Open AccessMulti‐epoch Doppler tomography and polarimetry of QQ Vul
Author(s) -
Schwope Axel D.,
Catalán Maria S.,
Beuermann Klaus,
Metzner André,
Smith Robert Con,
Steeghs Danny
Publication year - 2000
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.1365-8711.2000.03240.x
Subject(s) - physics , astrophysics , polarimetry , orbital motion , polarization (electrochemistry) , astronomy , linear polarization , photosphere , light curve , position angle , binary star , right ascension , azimuth , orbital period , emission spectrum , ephemeris , stars , angular momentum , spectral line , optics , galaxy , declination , satellite , scattering , laser , chemistry , quantum mechanics
We present multi‐epoch high‐resolution spectroscopy and photoelectric polarimetry of the long‐period polar (AM Herculis star) QQ Vul. The blue emission lines show several distinct components, the sharpest of which can unequivocally be assigned to the illuminated hemisphere of the secondary star and used to trace its orbital motion. This narrow emission line can be used in combination with Na i absorption lines from the photosphere of the companion to build a stable long‐term ephemeris for the star: inferior conjunction of the companion occurs at HJD=244 8446.4710(5)+ E ×0154 520 11(11). The polarization curves are dissimilar at different epochs, thus supporting the idea of fundamental changes of the accretion geometry, e.g., between one‐ and two‐pole accretion modes. The linear polarization pulses display a random scatter by 0.2 phase units and are not suitable for the determination of the binary period. The polarization data suggest that the magnetic (dipolar) axis has a colatitude of 23°, an azimuth of −50°, and an orbital inclination between 50° and 70°. Doppler images of blue emission and red absorption lines show a clear separation between the illuminated and non‐illuminated hemispheres of the secondary star. The absorption lines on their own can be used to determine the mass ratio of the binary by Doppler tomography with an accuracy of 15–20 per cent. The narrow emission lines of different atomic species show remarkably different radial velocity amplitudes: K =85–130 km s −1 . Emission lines from the most highly ionized species, He ii , originate closest to the inner Lagrangian point L 1 . We can discern two kinematic components within the accretion stream; one is associated with the ballistic part, and the other with the magnetically threaded part of the stream. The location of the emission component associated with the ballistic accretion stream appears displaced between different epochs. Whether this displacement indicates a dislocation of the ballistic stream, e.g. by a magnetic drag, or emission from the magnetically threaded part of the stream with near‐ballistic velocities, remains unsolved.