North, R.C.; Marsh, T.R.; Kolb, U.; Dhillon, V.S. and Moran, C.K.J.
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1046/j.1365-8711.2002.05795.x|
|Google Scholar:||Look up in Google Scholar|
Although a large number of orbital periods of cataclysmic variable (CV) stars have been measured, comparison of period and luminosity distributions with evolutionary theory is affected by strong selection effects. A test has been discovered that is independent of these selection effects and is based upon the kinematics of CVs. If the standard models of evolution are correct then long-period (Porb > 5 h) CVs should be typically less than 1.5 Gyr old, and their line-of-sight velocity dispersion (σ) should be small. We present results from a pilot study, which indicate that this postulate is indeed true. Four long-period dwarf novae (EM Cyg, V426 Oph, SS Cyg and AH Her) were observed over a complete orbit, in order for accurate radial velocities to be obtained. We find values of −1.7, 5.4, 15.4 and 1.8 km s1 with uncertainties of the order of 3 km s1, referred to the dynamical local standard of rest, leading to a dispersion of 8 km s1. Calculation of a 95 per cent confidence interval gives the result 4 <σ < 28 km s1 compared with a prediction of 15 km s1. We also have an improved determination of mass donor spectral type, K2 and q for the four systems.
|Item Type:||Journal Article|
|Copyright Holders:||2002 The Royal Astronomical Society|
|Keywords:||accretion; accretion discs; techniques; radial velocities; binaries; spectroscopic; novae; cataclysmic variables|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 6827 not found.|
|Date Deposited:||06 Jul 2006|
|Last Modified:||14 Jan 2016 16:02|
|Share this page:|