1,020 research outputs found
3D simulations of Rayleigh-Taylor mixing in core-collapse SNe with CASTRO
We present multidimensional simulations of the post-explosion hydrodynamics
in three different 15 solar mass supernova models with zero, 10^{-4} solar
metallicity, and solar metallicities. We follow the growth of the
Rayleigh-Taylor instability that mixes together the stellar layers in the wake
of the explosion. Models are initialized with spherically symmetric explosions
and perturbations are seeded by the grid. Calculations are performed in
two-dimensional axisymmetric and three-dimensional Cartesian coordinates using
the new Eulerian hydrodynamics code, CASTRO. We find as in previous work, that
Rayleigh-Taylor perturbations initially grow faster in 3D than in 2D. As the
Rayleigh-Taylor fingers interact with one another, mixing proceeds to a greater
degree in 3D than in 2D, reducing the local Atwood number and slowing the
growth rate of the instability in 3D relative to 2D. By the time mixing has
stopped, the width of the mixed region is similar in 2D and 3D simulations
provided the Rayleigh-Taylor fingers show significant interaction. Our results
imply that 2D simulations of light curves and nucleosynthesis in supernovae
(SNe) that die as red giants may capture the features of an initially
spherically symmetric explosion in far less computational time than required by
a full 3D simulation. However, capturing large departures from spherical
symmetry requires a significantly perturbed explosion. Large scale asymmetries
cannot develop through an inverse cascade of merging Rayleigh-Taylor
structures; they must arise from asymmetries in the initial explosion.Comment: 12 pages, 5 figures, ApJ accepte
PHotometry Assisted Spectral Extraction (PHASE) and identification of SNLS supernovae
Aim: We present new extraction and identification techniques for supernova
(SN) spectra developed within the Supernova Legacy Survey (SNLS) collaboration.
Method: The new spectral extraction method takes full advantage of
photometric information from the Canada-France-Hawai telescope (CFHT) discovery
and reference images by tracing the exact position of the supernova and the
host signals on the spectrogram. When present, the host spatial profile is
measured on deep multi-band reference images and is used to model the host
contribution to the full (supernova + host) signal. The supernova is modelled
as a Gaussian function of width equal to the seeing. A chi-square minimisation
provides the flux of each component in each pixel of the 2D spectrogram. For a
host-supernova separation greater than <~ 1 pixel, the two components are
recovered separately and we do not use a spectral template in contrast to more
standard analyses. This new procedure permits a clean extraction of the
supernova separately from the host in about 70% of the 3rd year ESO/VLT spectra
of the SNLS. A new supernova identification method is also proposed. It uses
the SALT2 spectrophotometric template to combine the photometric and spectral
data. A galaxy template is allowed for spectra for which a separate extraction
of the supernova and the host was not possible.
Result: These new techniques have been tested against more standard
extraction and identification procedures. They permit a secure type and
redshift determination in about 80% of cases. The present paper illustrates
their performances on a few sample spectra.Comment: 27 pages, 18 Figures, 1 Table. Accepted for publication in A&
Spectroscopy of High-Redshift Supernovae from the ESSENCE Project: The First Four Years
We present the results of spectroscopic observations from the ESSENCE
high-redshift supernova (SN) survey during its first four years of operation.
This sample includes spectra of all SNe Ia whose light curves were presented by
Miknaitis et al. (2007) and used in the cosmological analyses of Davis et al.
(2007) and Wood-Vasey et al. (2007). The sample represents 273 hours of
spectroscopic observations with 6.5 - 10-m-class telescopes of objects detected
and selected for spectroscopy by the ESSENCE team. We present 174 spectra of
156 objects. Combining this sample with that of Matheson et al. (2005), we have
a total sample of 329 spectra of 274 objects. From this, we are able to
spectroscopically classify 118 Type Ia SNe. As the survey has matured, the
efficiency of classifying SNe Ia has remained constant while we have observed
both higher-redshift SNe Ia and SNe Ia farther from maximum brightness.
Examining the subsample of SNe Ia with host-galaxy redshifts shows that
redshifts derived from only the SN Ia spectra are consistent with redshifts
found from host-galaxy spectra. Moreover, the phases derived from only the SN
Ia spectra are consistent with those derived from light-curve fits. By
comparing our spectra to local templates, we find that the rate of objects
similar to the overluminous SN 1991T and the underluminous SN 1991bg in our
sample are consistent with that of the local sample. We do note, however, that
we detect no object spectroscopically or photometrically similar to SN 1991bg.
