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A Spectroscopic and Photometric Study of 1H0542-407: A New Magnetic Variable

Published online by Cambridge University Press:  25 April 2016

D. A. H. Buckley  and
I. R. Tuohy
D. A. H. Buckley
Affiliation:
Mount Stromlo and Siding Springs Observatories, Institute of Advanced Studies, Australian National University
I. R. Tuohy
Affiliation:
Mount Stromlo and Siding Springs Observatories, Institute of Advanced Studies, Australian National University
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Abstract

We report spectroscopic and photometric observations of the new DQ Hercuis system 1H0542-407, recently discovered by us to be the optical counterpart of a HEAO-1 X-ray source. Medium resolution spectroscopy using the AAT in the region λ3930 to λ4960 conducted over consecutive nights shows radial velocity variations at periods of ∼ 1910 s, consistent with the white dwarf rotation period, and 5.7 h, in agreement with the orbital period derived from our EXOSAT observations. The K semi-amplitude velocities are ∼ 50 and 20 km s-1 respectively, leading to a mass function f(M) = 3.3 ± 0.6 × 10-3M⊙ and an orbital inclination close to 20°. The emission line profiles are characterized by simple Gaussians whose FWHM vary at the rotation period. A time series analysis of high resolution photometry conducted on the ANU 2.3 metre telescope reveals the presence of several periodicities, including the orbital sidebands. The dominant sideband (Vr − Vo) arises from X-rays reprocessed in a region corotating at the orbital frequency. A model is developed for 1H0542-407 which indicates that the accretion disk is disrupted at ∼5Rwd by the primary’s magnetic field. The short period velocity variations arise within the magnetosphere. A white dwarf magnetic field strength of < ∼ 3 MG is implied.

Type
Stellar
Information
Publications of the Astronomical Society of Australia , Volume 7 , Issue 2 , 1987 , pp. 151 - 158
Copyright
Copyright © Astronomical Society of Australia 1987

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