Heart of Development, V. 1

Wheeler, Gordon; McConville, Mark

doi:10.4324/9781315781976

Cited by 1 publication

(2 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For a given opacity and velocity, the diffusion timescale thus allows us to derive the mass. Other authors have taken the observed rise times of SNe as an estimate of τm (most recently Wheeler, Johnson & Clocchiatti 2014). This is a reasonable approximation for 56 Ni-powered light curves, where the decay time is well known, and is closely matched to the typical diffusion times (a coincidence that results in the high peak luminosities in Type Ia SNe).…”

Section: Models: Overviewmentioning

confidence: 92%

“…This was discussed in detail, both in general and for specific models, in section 4, but we recap here for convenience. It is common practice to use the rise time as an estimate of τm (for a recent example, see Wheeler, Johnson & Clocchiatti 2014). This is approximately true in the original formulation of Arnett (1982), but that derivation was only for 56 Ni-powered SNe ( 56 Ni having an exponential lifetime of 8.8 days, comparable to the diffusion time in SNe Ia).…”

Section: Mass Estimatesmentioning

confidence: 99%

See 1 more Smart Citation

On the diversity of superluminous supernovae: ejected mass as the dominant factor

Nicholl¹,

Smartt²,

Jerkstrand³

et al. 2015

Mon. Not. R. Astron. Soc.

186

247

View full text Add to dashboard Cite

We assemble a sample of 24 hydrogen-poor super-luminous supernovae (SLSNe). Parameterizing the light curve shape through rise and decline timescales shows that the two are highly correlated. Magnetar-powered models can reproduce the correlation, with the diversity in rise and decline rates driven by the diffusion timescale. Circumstellar interaction models can exhibit a similar rise-decline relation, but only for a narrow range of densities, which may be problematic for these models. We find that SLSNe are approximately 3.5 magnitudes brighter and have light curves 3 times broader than SNe Ibc, but that the intrinsic shapes are similar. There are a number of SLSNe with particularly broad light curves, possibly indicating two progenitor channels, but statistical tests do not cleanly separate two populations. The general spectral evolution is also presented. Velocities measured from Fe II are similar for SLSNe and SNe Ibc, suggesting that diffusion time differences are dominated by mass or opacity. Flat velocity evolution in most SLSNe suggests a dense shell of ejecta. If opacities in SLSNe are similar to other SNe Ibc, the average ejected mass is higher by a factor 2-3. Assuming κ = 0.1 cm 2 g −1 , we estimate a mean (median) SLSN ejecta mass of 10 M (6 M ), with a range of 3-30 M . Doubling the assumed opacity brings the masses closer to normal SNe Ibc, but with a high-mass tail. The most probable mechanism for generating SLSNe seems to be the core-collapse of a very massive hydrogen-poor star, forming a millisecond magnetar.

show abstract

Section: Models: Overviewmentioning

confidence: 92%

Section: Mass Estimatesmentioning

confidence: 99%