Supernova Light Curves Powered by Young Magnetars

Kasen, Daniel; Bildsten, Lars

doi:10.1088/0004-637x/717/1/245

Cited by 794 publications

(1,012 citation statements)

References 31 publications

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“…We think of this as macrophysical uncertainties, e.g., a clumpy density distribution. Radiation hydrodynamic calculations show that the magnetardriven ejecta pile up at some radius (Kasen & Bildsten 2010), rather than homogeneously distributed, as assumed in this work.…”

Section: Discussionmentioning

confidence: 66%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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Section: Discussionmentioning

confidence: 66%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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“…Expanding upon this and a number of authors have suggested that magnetars may power superluminous type II and Ibc SNe (Thompson et al 2004;Woosley 2010;Kasen & Bildsten 2010;Gal-Yam 2012;Quimby et al 2011); indeed the 7.29 M progenitor model of Woosley (2010) is directly motivated by the presence of J1647-45 within Wd1. Moreover, Inserra et al (2013) studied the late-time lightcurves of five superluminous type Ic SNe, finding that the data are indeed consistent with these events being powered by the rapid spin-down of newly born magnetars (see also McCrum et al 2013;Nicholl et al 2013) Additionally, magnetars have also been proposed as the central engines of some gamma-ray bursts (GRBs; e.g.…”

Section: Discussionmentioning

confidence: 76%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Najarro

et al. 2014

A&A

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Context. The first soft gamma-ray repeater was discovered over three decades ago, and was subsequently identified as a magnetar, a class of highly magnetised neutron star. It has been hypothesised that these stars power some of the brightest supernovae known, and that they may form the central engines of some long duration gamma-ray bursts. However there is currently no consenus on the formation channel(s) of these objects. Aims. The presence of a magnetar in the starburst cluster Westerlund 1 implies a progenitor with a mass ≥40 M , which favours its formation in a binary that was disrupted at supernova. To test this hypothesis we conducted a search for the putative pre-SN companion.Methods. This was accomplished via a radial velocity survey to identify high-velocity runaways, with subsequent non-LTE model atmosphere analysis of the resultant candidate, Wd1-5. Results. Wd1-5 closely resembles the primaries in the short-period binaries, Wd1-13 and 44, suggesting a similar evolutionary history, although it currently appears single. It is overluminous for its spectroscopic mass and we find evidence of He-and N-enrichement, O-depletion, and critically C-enrichment, a combination of properties that is difficult to explain under single star evolutionary paradigms. We infer a pre-SN history for Wd1-5 which supposes an initial close binary comprising two stars of comparable (∼41 M + 35 M ) masses. Efficient mass transfer from the initially more massive component leads to the mass-gainer evolving more rapidly, initiating luminous blue variable/common envelope evolution. Reverse, wind-driven mass transfer during its subsequent WC Wolf-Rayet phase leads to the carbon pollution of Wd1-5, before a type Ibc supernova disrupts the binary system. Under the assumption of a physical association between Wd1-5 and J1647-45, the secondary is identified as the magnetar progenitor; its common envelope evolutionary phase prevents spin-down of its core prior to SN and the seed magnetic field for the magnetar forms either in this phase or during the earlier episode of mass transfer in which it was spun-up. Conclusions. Our results suggest that binarity is a key ingredient in the formation of at least a subset of magnetars by preventing spin-down via core-coupling and potentially generating a seed magnetic field. The apparent formation of a magnetar in a Type Ibc supernova is consistent with recent suggestions that superluminous Type Ibc supernovae are powered by the rapid spin-down of these objects.

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“…The spin-down power of a newly formed magnetar can create a brighter and faster evolving SN light curve than radioactive decay (Piro & Ott 2011). This mechanism can contribute to the extreme peak luminosity of Type Ib/c and super-luminous SNe (Woosley 2010;Kasen & Bildsten 2010;Chatzopoulos et al 2012). In this case, (t) includes radioactive energy production as well as magnetar spin-down: where Ni (t) is the energy production rate of radioactive decay of nickel and cobalt as defined in the previous section and M (t) is the energy production rate of the spin-down per unit mass.…”

Section: Magnetar Spin-downmentioning

confidence: 99%

A semianalytical light curve model and its application to type IIP supernovae

Nagy

Ordasi

Vinkó

et al. 2014

A&A

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The aim of this work is to present a semianalytical light curve model code that can be used for estimating physical properties of core collapse supernovae (SNe) in a quick and efficient way. To verify our code we fit light curves of Type II SNe and compare our best parameter estimates to those from hydrodynamical calculations. For this analysis, we use quasi-bolometric light curves of five different Type IIP SNe. In each case, we obtain appropriate results for initial pre-supernova parameters. We conclude that this semianalytical light curve model is useful to obtaining approximate physical properties of Type II SNe without using time-consuming numerical hydrodynamic simulations.

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Supernova Light Curves Powered by Young Magnetars

Cited by 794 publications

References 31 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

A VLT/FLAMES survey for massive binaries in Westerlund 1

A semianalytical light curve model and its application to type IIP supernovae

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