Near IR Spectroscopic monitoring of WR 140 during the 2001 periastron passage

Details Near IR Spectroscopic monitoring of WR 140 during the 2001 periastron passage Near IR Spectroscopic monitoring of WR 140 during the 2001 periastron passage

2004-03-27

arxiv.org/abs/astro-ph/0403639v1

Mon.Not.Roy.Astron.Soc. 351 (2004) 1307

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS - 13 Pages, 10 figures

Scientific paper

10.1111/j.1365-2966.2004.07867.x

We present new spectra of WR 140 (HD 193793) in the JHK bands with some covering the 1.083-micron He I emission line at higher resolution, observed between 2000 October and 2003 May to cover its 2001 periastron passage. The WC7 + O4-5 spectroscopic binary WR 140 is the prototype of colliding-wind, episodic dust-making Wolf-Rayet systems which also show strong variations in radio and X-ray emission. The JHK spectra showed changes in continuum and in the equivalent widths of the WC emission lines, consistent with formation of dust starting between 2001 January 3 and March 26 (orbital phases 0.989 and 0.017) and its subsequent fading and cooling. The 1.083-micron He I line has a P-Cygni profile which showed variations in both absorption and emission components as WR 140 went through periastron passage. The variation of the absorption component yielded tight constraints on the geometry of the wind-collision region, giving theta = 50 +/- 8 degrees for the opening semi-angle of the interaction `cone', indicating a wind-momentum ratio of the O to the WR star=0.1, about three times larger than previously believed. As the system approached periastron, the emission component showed the appearance of a significant sub-peak, movement of which across the profile was seen to be consistent with its formation in wind material flowing along the contact discontinuity between the two stellar winds and the changing orientation of the colliding wind region. The flux carried in the sub-peak exceeded the X-ray fluxes measured at previous periastron passages. This additional source of radiative cooling of the shock-heated gas probably causes it to depart from being adiabatic around periastron passage, thereby accounting for the departure of the X-ray flux from its previously expected $1/d$-dependency.

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