ar X iv : a st ro - p h / 01 04 11 3 v 1 6 A pr 2 00 1 1 / 2 Law for Non - Radiative Accretion Flow

ar X iv : a st ro - p h / 02 04 03 6 v 1 2 A pr 2 00 2 Investigating the Flame Microstructure in Type

ar X iv : a st ro - p h / 06 04 29 8 v 1 1 3 A pr 2 00 6 the Non - Gaussianity of Racetrack Inflation Models

In this paper, we use the result in [7] to calculate the non-Gaussianity of the racetrack models in [3, 5]. Our results show that the nonGaussianity in [3] is reasonable, while the non-Gaussianity in [5] is beyond the observational limits.

ar X iv : a st ro - p h / 01 11 13 6 v 1 7 N ov 2 00 1 1 Active Optics in Modern , Large Optical Telescopes

ar X iv : a st ro - p h / 06 04 29 8 v 2 1 4 A pr 2 00 6 the Non - Gaussianity of Racetrack Inflation Models

In this paper, we use the result in [7] to calculate the non-Gaussianity of the racetrack models in [3, 5]. Our results show that the nonGaussianity in [3] is reasonable, while the non-Gaussianity in [5] is beyond the observational limits. PACS: 98.80.Cq, 98.80.Jk, 04.20.Gz

ar X iv : a st ro - p h / 01 04 42 8 v 1 2 6 A pr 2 00 1 Echoes in X - ray binaries ; mapping the accretion flow

In X-ray binaries much of the optical/UV emission arises from X-rays reprocessed by material in the accretion disk, stream and the companion star. The resulting reprocessed variability will be delayed in time with respect to the X-ray variability by an amount depending on the position of the reprocessing regions. We can determine a range of time-delays present in the system. This time-delay tra...