas within astronomy available for PhD projects:

  • Galaxy formation
  • Cosmological, magnetohydrodynamical simulations
  • Circumgalactic medium
  • Chemical enrichment including neutron capture elements

Goruchwyliaeth gyfredol

Andrew Hannington

Andrew Hannington

Myfyriwr ymchwil

Andy Cook

Andy Cook

Myfyriwr ymchwil

Thomas Rintoul

Thomas Rintoul

Arddangoswr Graddedig

Contact Details

Email vandeVoortF@caerdydd.ac.uk

Campuses Adeiladau'r Frenhines, Ystafell N/2.08A, 5 The Parade, Heol Casnewydd, Caerdydd, CF24 3AA