2020ApJ...903L..24L -
Astrophys. J., 903, L24-L24 (2020/November-2)
A unified accreting magnetar model for long-duration gamma-ray bursts and Some stripped-envelope supernovae.
LIN W.L., WANG X.F., WANG L.J. and DAI Z.G.
Abstract (from CDS):
Both the long-duration gamma-ray bursts (LGRBs) and the Type I superluminous supernovae (SLSNe I) have been proposed to be primarily powered by central magnetars. A correlation, proposed between the initial spin period (P0) and the surface magnetic field (B) of the magnetars powering the X-ray plateaus in LGRB afterglows, indicates a possibility that the magnetars have reached an equilibrium spin period due to the fallback accretion. The corresponding accretion rates are inferred as {dot}M~10–4–10–1M☉ s–1, and this result holds for the cases of both isotropic and collimated magnetar wind. For the SLSNe I and a fraction of engine-powered normal Type Ic supernovae (SNe Ic) and the broad-lined subclass (SNe Ic-BL), the magnetars could also reach an accretion-induced spin equilibrium, but the corresponding B–P0 distribution suggests a different accretion rate range, i.e., {dot}M~10–7–10–3M☉ s–1. Considering the effect of fallback accretion, magnetars with relatively weak fields are responsible for the SLSNe I, while those with stronger magnetic fields could power SNe Ic/Ic-BL. Some SLSNe I in our sample could arise from compact progenitor stars, while others that require longer-term accretion may originate from the progenitor stars with more extended envelopes or circumstellar medium.
Abstract Copyright:
© 2020. The American Astronomical Society. All rights reserved.
Journal keyword(s):
Magnetars - Supernovae - Gamma-ray bursts
Simbad objects:
19
Full paper
View the references in ADS
To bookmark this query, right click on this link: simbad:2020ApJ...903L..24L and select 'bookmark this link' or equivalent in the popup menu