Envelope-to-disk mass transport in the FUor-type young eruptive star V346 Normae. (arXiv:2002.04342v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kospal_A/0/1/0/all/0/1">Á. Kóspál</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_P/0/1/0/all/0/1">P. Ábrahám</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feher_O/0/1/0/all/0/1">O. Fehér</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miera_F/0/1/0/all/0/1">F. Cruz-Saenz de Miera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takami_M/0/1/0/all/0/1">M. Takami</a>
Having disk-to-star accretion rates on the order of 10$^{-4},M_{odot}$/yr,
FU Orionis-type stars (FUors) are thought to be the visible examples for
episodic accretion. FUors are often surrounded by massive envelopes, which
replenish the disk material and enable the disk to produce accretion outbursts.
We observed the FUor-type star V346 Nor with ALMA at 1.3~mm continuum and in
different CO rotational lines. We mapped the density and velocity structure of
its envelope and analyzed the results using channel maps, position-velocity
diagrams, and spectro-astrometric methods. We discovered a pseudo-disk and a
Keplerian disk around a 0.1 $M_{odot}$ central star. We determined an infall
rate from the envelope onto the disk of 6$times$10$^{-6},M_{odot}$/yr, a
factor of few higher than the quiescent accretion rate from the disk onto the
star. This hints for a mismatch between the infall and accretion rates as the
cause of the eruption.
Having disk-to-star accretion rates on the order of 10$^{-4},M_{odot}$/yr,
FU Orionis-type stars (FUors) are thought to be the visible examples for
episodic accretion. FUors are often surrounded by massive envelopes, which
replenish the disk material and enable the disk to produce accretion outbursts.
We observed the FUor-type star V346 Nor with ALMA at 1.3~mm continuum and in
different CO rotational lines. We mapped the density and velocity structure of
its envelope and analyzed the results using channel maps, position-velocity
diagrams, and spectro-astrometric methods. We discovered a pseudo-disk and a
Keplerian disk around a 0.1 $M_{odot}$ central star. We determined an infall
rate from the envelope onto the disk of 6$times$10$^{-6},M_{odot}$/yr, a
factor of few higher than the quiescent accretion rate from the disk onto the
star. This hints for a mismatch between the infall and accretion rates as the
cause of the eruption.
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