2015ApJ...804L..32M

We report on monitoring observations of the TeV γ-ray binary HESS J0632+057, which were carried out to constrain the interaction between the Be circumstellar disk and the compact object of unknown nature and provide for the first time high-dispersion (R ≳ 50,000) optical spectra in the second half of the orbital cycle, from apastron through periastron. The Hα, Hβ, and Hγ line profiles are found to exhibit remarkable short-term variability for ∼1 month after the apastron (phase 0.6-0.7), whereas they show little variation near the periastron. These emission lines show ''S-shaped'' variations with a timescale of ∼150 days, which is about twice that reported previously. In contrast to the Balmer lines, no profile variability is seen in any Fe ii emission line. We estimate the radii of emitting regions of the Hα, Hβ, Hγ, and Fe ii emission lines to be ∼30, 11, 7, and 2 stellar radii (R_*), respectively. The amplitudes of the line profile variations in different lines indicate that the interaction with the compact object affects the Be disk down to, at least, the radius of 7 R_* after the apastron. This fact, together with little profile variability near the periastron, rules out the tidal force as the major cause of disk variability. Although this leaves the pulsar wind as the most likely candidate mechanism for disk variations, understanding the details of the interaction, particularly the mechanism for causing a large-scale disk disturbance after the apastron, remains an open question.