Figure 20 from RAPIDLY RISING TRANSIENTS IN THE SUPERNOVA

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RAPIDLY RISING TRANSIENTS IN THE SUPERNOVA—SUPERLUMINOUS SUPERNOVA GAP

Authors: Iair Arcavi, William M. Wolf, D. Andrew Howell, Lars Bildsten, Giorgos Leloudas, Delphine Hardin, Szymon Prajs, Daniel A. Perley, Gilad Svirski, Avishay Gal-Yam, Boaz Katz, Curtis McCully, S. Bradley Cenko, Chris Lidman, Mark Sullivan, Stefano Valenti, Pierre Astier, Cristophe Balland, Ray G. Carlberg, Alex Conley, Dominique Fouchez, Julien Guy, Reynald Pain, Nathalie Palanque-Delabrouille, Kathy Perrett, Chris J. Pritchet, Nicolas Regnault, James Rich, and Vanina Ruhlmann-Kleider

2016 The Astrophysical Journal 819 35.

Provider: AAS Journals

Caption: Figure 20.

Magnetar initial spin period and magnetic field contours (in units of 10¹⁴ G) from Kasen & Bildsten (2010); assuming an explosion energy of 10⁵¹ erg and an opacity κ = 0.2 cm² gr⁻¹) for an ejecta mass of 5M_⊙ (top) and 2M_⊙ (bottom). The magnetar models can reproduce the rise time and peak luminosity of our events only with extremely rapid initial spin periods and low ejecta masses.

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