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  SN2018kzr: A rapidly declining transient from the destruction of a white dwarf

McBrien, O. R., Smartt, S. J., Chen, T.-W., Inserra, C., Gillanders, J. H., Sim, S. A., et al. (2019). SN2018kzr: A rapidly declining transient from the destruction of a white dwarf. The Astrophysical Journal Letters, 885(1): L23. doi:10.3847/2041-8213/ab4dae.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-A1FC-9 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-A1FD-8
Genre: Journal Article

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 Creators:
McBrien, Owen R., Author
Smartt, Stephen J., Author
Chen, Ting-Wan, Author
Inserra, Cosimo, Author
Gillanders, James H., Author
Sim, Stuart A., Author
Jerkstrand, Anders1, Author              
Rest, Armin, Author
Valenti, Stefano, Author
Roy, Rupak, Author
Gromadzki, Mariusz, Author
Taubenberger, Stefan1, Author              
Floers, Andreas1, Author              
Huber, Mark E., Author
Chambers, Ken C., Author
Gal-Yam, Avishay, Author
Young, David R., Author
Nicholl, Matt, Author
Kankare, Erkki, Author
Smith, Ken W., Author
Maguire, Kate, AuthorMandel, Ilya, AuthorPrentice, Simon, AuthorRodríguez, Ósmar, AuthorGarcia, Jonathan Pineda, AuthorGutiérrez, Claudia P., AuthorGalbany, Lluís, AuthorBarbarino, Cristina, AuthorClark, Peter S. J., AuthorSollerman, Jesper, AuthorKulkarni, Shrinivas R., AuthorDe, Kishalay, AuthorBuckley, David A. H., AuthorRau, Arne, Author more..
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

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 Abstract: We present SN2018kzr, the fastest declining supernova-like transient, second only to the kilonova, AT2017gfo. SN2018kzr is characterized by a peak magnitude of M r = −17.98, a peak bolometric luminosity of ~1.4 × 1043 erg s−1, and a rapid decline rate of 0.48 ± 0.03 mag day−1 in the r band. The bolometric luminosity evolves too quickly to be explained by pure 56Ni heating, necessitating the inclusion of an alternative powering source. Incorporating the spin-down of a magnetized neutron star adequately describes the lightcurve and we estimate a small ejecta mass of M ej = 0.10 ± 0.05 M . Our spectral modeling suggests the ejecta is composed of intermediate mass elements including O, Si, and Mg and trace amounts of Fe-peak elements, which disfavors a binary neutron star merger. We discuss three explosion scenarios for SN2018kzr, given the low ejecta mass, intermediate mass element composition, and high likelihood of additional powering—the core collapse of an ultra-stripped progenitor, the accretion induced collapse (AIC) of a white dwarf, and the merger of a white dwarf and neutron star. The requirement for an alternative input energy source favors either the AIC with magnetar powering or a white dwarf–neutron star merger with energy from disk wind shocks.

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 Dates: 2019-10-31
 Publication Status: Published online
 Pages: -
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 Table of Contents: -
 Rev. Type: -
 Identifiers: DOI: 10.3847/2041-8213/ab4dae
Other: LOCALID: 3192624
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Title: The Astrophysical Journal Letters
  Other : Astrophys. J. Lett.
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: - Volume / Issue: 885 (1) Sequence Number: L23 Start / End Page: - Identifier: ISSN: 2041-8205
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215