The open cluster Messier 67 is known to have chemical composition, metallicity and age (~ 4 Gyr) close to the Sun. Therefore, it is advantageous for stellar physical studies and of stellar evolution, in particular for solar like stars within the cluster. This work considers three such stars, the formerly studied solar twin M67-1194 and two more recently suggested solar twins M67-1787 & 2018. Most solar twins show a ratio of volatile to refractory elements that systematically depart from the Sun’s. Our targets do not follow this trend as closely. Their composition is closer to the Sun and they are, therefore, exquisite targets for studies of stellar evolution within the cluster. However, their solar likeness also provides studies regarding the origin and evolution of the Solar system. The stellar ages of the solar twins are established through a chemical clock [Y/Mg] and via stellar isochrones from BaSTI. The latter age assessment of the solar twins is supplemented with the analysis of two subgiant stars M67-1442 & 1844. We approach the isochrone-based method using spectroscopically, astrometrically and photometrically derived parameters. The different ages of the stars and methods thus estimate the age of the cluster itself. The chemical ages of the stars suggest a cluster age of 4.56  ±0.44 Gyr and the isochrone-based estimates suggests a cluster age within the range 3.30-5.51 Gyr. Our results thus affirm and imply a near solar age of the cluster.

No description available.

This thesis was carried out in two parts. The stellar spectral data was used from the Gaia-ESO survey. The data used was fromthe public archive as well as data received from Dr. Recio-Blanco at Observatoire Cote D'Azure. 1) I performed anomaly detection using unsupervised random forests, by applying the concept of weirdness scores to identify outliers. 2) Using spectral data along with physical parameters of objects in the galactic bulge of the Gaia-ESO survey, I built a variational autoencoder neural network to reconstruct stellar spectra and explore latent features learning physical parameters by themselves.

SN2020qlb (ZTF20abobpcb) is an extensively sampled hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (max. Mg = -22:25+/-0:01 magnitudes) and long-rising (77.1 days from explosion to maximum) in a category of the brightest and longest rising SNe currently known in the Universe. SN2020qlb exhibits clear light-curve undulations, a phenomenon seen in other SLSNe but whose physical origin is still a mystery. This Master of Science Thesis discusses both the potential power source of these immense explosions as well as the power mechanisms behind the observed light-curve undulations. A particularly large set of photometric data in both the visible and ultraviolet ranges and covering the first 410 days after explosion, as well as 10 spectra are available for analysis. The explosion date is constrained to +/-0.28 days; the phase and magnitude of the peak luminosity are determined; light-curves for each telescope/filter combination are constructed; the g-r color evolution is plotted; the photospheric temperature and radius evolutions are estimated; the bolometric light-curve is constructed and compared with known power source models; and the rest-frame spectral evolution is plotted for analysis. SN2020qlb is found to meet all the known criteria to be a SLSN-I. A radioactive power source model based on the decay of 56Ni is rejected due to unphysical parameter results. A source model based on the dipole spindown energy deposition of a magnetar fits well the bulk portion of the bolometric light-curve with physically possible parameter values. Two full periods of about 32+/-6 day undulations are found on top of the bulk light-curve after subtracting the smooth model values. Evidence for them is also seen in each filter light-curve. Hypothetical power sources for these striking characteristics from the literature are analyzed and discussed. In summary, a magnetar source for the bulk of the light curve is favored. An external source for the undulations is favored, e.g. interaction with variations in the progenitor star’s circumstellar material, with a caveat that an explanation involving the break-down of model assumptions cannot be ruled out. Together they are favored to explain the entire light-curve of SN2020qlb.

Failed supernovae are the implosive final fates of massive stars, where ablack hole is formed. During the collapse, the proto-neutron star emits a huge number of neutrinos, and when the black hole is finally formed, it engulfs theneutrino-emitting material and the signal is cut off. Inspired by the recent work of Nagakura & Hotokezaka (2020), this thesis improves on some parts of theirs imulation work and further explores the neutrino signal from failed supernovae, using a supercomputer to perform Monte Carlo simulations. In particular, we realized the neutrino flux’ time evolution around black hole formation hasn’t previously been studied well, and so it is investigated here, as well as the plausibility of measuring the black hole mass through the shape of the decay. A new component of the signal is presented, an echo of neutrinos emitted before black hole formation that, due to scattering in supersonic material around the black hole, arrive with a time delay of up to 15 ms, and with a significantly higher average energy, for heavy lepton neutrinos around 50 MeV.

