(Sivun lopussa suomenkielisiä aihekuvauksia - omat ehdotukset myös tervetulleita!)
- Room MA308
- phone: +358 (0) 504 318 047
- Elmegreen, D. et al. (2011) ApJ 737, 32 (artikkeli sisältää hyviä referenssejä) "Grand design and flocculent spirals in S4G survey (3.6 micron)"
- Buta, R. (2011) "galaxy Morphology" https://ned.ipac.caltech.edu/level5/sep11/Buta/Buta_contents.html
Regulation of star formation and the mystery of a failed spiral galaxy (J. Janz):
In this project you will look at a peculiar galaxy (b) that is located far from other galaxies. This galaxy has a bright central part with similarities to a dwarf galaxy without star formation (a) or the inner part of bright spiral galaxies (d). However, the galaxy as a whole is very different from either, since it features a large faint disk with stars forming, which is just visible on the optical image, but evident at ultra-violet wavelengths (c). The question is: why? In order to answer this question you will learn about mining the wealth of data of the Sloan Digital Sky Survey and look for similar objects to identify common properties.
Failed Spiral Galaxy (IMAGES: SDSS and GALEX)
Ice-Volcanic Activity of Jupiter's Moon Europa (J. Schmidt):
Europa is one of the large moons of Jupiter. It is believed to harbor an ocean of water beneath its ice crust and it is the scientific target of the NASA Europa Clipper Mission, that will explore its habitability. Recently, two independent observations suggest that Europa is also active, expelling a plume of water vapor and other gases to space from an ice-volcano on its surface. This bachelor project will explore and review the literature on this topic and it will summarize the major scientific questions. In additions, a simple model for the ejection and the pattern of falling back plume material on the surface will be developed.
Left panel: Europa from the NASA Galileo Mission. Hubble Space Telescope observations, indicating ice-volcanic activity on Europa (Sparks et al., 2016, middle, Roth et al., 2013, right).
Mass distribution of black holes and neutron stars in X-ray binaries (V. Neustroev):
Black holes and neutron stars are the end point of massive star evolution. Most of them are thought to have been formed in supernova explosions due to the collapse of the massive stellar core. It is to be expected that the masses of the resultant compact remnants correlate with the masses of their progenitor stars which have a smooth distribution in the range from the heaviest to the lightest stars. Surprisingly, the observed distribution of black hole and neutron star masses seems to have a gap in the range between 2 to 5 solar masses. This gap, whose existence was fairly well established some time ago, has become a significant challenge to our understanding of compact object formation. However, in recent years, the measurements of masses of compact objects in several new binaries were obtained, and for a few others the masses were refined. The goal of this project is to update the mass distribution of black holes and neutron stars using the current sample of the mass measurements. Does the mass gap still exist? The presence or absence of the mass gap is a critical clue in understanding the formation of neutron stars and black holes and the engine behind supernova explosions.
X-ray binary GRS 1915. The black hole absorbs material from a companion star, which is heated by friction, emitting X-rays. (Picture: Rob Hynes)
Diffuse Ionized Gas in Star-Forming Galaxies (A. Watkins):
Almost all star-forming galaxies contain large amounts of diffuse gas traceable by recombination lines (light emitted when electrons stripped off their host atoms by energetic photons recombine with said atoms), alternately known as 'diffuse ionized gas' (DIG) or the 'warm ionized medium' (WIM). While the discovery of this gas dates back almost half a century, the source of the ionization energy remains mysterious. This project would involve making a summary of the current state of research on DIG, with a possible extra project to make a comparative study of the DIG fractions (the fraction of ionized gas in a galaxy found in DIG vs. that found in compact star forming regions) in two interacting systems --- M51 and M101 --- using the deepest available narrowband imaging of these two galaxies.
Left: Optical image of galaxy M51. Right: Distribution of diffuse ionized gas and hydrogen. (IMAGES: BST and A. Watkins)
Saturn's Ring Moons (X. Liu):
The moon Pan is located in the inner system of Saturn, and its orbit is in the Encke Gap within Saturn's A ring. One of the surprising discoveries of the Cassini mission in 2017 was that Pan has a very peculiar shape, a bit like a walnut or a ravioli. Besides, in the Encke gap, there are also three ringlets that are associated with the orbits of Pan. This bachelor project will review the previous research on the formation scenario of the moon Pan and the three ringlets.
The moon Pan embedded in Saturn's rings (IMAGES: NASA/JPL)
2D spectroscopy: What can we obtain from it? (S. Comeron):
If we want to know how and when galaxies have formed, we need to use spectroscopy. For instance, spectroscopy allows us to measure the stellar kinematics and the stellar populations of galaxies outside the Milky Way. The advent of Integral Field Spectroscopy allowed us to produce 2D maps of spectroscopically-derived quantities in the galaxies around us. However, extracting information from spectra is not easy and requires dedicated software. In this project the student will perform a literature search on software that studies spectra and on what information can be extracted. It will be possible to do some additional work with stellar/gas velocity and velocity dispersion maps provided by the supervisor.
