22 research outputs found
Recurrent dust formation by WR 48a on a 30-year timescale
We present infrared photometry of the WC8 Wolf-Rayet system WR 48a observed
with telescopes at ESO, the SAAO and the AAT between 1982 and 2011 which show a
slow decline in dust emission from the previously reported outburst in 1978--79
until about 1997, when significant dust emission was still evident. This was
followed by a slow rise, accelerating to reach and overtake the first (1978)
photometry, demonstrating that the outburst observed in 1978--79 was not an
isolated event, but that they recur at intervals of 32+ years. This suggests
that WR 48a is a long-period dust maker and colliding-wind binary (CWB). The
locus of WR 48a in the (H-L), K colour-magnitude diagram implies that the rate
of dust formation fell between 1979 and about 1997 and then increased steadily
until 2011. Superimposed on the long-term variation are secondary (`mini')
eruptions in (at least) 1990, 1994, 1997, 1999 and 2004, characteristic of
relatively brief episodes of additional dust formation. Spectra show evidence
for an Oe or Be companion to the WC8 star, supporting the suggestion that WR
48a is a binary system and indicating a system luminosity consistent with the
association of WR 48a and the young star clusters Danks 1 and Danks 2. The
range of dust formation suggests that these stars are in an elliptical orbit
having e ~ 0.6. The size of the orbit implied by the minimum period, together
with the WC wind velocity and likely mass-loss rate, implies that the
post-shock WC wind is adiabatic throughout the orbit -- at odds with the
observed dust formation. A similar conflict is observed in the `pinwheel'
dust-maker WR 112.Comment: 15 pages, 8 figures, accepted for publication in MNRA