Pith. sign in

REVIEW 1 cited by

The colliding-wind WC9+OB system WR 65 and dust formation by WR stars

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 1508.00724 v1 pith:CUIUZVBM submitted 2015-08-04 astro-ph.SR

The colliding-wind WC9+OB system WR 65 and dust formation by WR stars

P. M. Williams (1) , K. A. van der Hucht (2 , 3) ((1) University of Edinburgh , Royal Observatory , Edinburgh , (2) SRON Utrecht , (3) University of Amsterdam) This is my paper
classification astro-ph.SR
keywords duststarscolliding-windemissionformationmaximumsystemadopt
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

Observations of the WC9+OB system WR 65 in the infrared show variations of its dust emission consistent with a period near 4.8~yr, suggesting formation in a colliding-wind binary (CWB) having an elliptical orbit. If we adopt the IR maximum as zero phase, the times of X-ray maximum count and minimum extinction to the hard component measured by Oskinova & Hamann fall at phases 0.4--0.5, when the separation of the WC9 and OB stars is greatest. We consider WR 65 in the context of other WC8-9+OB stars showing dust emission.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Variable dust emission by WC type Wolf-Rayet stars observed in the NEOWISE-R survey

    astro-ph.SR 2019-06 unverdicted novelty 5.0

    NEOWISE-R data identifies ten new non-variable dust makers among WC stars (including three early subtypes), six new episodic dust makers, and revises the dust formation period of HD 36402 to 5.1 years.