(Comeron et al, in preparation)
Jupiter's Gossamer Rings (X. Liu, J. Schmidt):
The giant planet Jupiter has a system of faint dust rings. Among these are the so-called gossamer rings, which were discovered in an image taken by the Voyager spacecraft, and later explored in more detail in images taken by the Galileo orbiter mission and earthbound observations. The gossamer rings are believed to be formed by dust that is ejected from two small moons of Jupiter, Amalthea and Thebe. This bachelor project will explore and review the literature on this topic.
Edge-on image taken from the NASA Galileo spacecraft showing Jupiter's dusty gossamer rings. (Image modified from Burns et al., 1999, Science.)
Main Belt Comets (J. Schmidt):
Until recently, it was believed that asteroids and comets are fundamentally different types of solar system objects. This picture was put into question by the discovery of objects in the asteroid belt of the solar system that show clear signs of comet-like activity. Apparently some process leads to the release of dust streams from these asteroids, which form a tail, in a very similar way like comets. This bachelor project will explore and review the literature on this topic.
Asteroids in the solar system develop comet like dust tails (Hsieh and Jewitt, 2006).
Stellar cannibalism transforms normal stars into brown dwarfs. How does it happen? (V. Neustroev):
Interacting binary stars known as Cataclysmic variables (CVs) consist of a white dwarf as primary and a low-mass star as secondary component. According to standard evolutionary theory, CVs evolve from longer to shorter orbital periods until a minimum period is reached (Pmin~76 min). The properties of the secondary star here are expected to change dramatically. The previously normal donor star becomes of a substellar mass and partially degenerate, resulting in a kind of a brown-dwarf-like object. I have recently initiated a new project to systematically search for such objects by means of photometric and spectroscopic observations. I have already obtained a significant amount of data and more observations will be collected soon. I invite students to help me to analyze these data, using statistical and other methods. Subtopics of the project can be formulated for both Bachelor and Master levels.
Hypernopeat tähdet (H. Salo) || (High-velocity stars ejected from Galaxy Center):
Linnunradassa on havaittu tähtiä, joiden nopeus on niin suuri että ne pystyvät karkaamaan Linnunradan gravitaatiokentästä. Todennäköisenä selityksenä pidetään Linnunradan keskuksen mustaa aukkoa, ja sen lähistölle tulleita kaksoistähtiä: mustan aukon painovoima voi irrottaa kaksoistähden komponentit keskinäiseltä radoiltaan ja johtaa tähtien nopeaan sinkoutumiseen.
Luk-tutkielmassa perehdyt aiheeseen liittyvään kirjallisuuteen, käyttäen lähtökohtana Brown (2015) review-artikkelia. Voit tehdä myös omia numeerisia integrointeja, joilla havainnollistat kyseistä mekanismia.
(W.R. Brown (2015) Hypervelocity Stars. Annu Rev. Astron. Astrophys 53, 15-49)
Some Milky Way stars move with velocities that exceed the the escape velocity of our Galaxy. The plausible explanation for such stars is the Galaxy's central black hole which has disrupted a binary star system in its vicinity: this can lead to ejection of the components with high velocities. In the bachelor thesis you familiarize yourself with the literature related to the topic, using Brown (2015) review as a starting point. You may also include your own numerical integrations illustrating the disruption mechanism.
Galaksien spiraalirakenne optisissa ja infrapunakuvissa (H. Salo) || (Spiral structure in optical and near-IR):
Kierteisgalaksien spiraalirakenne näkyy selvimmin optisissa kuvissa, joissa korostuu kirkkaat nuoret tähdet ja niiden ympärillään ionisoiman kaasun lähettämä säteily. Lähi-infrapunassa säteily on peräisin pienimassaisemmista tähdistä ja seuraa tarkemmin galaksin tähtien massajakaumaa.
Luk-tutkielmassa perehdyt kirjallisuuden perusteella galaksien spiraalirakenteeseen ja siihen miten se eroaa eri aallonpituuksilla tehdyissä havainnoissa. Teet myös omia vertailuja siitä miten spiraalien Fourier-amplitudit poikkeavat SDSS (ugriz-kaistat) ja S4G (3.6 mikronia kuvissa; tätä varten sovellat valmiita IDL-ohjelmia.)
Kosmologiset simulaatiot (H. Salo):
Vuonna 2005 julkaistu Millenium-simulaatio oli ensimmäinen koko maailmankaikkeuden kehitystä mallintava tietokonesimulaatio. Siinä jäljiteltiin pimeän aineen gravitaation aikaansaamaa suuren mittakaavan rakennetta seuraamalla 1E10 simulaatiopartikkelia laajenevassa maailmankaikkeudessa. Tämän jälkeen on ilmestynyt toinen toistaan kehittyneempiä simulaatioita (mm. Illustis, Eagle), joissa on pimeän aineen lisäksi mallinnettu myös huomattavasti vaikeampaa ongelmaa, eli tavallisen aineen prosesseja (kaasudynaamisia ilmiöitä, tähtien syntyä, aktiivisia galaksiytimiä jne).
Luk tukielmassa laadit kirjallisuuden perusteella vertailevan yhteenvedon erilaisista kosmologisista simulaatioista, niiden tärkeimmistä eroista ja keskeisistä tuloksista.
http://www.illustris-project.org/media/Topics for Bachelor's Theses