SN2018kzr: A Rapidly Declining Transient from the Destruction of a White Dwarf

We present SN2018kzr, the fastest declining supernova-like transient, second only to the kilonova, AT2017gfo. SN2018kzr is characterized by a peak magnitude of Mr = −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 bolomet...

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Published inAstrophysical journal. Letters Vol. 885; no. 1; p. L23
Main Authors McBrien, Owen R., Smartt, Stephen J., Chen, Ting-Wan, Inserra, Cosimo, Gillanders, James H., Sim, Stuart A., Jerkstrand, Anders, Rest, Armin, Valenti, Stefano, Roy, Rupak, Gromadzki, Mariusz, Taubenberger, Stefan, Flörs, Andreas, Huber, Mark E., Chambers, Ken C., Gal-Yam, Avishay, Young, David R., Nicholl, Matt, Kankare, Erkki, Smith, Ken W., Maguire, Kate, Mandel, Ilya, Prentice, Simon, Rodríguez, Ósmar, Garcia, Jonathan Pineda, Gutiérrez, Claudia P., Galbany, Lluís, Barbarino, Cristina, Clark, Peter S. J., Sollerman, Jesper, Kulkarni, Shrinivas R., De, Kishalay, Buckley, David A. H., Rau, Arne
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.11.2019
IOP Publishing
Subjects
Alternative energy sources
Binary stars
Bolometers
Deposition
Ejecta
Luminosity
Magnetars
Neutron stars
Neutrons
Stellar winds
Supernova
Supernovae
White dwarf stars
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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 Mr = −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 Mej = 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.
AbstractList 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 נ1043 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.
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 & xfffd;=& xfffd;?17.98, a peak bolometric luminosity of ?1.4 & xfffd;& x5e0;10(43) erg s(?1), and a rapid decline rate of 0.48 & xfffd;& xfffd;0.03 mag day(?1) in the r band. The bolometric luminosity evolves too quickly to be explained by pure Ni-56 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 & xfffd;=& xfffd;0.10 & xfffd;& xfffd;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.
We present SN2018kzr, the fastest declining supernova-like transient, second only to the kilonova, AT2017gfo. SN2018kzr is characterized by a peak magnitude of Mr = −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 Mej = 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.
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 × 10 43 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 56 Ni 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.
Author Smith, Ken W.
Mandel, Ilya
Flörs, Andreas
Sollerman, Jesper
Sim, Stuart A.
Buckley, David A. H.
Inserra, Cosimo
Rest, Armin
Nicholl, Matt
Gutiérrez, Claudia P.
Gromadzki, Mariusz
Barbarino, Cristina
Galbany, Lluís
Jerkstrand, Anders
Kankare, Erkki
Prentice, Simon
Taubenberger, Stefan
Maguire, Kate
Clark, Peter S. J.
McBrien, Owen R.
Chambers, Ken C.
De, Kishalay
Garcia, Jonathan Pineda
Young, David R.
Kulkarni, Shrinivas R.
Rau, Arne
Smartt, Stephen J.
Roy, Rupak
Gillanders, James H.
Chen, Ting-Wan
Gal-Yam, Avishay
Valenti, Stefano
Rodríguez, Ósmar
Huber, Mark E.
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DocumentTitleAlternate SN2018kzr: A Rapidly Declining Transient from the Destruction of a White Dwarf
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Snippet We present SN2018kzr, the fastest declining supernova-like transient, second only to the kilonova, AT2017gfo. SN2018kzr is characterized by a peak magnitude of...
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StartPage L23
SubjectTerms Alternative energy sources
Binary stars
Bolometers
Deposition
Ejecta
Luminosity
Magnetars
Neutron stars
Neutrons
Stellar winds
Supernova
Supernovae
White dwarf stars
Title SN2018kzr: A Rapidly Declining Transient from the Destruction of a White Dwarf
URI https://iopscience.iop.org/article/10.3847/2041-8213/ab4dae
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