Core-collapse explosions of Wolf-Rayet stars and the connection to type IIb/Ib/Ic supernovae

We present non-LTE time-dependent radiative-transfer simulations of supernova (SN) IIb/Ib/Ic spectra and light curves, based on ~1B-energy piston-driven ejecta, with and without 56Ni, produced from single and binary Wolf-Rayet (W-R) stars evolved at solar and sub-solar metallicities. Our bolometric light curves show a 10-day long post-breakout plateau with a luminosity of 1-5x10^7Lsun. In our 56Ni-rich models, with ~3Msun ejecta masses, this plateau precedes a 20-30-day long re-brightening phase initiated by the outward-diffusing heat wave powered by radioactive decay at depth. In low ejecta-mass models with moderate mixing, Gamma-ray leakage starts as early as ~50d after explosion and causes the nebular luminosity to steeply decline by ~0.02mag/d. Such signatures, which are observed in standard SNe IIb/Ib/Ic, are consistent with low-mass progenitors derived from a binary-star population. We propose that the majority of stars with an initial mass ~<20Msun yield SNe II-P if 'effectively" single, SNe IIb/Ib/Ic if part of a close binary system, and SN-less black holes if more massive. Our ejecta, with outer hydrogen mass fractions as low as ~>0.01 and a total hydrogen mass of ~>0.001Msun, yield the characteristic SN IIb spectral morphology at early times. However, by ~15d after the explosion, only Halpha may remain as a weak absorption feature. Our binary models, characterised by helium surface mass fractions of ~>0.85, systematically show HeI lines during the post-breakout plateau, irrespective of the 56Ni abundance. Synthetic spectra show a strong sensitivity to metallicity, which offers the possibility to constrain it directly from SN spectroscopic modelling.Comment: 23 pages, 2 tables, 13 figures, accepted to MNRA

The properties of the "standard" type Ic supernova 1994I from spectral models

The properties of the type Ic supernova SN 1994I are re-investigated. This object is often referred to as a "standard SN Ic" although it exhibited an extremely fast light curve and unusually blue early-time spectra. In addition, the observations were affected by significant dust extinction. A series of spectral models are computed based on the explosion model CO21 (Iwamoto et al. 1994) using a Monte Carlo transport spectral synthesis code. Overall the density structure and abundances of the explosion model are able to reproduce the photospheric spectra well. Reddening is estimated to be E(B-V)=0.30 mag, a lower value than previously proposed. A model of the nebular spectrum of SN 1994I points toward a slightly larger ejecta mass than that of CO21. The photospheric spectra show a large abundance of iron-group elements at early epochs, indicating that mixing within the ejecta must have been significant. We present an improved light curve model which also requires the presence of 56Ni in the outer layers of the ejecta.Comment: 11 pages, 8 figures. Acccepted for publication in MNRA

Patterns of abundance across geographical ranges as a predictor for responses to climate change:Evidence from UK rocky shores

Aim: Understanding patterns in the abundance of species across thermal ranges can give useful insights into the potential impacts of climate change. The abundant-centre hypothesis suggests that species will reach peak abundance at the centre of their thermal range where conditions are optimal, but evidence in support of this hypothesis is mixed and limited in geographical and taxonomic scope. We tested the applicability of the abundant-centre hypothesis across a range of intertidal organisms using a large, citizen science-generated data set. Location: UK. Methods: Species' abundance records were matched with their location within their thermal range. Patterns in abundance distribution for individual species, and across aggregated species abundances, were analysed using Kruskal–Wallis tests and quantile general additive models. Results: Individually, invertebrate species showed increasing abundances in the cooler half of the thermal range and decreasing abundances in the warmer half of the thermal range. The overall shape for aggregated invertebrate species abundances reflected a broad peak, with a cool-skewed maximum abundance. Algal species showed little evidence for an abundant-centre distribution individually, but overall the aggregated species abundances suggested a hump-backed abundance distribution. Main Conclusions: Our study follows others in showing mixed support for the abundant-centre hypothesis at an individual species level, but demonstrates an increased predictability in species responses when an aggregated overall response is considered

Development of risk maps to minimize uranium exposures in the Navajo Churchrock mining district

© 2009 deLemos et al; licensee BioMed Central Ltd. This is an Open Access article distributed under the terms of the Creative Commons Attribution Licens

From Shock Breakout to Peak and Beyond: Extensive Panchromatic Observations of the Type Ib Supernova 2008D associated with Swift X-ray Transient 080109

We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift/X-ray transient (XRT) 080109. Our data span a time range of 5 hours before the detection of the X-ray transient to 150 days after its detection, and detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines), and show that SN 2008D had a relatively long rise time of 18 days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for \Delta t~0.1- 4 day, most pronounced in the blue bands) followed by 56^Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E_K and M_ej from the literature, estimate the stellar radius R_star of its probable Wolf-Rayet progenitor. According to the model of Waxman et al. and of Chevalier & Fransson, we derive R_star^{W07}= 1.2+/-0.7 R_sun and R_star^{CF08}= 12+/-7 R_sun, respectively; the latter being more in line with typical WN stars. Spectra obtained at 3 and 4 months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.Comment: Accepted to ApJ, v3 contains more data than v2 and more references, conclusions not significantly changed, 28 pages in emulateapj, 17 figure

Stellar Forensics with the Supernova-GRB Connection

Long-duration gamma-ray bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) are amongst nature's most magnificent explosions. While GRBs launch relativistic jets, SNe Ib/c are core-collapse explosions whose progenitors have been stripped of their hydrogen and helium envelopes. Yet for over a decade, one of the key outstanding questions is which conditions lead to each kind of explosion and death in massive stars. Determining the fates of massive stars is not only a vibrant topic in itself, but also impacts using GRBs as star formation indicators over distances of up to 13 billion light-years and for mapping the chemical enrichment history of the universe. This article reviews a number of comprehensive observational studies that probe the progenitor environments, their metallicities and the explosion geometries of SN with and without GRBs, as well as the emerging field of SN environmental studies. Furthermore, it discusses SN 2008D/XRT 080109 that was discovered serendipitously with the Swift satellite via its X-ray emission from shock breakout, and that has generated great interest amongst both observers and theorists while illustrating a novel technique for stellar forensics. The article concludes with an outlook on how the most promising venues of research - with the existing and upcoming innovative large-scale surveys such as the Palomar Transient Factory and LSST - will shed new light on the diverse deaths of massive stars.Comment: Ludwig-Biermann Award Lecture 2010, 17 pages, 5 figures, submitted April 1 2011, published in AN 332, 43

A dynamic model of financial balances for the United Kingdom

We construct a new scenario analysis model for the United Kingdom using ONS data from 1987 to the present. The model links decisions about real variables to credit creation in the financial sector and decisions about asset allocation among investors for a wide array of financial assets. We develop, estimate, and calibrate the model from first principles as well as describing the stock-flow coherent database we construct to validate the model. We impose several scenarios on the model to test its usefulness as a medium term scenario analysis tool, including increases in banks’ capital ratios, sudden stops, changes in investment, increases in house prices and fiscal expansions