ar X iv : a st ro - p h / 98 02 30 4 v 1 2 4 Fe b 19 98 1

ar X iv : a st ro - p h / 99 02 23 4 v 2 1 7 Fe b 19 99 OB ASSOCIATIONS

ar X iv : a st ro - p h / 98 02 06 1 v 2 2 4 Fe b 19 98 Cosmic Axion ∗

+ θ̄ 16π2 TrFμνF̃ μν (2) Since this θ̄ term violates CP invariance, the upper bound of the neutron electric dipole moment puts a strong constraint on the magnitude of θ̄, |θ̄| < 10. The smallness of θ̄ has led to the strong CP problem, “Why is θ̄ so small?” [1] We know that many small parameters in physics have led to new ideas, in most cases leading to new symmetries. For example, MW/MP ≪ 1 has led t...

ar X iv : h ep - p h / 98 02 41 9 v 1 2 5 Fe b 19 98 COURSE LARGE N QCD

ar X iv : a st ro - p h / 98 02 16 1 v 1 1 2 Fe b 19 98 The intrinsic properties of the local interstellar medium

We propose a new method to constrain the actual state of the interstellar cloud that surrounds the solar system. Using Voyager UVS Lyman-α sky maps and the powerful principle of invariance, we derive the H distribution all along the spacecraft path. Provided current models of the heliopause interface between the solar and the interstellar winds, we extrapolate this distribution to farther dista...

ar X iv : a st ro - p h / 98 02 12 1 v 2 1 1 Fe b 19 98 Distance to M 31 With the HST and Hipparcos Red Clump Stars

Following an approach by Paczy´nski & Stanek we compare red clump stars with parallaxes known to better than 10% in the Hipparcos catalog with the red clump stars observed in three fields in M31 using the HST. There are ∼ 600 and ∼ 6, 300 such stars in the two data sets, respectively. The local red clump luminosity function is well represented by a Gaussian with the peak at M I 0 ,m = −0.23, an...