Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a). (arXiv:1903.09232v1 [astro-ph.HE])

Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a). (arXiv:1903.09232v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Aydi_E/0/1/0/all/0/1">E. Aydi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chomiuk_L/0/1/0/all/0/1">L. Chomiuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strader_J/0/1/0/all/0/1">J. Strader</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swihart_S/0/1/0/all/0/1">S. J. Swihart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bahramian_A/0/1/0/all/0/1">A. Bahramian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harvey_E/0/1/0/all/0/1">E. J. Harvey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Britt_C/0/1/0/all/0/1">C. T. Britt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_D/0/1/0/all/0/1">D. A. H. Buckley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_P/0/1/0/all/0/1">P. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dage_K/0/1/0/all/0/1">K. Dage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Darnley_M/0/1/0/all/0/1">M. J. Darnley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_S/0/1/0/all/0/1">S. Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hambsch_F/0/1/0/all/0/1">F-J. Hambsch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holoien_T/0/1/0/all/0/1">T. W.-S. Holoien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jha_S/0/1/0/all/0/1">S. W. Jha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kochanek_C/0/1/0/all/0/1">C. S. Kochanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuin_N/0/1/0/all/0/1">N. P. M. Kuin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_K/0/1/0/all/0/1">K. L. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monard_L/0/1/0/all/0/1">L. A. G. Monard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mukai_K/0/1/0/all/0/1">K. Mukai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Page_K/0/1/0/all/0/1">K. L. Page</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_J/0/1/0/all/0/1">J. L. Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richardson_N/0/1/0/all/0/1">N. D. Richardson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shappee_B/0/1/0/all/0/1">B. J. Shappee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shishkovsky_L/0/1/0/all/0/1">L. Shishkovsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokolovsky_K/0/1/0/all/0/1">K. V. Sokolovsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanek_K/0/1/0/all/0/1">K. Z. Stanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">T. Thompson</a>

We present a detailed study of the 2017 eruption of the classical nova
ASASSN-17pf (LMCN 2017-11a), which is located in the Large Magellanic Cloud,
including data from AAVSO, ASAS-SN, SALT, SMARTS, SOAR, and the Neil Gehrels
textit{Swift} Observatory. The optical light-curve is characterized by
multiple maxima (flares) on top of a slowly evolving light-curve (with a
decline time, $t_2>$ 100 d). The maxima correlate with the appearance of new
absorption line systems in the optical spectra characterized by increasing
radial velocities. We suggest that this is evidence of multiple episodes of
mass-ejection with increasing expansion velocities. The line profiles in the
optical spectra indicate very low expansion velocities (FWHM $sim$ 190 km
s$^{-1}$), making this nova one of the slowest expanding ever observed,
consistent with the slowly evolving light-curve. The evolution of the colors
and spectral energy distribution show evidence of decreasing temperatures and
increasing effective radii for the pseudo-photosphere during each maximum. The
optical and infrared light-curves are consistent with dust formation 125 days
post-discovery. We speculate that novae showing several optical maxima have
multiple mass-ejection episodes leading to shocks that may drive $gamma$-ray
emission and dust formation.

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