Although systematic effects could reduce the high-redshift rate we expect based
on the low-redshift surveys, it is possible that SN 1991bg-like SNe Ia are less
prevalent at high redshift.Comment: 21 pages, 17 figures, accepted to A
2D and 3D Core-Collapse Supernovae Simulation Results Obtained with the CHIMERA Code
Much progress in realistic modeling of core-collapse supernovae has occurred
recently through the availability of multi-teraflop machines and the increasing
sophistication of supernova codes. These improvements are enabling simulations
with enough realism that the explosion mechanism, long a mystery, may soon be
delineated. We briefly describe the CHIMERA code, a supernova code we have
developed to simulate core-collapse supernovae in 1, 2, and 3 spatial
dimensions. We then describe the results of an ongoing suite of 2D simulations
initiated from a 12, 15, 20, and 25 solar mass progenitor. These have all
exhibited explosions and are currently in the expanding phase with the shock at
between 5,000 and 20,000 km. We also briefly describe an ongoing simulation in
3 spatial dimensions initiated from the 15 solar mass progenitor.Comment: 5 pages, 3 figure
Probing the Nature of the Vela X Cocoon
Vela X is a pulsar wind nebula (PWN) associated with the active pulsar
B0833-45 and contained within the Vela supernova remnant (SNR). A collimated
X-ray filament ("cocoon") extends south-southwest from the pulsar to the center
of Vela X. VLA observations uncovered radio emission coincident with the
eastern edge of the cocoon and H.E.S.S. has detected TeV -ray emission
from this region as well. Using XMM-\textit{Newton} archival data, covering the
southern portion of this feature, we analyze the X-ray properties of the
cocoon. The X-ray data are best fit by an absorbed nonequilibrium plasma model
with a powerlaw component. Our analysis of the thermal emission shows enhanced
abundances of O, Ne, and Mg within the cocoon, indicating the presence of
ejecta-rich material from the propagation of the SNR reverse shock, consistent
with Vela X being a disrupted PWN. We investigate the physical processes that
excite the electrons in the PWN to emit in the radio, X-ray and -ray
bands. The radio and non-thermal X-ray emission can be explained by synchrotron
emission. We model the -ray emission by Inverse Compton scattering of
electrons off of cosmic microwave background (CMB) photons. We use a
3-component broken power law to model the synchrotron emission, finding an
intrinsic break in the electron spectrum at keV and a
cooling break at 5.5 keV. This cooling break along with
a magnetic field strength of 5 G indicate that the synchrotron
break occurs at 1 keV.Comment: accepted for publication to ApJ
An Investigation into the Character of Pre-Explosion Core-Collapse Supernova Shock Motion
We investigate the structure of the stalled supernova shock in both 2D and 3D
and explore the differences in the effects of neutrino heating and the standing
accretion shock instability (SASI). We find that early on the amplitude of the
dipolar mode of the shock is factors of 2 to 3 smaller in 3D than in 2D.
However, later in both 3D and 2D the monopole and dipole modes start to grow
until explosion. Whereas in 2D the (l,m) = (1,0) mode changes sign
quasi-periodically, producing the "up-and-down" motion always seen in modern 2D
simulations, in 3D this almost never happens. Rather, in 3D when the dipolar
mode starts to grow, it grows in magnitude and wanders stochastically in
direction until settling before explosion to a particular patch of solid angle.
In 2D we find that the amplitude of the dipolar shock deformation separates
into two classes. For the first, identified with the SASI and for a wide range
of "low" neutrino luminosities, this amplitude remains small and roughly
constant. For the other, identified with higher luminosities and
neutrino-driven convection, the dipolar amplitude grows sharply. Importantly,
it is only for this higher luminosity class that we see neutrino-driven
explosions within ~1 second of bounce. Moreover, for the "low" luminosity runs,
the power spectra of these dipolar oscillations peak in the 30-50 Hz range
associated with advection timescales, while for the high-luminosity runs the
power spectra at lower frequencies are significantly more prominent. We
associate this enhanced power at lower frequencies with slower convective
effects and the secular growth of the dipolar shock amplitude. On the basis of
our study, we hypothesize that neutrino-driven buoyant convection should almost
always dominate the SASI when the supernova explosion is neutrino-driven.Comment: Accepted to the Astrophysical Journal; updated with additional
figures and analysi
Pulsar spins from an instability in the accretion shock of supernovae
Rotation-powered radio pulsars are born with inferred initial rotation
periods of order 300 ms (some as short as 20 ms) in core-collapse supernovae.
In the traditional picture, this fast rotation is the result of conservation of
angular momentum during the collapse of a rotating stellar core. This leads to
the inevitable conclusion that pulsar spin is directly correlated with the
rotation of the progenitor star. So far, however, stellar theory has not been
able to explain the distribution of pulsar spins, suggesting that the birth
rotation is either too slow or too fast. Here we report a robust instability of
the stalled accretion shock in core-collapse supernovae that is able to
generate a strong rotational flow in the vicinity of the accreting
proto-neutron star. Sufficient angular momentum is deposited on the
proto-neutron star to generate a final spin period consistent with
observations, even beginning with spherically symmetrical initial conditions.
This provides a new mechanism for the generation of neutron star spin and
weakens, if not breaks, the assumed correlation between the rotational periods
of supernova progenitor cores and pulsar spin.Comment: To be published in Natur
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