SN 2019vxm is a luminous, long-lived Type IIn supernova showing early flash-ionization features, a power-law bolometric light curve, and mid-IR dust formation, with a progenitor mass-loss rate lower limit of at least 0.01 solar masses per year.
Optical observations of the luminous Type IIn Supernova 2010jl for over 900 days
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The luminous Type IIn Supernova (SN) 2010jl shows strong evidence for the interaction of the SN ejecta with dense circumstellar material (CSM). We present observations of SN 2010jl for $t \sim 900$ d after its earliest detection, including a sequence of optical spectra ranging from $t = 55$ to $909$ d. We also supplement our late time spectra and the photometric measurements in the literature with an additional epoch of new, late time $BVRI$ photometry. Combining available photometric and spectroscopic data, we derive a semi-bolometric optical light curve and calculate a total radiated energy in the optical for SN 2010jl of $\sim 3.5\times10^{50}$ erg. We also examine the evolution of the H$\alpha$ emission line profile in detail and find evidence for asymmetry in the profile for $t \gtrsim 775$ d that is not easily explained by any of the proposed scenarios for this fascinating event. Finally, we discuss the interpretations from the literature of the optical and near-infrared light curves, and propose that the most likely explanation of their evolution is the formation of new dust in the dense, pre-existing CSM wind after $\sim 300$ d.
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2026 2verdicts
UNVERDICTED 2representative citing papers
Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.
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SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
SN 2019vxm is a luminous, long-lived Type IIn supernova showing early flash-ionization features, a power-law bolometric light curve, and mid-IR dust formation, with a progenitor mass-loss rate lower limit of at least 0.01 solar masses per year.
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Late-time evolution of the interacting stripped-envelope supernova 2017dio
Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.