Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 1 A. Evans,Janet H. Wood Conference proceedings 1996 Kluwer Academic Publishe

考博

漫不經(jīng)心

Dwarf Nova Outbursts and Superoutburstsapproach, of putting some constraints on α. In particular, the strong dependence of the viscous time-scale on viscosity itself permits us to estimate aα almost directly from the observed time-scales. In the case of the hot branch of the Σ - .. relation, the most reliable estimates (α.) are based on

boisterous

New Observational Frontiers of Er Uma (= PG 0943+521) Type Dwarf Novaethe extremely short recurrence time of the superoutburst (～ 40 d in ER UMa and V1159 Ori, ～ 20 d in RZ LMi), (ii) short outbursts with short recurrence times (～ 4 d) between the bright states, and (iii) extremely long duty cycles (～ 0.5). Assuming that the mass transfer rate from the secondary is te

Notorious

Superhumps in the SU UMa Star AK CNC (Chile), Ouda Station (Kyoto, Japan) and in England. Superhumps with amplitude 0.2 mag appeared at least 4d after maximum. They evolved from a single peak structure, developing a secondary peak during decline, until they reached a double-wave modulation with 0.05 mag amplitude, after 8 d. After rem

按等級(jí)

Applications of Indirect Accretion Disc Imaging to Orbital Solutions for Primary Starsc in order to provide information on the primary’s motion. However, discs are not axisymmetric structures and the standard approach generally fails because the asymmetry-free inner disc emission is usually dominated by statistical noise.

sed-rate

Studies in Flickeringent of the total luminosity of the system (hence it is often more luminous than the entire secondary star); (iii) flickering is inherently a time—dependent phenomenon and it is hoped that it can provide clues to the nature of the disc viscosity, something that time—independent theory cannot provide.

ear-canal

Waveforms and Instrumentation Overview, (1990) in order to establish whether these systems are truely at large distances, or are instead a population of intrinsically faint objects lying relatively nearby. The distances were determined using Bailey’s method (1982) and incorporated the recent .. calibrations by Ramseyer (1994).

transplantation

CROAK

jeopardize

Online Resolution of E-commerce Disputes996) showed that the light curves of these stars can be reproduced by the disk instability model, which does not require mass transfer bursts. These indicate that ER UMa, VI159 Ori and RZ LMi are not on the natural extension of SU UMa-type dwarf novae.