X iv : a st ro - p h / 98 05 25 2 v 1 1 9 M ay 1 99 8 Open Universes , Inflation , and the Anthropic Principle ∗

ar X iv : a st ro - p h / 98 05 25 2 v 2 2 8 M ay 1 99 8 Open Universes , Inflation , and the Anthropic Principle ∗

Models of open inflation with a variable density parameter Ω provide the most natural way to reconcile an open universe with inflation. The use of anthropic principle is essential to derive observational predictions of such models. I discuss how this principle can be used in a quantitative way to determine the most probable value of Ω. I also comment on recent work by Hawking and Turok on quant...

ar X iv : a st ro - p h / 99 05 37 6 v 1 2 8 M ay 1 99 9 A 6 . 4 - hr positive superhump period in TV

ar X iv : a st ro - p h / 98 05 24 3 v 1 1 9 M ay 1 99 8 ι Cas : Multi - element Doppler imaging and magnetic field geometry

In order to clarify the role of the magnetic field in generating abundance inhomogeneities in the atmospheres of Ap stars, we present new abundance Doppler images and an approximate magnetic field geometry for the Ap star ι Cas.

ar X iv : a st ro - p h / 98 05 18 9 v 1 1 4 M ay 1 99 8 Isotopic composition of Hg and Pt in slowly rotating HgMn stars

Preliminary results from a study of the isotopic compositions of the elements Hg and Pt in a number of HgMn stars are presented. This work represents an improvement over previous studies thanks to the very high spectral resolution available (R = 118 000) and to the new information on wavelengths and atomic structure of Hg II and Pt II.

ar X iv : a st ro - p h / 92 05 00 5 v 1 9 M ay 1 99 2 UCSBTH – 92 – 05 April 1992 CHAOTIC DARK MATTER

A very weakly coupled scalar field with mass m and initial vacuum expectation value V will provide enough mass to close the universe provided V ≃ (3 × 10 8 GeV)(100 GeV/m) 1/4. We discuss possible models in which such a field could arise. (a) Electronic address (internet): [email protected].