Open AccessEvidence for a rotational velocity field about the white dwarf of V347 Puppis
Author(s) -
Still M. D.,
Buckley D. A. H.,
Garlick M. A.
Publication year - 1998
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1998.01806.x
Subject(s) - physics , astrophysics , white dwarf , radial velocity , line (geometry) , binary star , accretion (finance) , stars , astronomy , dwarf nova , emission spectrum , proper motion , spectral line , geometry , mathematics
We present time‐resolved optical spectroscopy of the deeply eclipsing nova‐like binary V347 Pup, which provides evidence for a rotational velocity field in the low‐excitation lines, as expected from accretion disc emission. The low‐excitation line profiles are a composite of the disc and the irradiated inner‐face of the donor star. This picture is remarkably simple compared to the other members of the eclipsing nova‐like family. Unsatisfactory radial velocity solutions for the accreting object provided by standard methods encourage us to apply a technique developed to measure stellar motion from tomographic reconstructions of the time‐dependent line profiles. We find some evidence for a spiral pattern over the disc and for disc‐overflow accretion. If the emission distribution proves to be a long‐term feature, V347 Pup will provide an opportunity to study disc kinematics with greater confidence than allowed by the other eclipsing nova‐like objects.