The optically thick rotating magnetic wind from a massive white dwarf merger product. (arXiv:1907.12317v1 [astro-ph.SR])

The optically thick rotating magnetic wind from a massive white dwarf merger product. (arXiv:1907.12317v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kashiyama_K/0/1/0/all/0/1">Kazumi Kashiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujisawa_K/0/1/0/all/0/1">Kotaro Fujisawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shigeyama_T/0/1/0/all/0/1">Toshikazu Shigeyama</a>

WD J005311 is a newly identified white dwarf (WD) in a mid-infrared nebula.
The spectroscopic observation indicates the existence of a neon-enriched
carbon/oxygen wind with a terminal velocity of $v_{infty,rm obs}sim
16,000,rm km,s^{-1}$ and a mass loss rate of $dot M_{rm obs}sim 3.5times
10^{-6},M_odot$ yr$^{-1}$. Here we consistently explain the properties of WD
J005311 using a newly constructed wind solution, where the optically thick
outflow is launched from the carbon burning shell on an oxygen-neon core and
accelerated by the rotating magnetic field to become supersonic and unbound
well below the photosphere. Our model implies that WD J005311 has a mass of
$M_* sim 1.1mbox{-}1.3,M_odot$, a magnetic field of $B_* sim
(2mbox{-}5)times 10^7,rm G$, and a spin angular frequency of $Omega sim
0.2mbox{-}0.5 ,rm s^{-1}$. The large magnetic field and fast spin support
the carbon-oxygen WD merger origin. WD J005311 will neither explode as a type
Ia supernova nor collapse into a neutron star. If the wind continues to blow
another few kyr, WD J005311 will spin down significantly and join to the known
sequence of slowly-rotating magnetic WDs. Otherwise it may appear as a
fast-spinning magnetic WD and could be a new high energy source.

WD J005311 is a newly identified white dwarf (WD) in a mid-infrared nebula.
The spectroscopic observation indicates the existence of a neon-enriched
carbon/oxygen wind with a terminal velocity of $v_{infty,rm obs}sim
16,000,rm km,s^{-1}$ and a mass loss rate of $dot M_{rm obs}sim 3.5times
10^{-6},M_odot$ yr$^{-1}$. Here we consistently explain the properties of WD
J005311 using a newly constructed wind solution, where the optically thick
outflow is launched from the carbon burning shell on an oxygen-neon core and
accelerated by the rotating magnetic field to become supersonic and unbound
well below the photosphere. Our model implies that WD J005311 has a mass of
$M_* sim 1.1mbox{-}1.3,M_odot$, a magnetic field of $B_* sim
(2mbox{-}5)times 10^7,rm G$, and a spin angular frequency of $Omega sim
0.2mbox{-}0.5 ,rm s^{-1}$. The large magnetic field and fast spin support
the carbon-oxygen WD merger origin. WD J005311 will neither explode as a type
Ia supernova nor collapse into a neutron star. If the wind continues to blow
another few kyr, WD J005311 will spin down significantly and join to the known
sequence of slowly-rotating magnetic WDs. Otherwise it may appear as a
fast-spinning magnetic WD and could be a new high energy source.

http://arxiv.org/icons/sfx.gif