WR 72: a born-again planetary nebula with hydrogen-poor knots. (arXiv:1912.11051v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gvaramadze_V/0/1/0/all/0/1">V.V. Gvaramadze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kniazev_A/0/1/0/all/0/1">A.Y. Kniazev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graefener_G/0/1/0/all/0/1">G. Graefener</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Langer_N/0/1/0/all/0/1">N. Langer</a>
We report the discovery of a handful of optical hydrogen-poor knots in the
central part of an extended infrared nebula centred on the [WO1] star WR 72,
obtained by spectroscopic and imaging observations with the Southern African
Large Telescope (SALT). Wide-field Infrared Survey Explorer (WISE) images of
the nebula show that it is composed of an extended almost circular halo (of
$approx6$ arcmin or $approx2.4$ pc in diameter) and an elongated and
apparently bipolar inner shell (of a factor of six smaller size), within which
the knots are concentrated. Our findings indicate that WR 72 is a new member of
the rare group of hydrogen-poor planetary nebulae, which may be explained
through a very late thermal pulse of a post-AGB star, or by a merger of two
white dwarfs.
We report the discovery of a handful of optical hydrogen-poor knots in the
central part of an extended infrared nebula centred on the [WO1] star WR 72,
obtained by spectroscopic and imaging observations with the Southern African
Large Telescope (SALT). Wide-field Infrared Survey Explorer (WISE) images of
the nebula show that it is composed of an extended almost circular halo (of
$approx6$ arcmin or $approx2.4$ pc in diameter) and an elongated and
apparently bipolar inner shell (of a factor of six smaller size), within which
the knots are concentrated. Our findings indicate that WR 72 is a new member of
the rare group of hydrogen-poor planetary nebulae, which may be explained
through a very late thermal pulse of a post-AGB star, or by a merger of two
white dwarfs.
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