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Long-term stability of the HR 8799 planetary system without resonant lock
News from the quantum zoo
Twist and finite size effects for the source method
We analyze the finite size effects for the source method in pure lattice gauge theory at weak coupling. They are found to be strongly suppressed by twisting the boundary conditions, for SU(3) by typically an order of magnitude.
MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters - IV. Cataclysmic variables - properties of bright and faint populations
Probing the vertical abundance structure of the Galactic disc using red clump stars
What Gaia can reveal about the matter distribution in the Milky Way
Context. With the goal to accurately map about a billion of the Milky Way stars, the astrometric satellite Gaia was launched in December 2013. Its high precision and sensitivity will lead to better understanding of the Galactic structure and evolution. Also, it will be possible to probe the matter distribution in the Galaxy. Aims. To study how well the Galactic matter distribution can be determin
Measurements of oscillator strengths in V II using charge transfer reactions
A kinematic check of the distance scale of Galactic Cepheids
A selection of well known period luminosity relations for cepheid variables are studied under the assumption that cepheid variables have a mean vertical velocity of zero in the galactic plane. Proper motion data from Hipparcos and Thyco-2 catalogues are coupled with the distances obtained from applying the period luminosity relations on a database of known classical cepheids to calculate the veloc
Accurate Abundances of Giant Stars in the Local disk: A manual analysis of IR APOGEE spectra
Purpose: In order to study the Galactic Chemical Evolution, elemental abundances are needed. The purpose of this work is to investigate the chemical evolution of the Milky Way by determining several elemental abundances of giants in the local disk. Large surveys are up and coming, and several surveys are already working, and with these, the aim is high quality abundance measurements of several ele
Do variations in the initial mass function affect galaxy evolution?
Grain size distribution in protoplanetary disks
The chemical composition of hot and cold gas giants
The survival of stellar clusters
In this project I have studied the effect of gas expulsion on the evolution of stellar clusters. What effect the rate of gas removal and the quantity of gas removed has on the evolution on the cluster will be studied through computer simulations with the NBody6 code and compared to analytical predictions. The rate at which gas is removed has a very significant impact on how the cluster evolves
The consequences of dwarf galaxies colliding with the Milky Way
Monte Carlo studies of protein aggregation
The disease-linked amyloid beta (A beta) and alpha-synuclein (alpha S) proteins are both fibril-forming and natively unfolded in free monomeric form. Here, we discuss two recent studies, where we used extensive implicit solvent all-atom Monte Carlo (MC) simulations to elucidate the conformational ensembles sampled by these proteins. For alpha S, we somewhat unexpectedly observed two distinct phase
Non-representative Quantum Mechanical Weak Values
The operational definition of a weak value for a quantum mechanical system involves the limit of the weak measurement strength tending to zero. I study how this limit compares to the situation for the undisturbed (no weak measurement) system. Under certain conditions, which I investigate, this limit is discontinuous in the sense that it does not merge smoothly to the Hilbert space description of t
Har materien charm? Om Psi och andra elementarpartiklar
The Gaia-ESO survey: Calibration strategy
The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consi