Modelling stellar structures and comparing them with observationsis a very important step when it comes to verifying our theories aboutstellar evolution. Three-dimensional reconstruction is therefore impor-tant and in the case of certain stellar types it makes for a large portionof the ongoing research.For this project, three dierent objects and their three-dimensionalmodels were selected for 3D-printing. The systems in question areEta Carinae, 1 Gruis and HD 101584 and the reason behind thischoice is the fact that each object showcases a dierent phase and/orprocess of stellar evolution approaching or during the planetary nebula(PN) stage. On top of that, these objects have been observed using atechnique that allows us to deduce their 3D structure.The three-dimensional models and prints allow us to nd features(such as axial symmetries) that give us more information about themovements inside the system and their consequences on how the stellarstructure has and will evolve.

For this project, a historical statistical analysis of the Amplitude of Mass Fluctuations ($\sigma_8$) and Hubble's Constant ($H_0$) parameters in the Standard Cosmological Model was carried out to determine whether or not the given error bars truly represent the dispersion of values. It was found through analysis of the Chi-Squared ($\chi^2$) values of the data that for $\sigma_8$ (60 data points and $\chi^2$ between 183.167 and 189.037) that the associated probability Q is extremely low, with $Q = 1.5597*10^{-15}$ for the weighted average and $Q = 1.2107*10^{-14}$ for the best fit of the data. This was also the case for the $\chi^2$ values (163 data points and $\chi^2$ between 484.3977 and 575.655) of $H_0$, where $Q = 4.2176*10^{-34}$ for the linear fit of the data and $Q = 1.0342*10^{-47}$ for the weighted average of the data. Through further analysis, it is shown in question, a linear fit is a better estimate of the data than the weighted average. The general conclusion is that the statistical error bars have been underestimated (in around 20\% of the measurements), or the systematic errors were not properly taken into account.

This project aims to determine the solar Mg abundance with two infrared spectral lines: MgI λ10811 and λ10965. Downloaded line data from VALD are updated with modern values for the oscillator strengths and van der Waals damping parameters, the latter obtained through ABO theory. Utilizing SME, the Mg abundances of synthetic spectra are fitted with respect to a solar atlas. The derived abundance for varied turbulence configurations is found to be between logAMg+12 = 7.40–7.52, which is slightly lower than meteoric and 3D-modeled values. Suggested improvements would be to consider the effects of NLTE and line blending.

The current cosmological paradigm of an accelerating cosmic expansion issupported by observations of Type Ia supernovae. However, the light emittedby these and other cosmological sources is not only redshifted by cosmicexpansion but will also interact with matter along the light path. Especiallyintergalactic dust can lead to additional reddening and dimming of distantsources due to light scattering or absorption. This yields systematiccontaminations to cosmological measurements. This project builds afoundation and some of the tools that will be used in a master’s thesis withthe aim of analysing the spatial distribution and the properties of this cosmicdust. While previous studies assumed cosmic dust to be homogeneouslydistributed, it is expected to follow the spatial distribution of galaxies fromwhich it was expelled. This project also starts to recreate previous models ofhomogeneous dust models and measurements which will be used the futuremaster’s thesis. An analysis of the methods and tools used, along with some ofthe dust properties, is also made in this project.

The complex interactions between the Sun and Earth are referred to as Space Weather. Key parameters include magnetic indices which quantitatively describe geomagnetic activity by determining a baseline that removes the background magnetic field and allows quantification of the remaining activity during geomagnetic events. However, most used indices have a low temporal resolution and rely on a sparse and frozen network of ground magnetic observatories. This thesis introduces a novel way of determining the baseline for future high temporal and spatial resolution magnetic indices. Firstly, the main phenomena and effects of Space Weather are outlined, followed by a review of currently used magnetic indices and their derivation. The computation of a novel baseline introduced in this work relies on basic statistical methods which are applied on magnetic data from a dense and flexible network of ground observatories for the period 1991-2016. The focus is on the investigation of geomagnetic quiet periods for which average annual activity at each observatory is determined. A global latitudinal normalisation function with dependency on solar activity for quiet periods is found. The analysis of the newly derived baseline shows that it provides the temporal, spatial and amplitudinal resolution needed to characterise geomagnetic disturbances adequately. The residual signal has the capability of being used as the basis for further quiet period studies. A first attempt of new indices based on the introduced derivation shows a good agreement with already existing high temporal and spatial resolution magnetic indices. Future indices derived with this baseline lay a favourable fundament for the application of articial intelligence methods.