Figure 4 - uploaded by Lawrence Krauss
Content may be subject to copyright.
Color-magnitude diagram for a typical globular cluster, M15. Vertical axis plots the magnitude (luminosity) of the stars in the V wavelength region and the horizontal axis plots the color (surface temperature) of the stars.

Color-magnitude diagram for a typical globular cluster, M15. Vertical axis plots the magnitude (luminosity) of the stars in the V wavelength region and the horizontal axis plots the color (surface temperature) of the stars.

Source publication
Article
Full-text available
The flat matter dominated Universe that dominated cosmological model building for much of the past 20 years does not correspond to the Universe in which we live. This has profound implications both for our understanding of dark matter, and also for our understanding of the future of the Universe. I review recent developments here and present best f...

Similar publications

Article
Full-text available
Most cosmological models of inflation are far away from providing a smoking gun at low energies. A model of Higgs inflation in the Next-to-Minimal Supersymmetric Standard Model, however, changes the NMSSM phenomenology drastically and may be well distinguished from the pure NMSSM or MSSM at a future Linear Collider. We point out certain differences...
Article
Full-text available
This white paper describes the basic idea for indirect dark matter searches using antideuterons. Low energy antideuterons produced by dark matter annihilations/decays provide an attractive dark matter signature, due to the low astrophysical background. The current and future experiments have a strong potential to detect antideuterons from dark matt...
Article
Full-text available
Understanding galaxy formation is one of the most pressing issues in cosmology. We review the current status of galaxy formation from both an observational and a theoretical perspective, and summarise the prospects for future advances.
Article
We briefly discuss some aspects of the problem of forming large scale structures in the Universe. The basic picture that initially small perturbations generated by inflation grow by the process of gravitational instability to give the observed structures is largely consistent with the observations. The growth of the perturbations depends crucially...
Article
Full-text available
We describe a technique for using simulated tensor perturbations in order to place upper limits on the intensity of magnetic fields in the early universe. As an example, we apply this technique to the beginning of primordial nucleosynthesis. We determined that any magnetic seed fields that existed before that time were still in the process of being...

Citations

... [19][20][21][22][23][24] Other papers about "physics via human eyes" can be found e.g. here [25][26][27] in part motivated by the recent movie Interstellar. [28][29][30] This paper takes a new step in the before-mentioned direction. ...
Article
Full-text available
It is generally believed that in the epoch prior to the formation of the first stars, the Universe was completely dark (the period is therefore known as the Dark Ages). Usually the start of this epoch is placed at the photon decoupling. In this work we investigate the question whether there was enough light during the dark epoch for a human eye to see. We use the black body spectrum of the Universe to find the flux of photon energy for different temperatures and compare them with visual limits of blindness and darkness. We find that the Dark Ages actually began approximately 5 million years later than commonly stated.
Article
Full-text available
Dark energy models due to a slowly evolving scalar (quintessence) field Phi are studied for various potentials V (Phi) in a universe with negative curvature. The potentials differ in whether they possess a minimum at Phi = 0 or are monotonously declining, i. e. have a minimum at infinity. The angular power spectrum C_ l of the cosmic microwave background (CMB) as well as the magnitude-redshift relation m_B (z) of the type Ia supernovae are compared with the quintessence models. It is demonstrated that some of the models with Omega_tot ~ 0.85 to 0.9 are in agreement with the observations, i. e. possess acoustic peaks in the angular power spectrum of the CMB anisotropy as observed experimentally, and yield a magnitude-redshift relation in agreement with the data. Furthermore, it is found that the power spectrum P (k) of the large-scale structure (LSS) agrees with the observations too.
Article
Full-text available
We analyze the implications of several recent cosmological and experimental measurements for the mass spectra of the Constrained MSSM (CMSSM). We compute the relic abundance of the neutralino and compare the new cosmologically expected and excluded mass ranges with those ruled out by the final LEP bounds on the lightest chargino and Higgs masses, with those excluded by current experimental values of $\br(B\to X_s \gamma)$, and with those favored by the recent measurement of the anomalous magnetic moment of the muon. We find that for $tan\beta\lsim 45$ there remains relatively little room for the mass spectra to be consistent with the interplay of the several constraints. On the other hand, at larger values of $tan\beta\$ the decreasing mass of the pseudoscalar Higgs gives rise to a wide resonance in the neutralino WIMP pair-annihilation, whose position depends on the ratio of top and bottom quark masses. As a consequence, the cosmologically expected regions consistent with other constraints often grow significantly and generally shift towards superpartner masses in the $\tev$ range. Comment: LaTex, 21 pages, 4 PS figures. Version published in JHEP, for updates see hep-ph/0206178