Radial velocity studies of Hell and H-beta emission from cataclysmic variables

    Authors

    C. Schwarz;M. M. Montgomery

    Comments

    Authors: contact us about adding a copy of your work at STARS@ucf.edu

    Abbreviated Journal Title

    New Astron.

    Keywords

    Accretion; Accretion disks; Binaries: general; Binaries: close; Stars:; dwarf novae; Novae; Cataclysmic variables; Hydrodynamics; Radial; velocity curves; STREAM-DISK IMPACT; ACCRETION DISKS; INTERACTING BINARIES; SIMULATIONS; SUPERHUMPS; DYNAMICS; SYSTEMS; Astronomy & Astrophysics

    Abstract

    Radial velocity (RV) plots of Hell and Hp emission lines from non-magnetic Cataclysmic Variable (CV) systems are frequently fit with a sin curve but sometimes contain outlying data points around phase phi similar to 1.0. A lack of consensus exists on the origin of these outlying points. In this work, we develop an analytical model that is based upon our 3D Smoothed Particle Hydrodynamic (SPH) numerical model to simulate these RV curves. Our chosen targets are CV SW Sextanis-like systems UX Uma and RW Tri as well as SU UMa dwarf novae systems H alpha 0242-28 and 1RXSJ1808+10, which have secondary-to-primary mass ratios of q = (0.43, 0.86, 0.27, 0.18), respectively. In our model, we include disk eccentricity, inclination angle, degree of disk-tilt, bright spot (s), and/or gas stream overflow. Our model provides good non-sinusoidal fits to the observed RV data, including outlying data points near phi similar to 1.0, suggesting these excess points may be caused by gas-stream overflow. (C) 2013 Elsevier B.V. All rights reserved.

    Journal Title

    New Astronomy

    Volume

    27

    Publication Date

    1-1-2014

    Document Type

    Article

    Language

    English

    First Page

    73

    Last Page

    80

    WOS Identifier

    WOS:000327169400010

    ISSN

    1384-1076

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