The precessing jets of classical nova YZ Reticuli. (arXiv:2102.12946v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+McLoughlin_D/0/1/0/all/0/1">Dominic McLoughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blundell_K/0/1/0/all/0/1">Katherine M. Blundell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_S/0/1/0/all/0/1">Steven Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCowage_C/0/1/0/all/0/1">Chris McCowage</a>
The classical nova YZ Reticuli was discovered in July 2020. Shortly after
this we commenced a sustained, highly time-sampled coverage of its subsequent
rapid evolution with time-resolved spectroscopy from the Global Jet Watch
observatories. Its H-alpha complex exhibited qualitatively different spectral
signatures in the following weeks and months. We find that these H-alpha
complexes are well described by the same five Gaussian emission components
throughout the six months following eruption. These five components appear to
constitute two pairs of lines, from jet outflows and an accretion disc,
together with an additional central component. The correlated, symmetric
patterns that these jet/accretion disc pairs exhibit suggest precession,
probably in response to the large perturbation caused by the nova eruption. The
jet and accretion disc signatures persist from the first ten days after
brightening — evidence that the accretion disc survived the disruption. We
also compare another classical nova (V6568 Sgr) that erupted in July 2020 whose
H-alpha complex can be described analogously, but with faster line-of-sight jet
speeds exceeding 4000 km/s. We suggest that classical novae with higher mass
white dwarfs bridge the gap between recurrent novae and classical novae such as
YZ Reticuli.
The classical nova YZ Reticuli was discovered in July 2020. Shortly after
this we commenced a sustained, highly time-sampled coverage of its subsequent
rapid evolution with time-resolved spectroscopy from the Global Jet Watch
observatories. Its H-alpha complex exhibited qualitatively different spectral
signatures in the following weeks and months. We find that these H-alpha
complexes are well described by the same five Gaussian emission components
throughout the six months following eruption. These five components appear to
constitute two pairs of lines, from jet outflows and an accretion disc,
together with an additional central component. The correlated, symmetric
patterns that these jet/accretion disc pairs exhibit suggest precession,
probably in response to the large perturbation caused by the nova eruption. The
jet and accretion disc signatures persist from the first ten days after
brightening — evidence that the accretion disc survived the disruption. We
also compare another classical nova (V6568 Sgr) that erupted in July 2020 whose
H-alpha complex can be described analogously, but with faster line-of-sight jet
speeds exceeding 4000 km/s. We suggest that classical novae with higher mass
white dwarfs bridge the gap between recurrent novae and classical novae such as
YZ Reticuli.
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