626 research outputs found
The Earliest Near-infrared Time-series Spectroscopy of a Type Ia Supernova
We present ten medium-resolution, high signal-to-noise ratio near-infrared
(NIR) spectra of SN 2011fe from SpeX on the NASA Infrared Telescope Facility
(IRTF) and Gemini Near-Infrared Spectrograph (GNIRS) on Gemini North, obtained
as part of the Carnegie Supernova Project. This data set constitutes the
earliest time-series NIR spectroscopy of a Type Ia supernova (SN Ia), with the
first spectrum obtained at 2.58 days past the explosion and covering -14.6 to
+17.3 days relative to B-band maximum. C I {\lambda}1.0693 {\mu}m is detected
in SN 2011fe with increasing strength up to maximum light. The delay in the
onset of the NIR C I line demonstrates its potential to be an effective tracer
of unprocessed material. For the first time in a SN Ia, the early rapid decline
of the Mg II {\lambda}1.0927 {\mu}m velocity was observed, and the subsequent
velocity is remarkably constant. The Mg II velocity during this constant phase
locates the inner edge of carbon burning and probes the conditions under which
the transition from deflagration to detonation occurs. We show that the Mg II
velocity does not correlate with the optical light-curve decline rate
{\Delta}m15. The prominent break at ~1.5 {\mu}m is the main source of concern
for NIR k-correction calculations. We demonstrate here that the feature has a
uniform time evolution among SNe Ia, with the flux ratio across the break
strongly correlated with {\Delta}m15. The predictability of the strength and
the onset of this feature suggests that the associated k-correction
uncertainties can be minimized with improved spectral templates.Comment: 14 pages, 13 figures, accepted for publication in Ap
Delay Times and Rates for Type Ia Supernovae and Thermonuclear Explosions from Double-detonation Sub-Chandrasekhar Mass Models
We present theoretical delay times and rates of thermonuclear explosions that
are thought to produce Type Ia supernovae, including the double-detonation
sub-Chandrasekhar mass model, using the population synthesis binary evolution
code StarTrack. If detonations of sub-Chandrasekhar mass carbon-oxygen white
dwarfs following a detonation in an accumulated layer of helium on the white
dwarf's surface ("double-detonation" models) are able to produce thermonuclear
explosions which are characteristically similar to those of SNe Ia, then these
sub-Chandrasekhar mass explosions may account for at least some substantial
fraction of the observed SN Ia rate. Regardless of whether all
double-detonations look like 'normal' SNe Ia, in any case the explosions are
expected to be bright and thus potentially detectable. Additionally, we find
that the delay time distribution of double-detonation sub-Chandrasekhar mass
SNe Ia can be divided into two distinct formation channels: the 'prompt'
helium-star channel with delay times <500 Myr (~10% of all sub-Chandras), and
the 'delayed' double white dwarf channel, with delay times >800 Myr spanning up
to a Hubble time (~90%). These findings coincide with recent
observationally-derived delay time distributions which have revealed that a
large number of SNe Ia are prompt with delay times <500 Myr, while a
significant fraction also have delay times spanning ~1 Gyr to a Hubble time.Comment: MNRAS Accepted: 13 pages, shortened text, now 3 figure
A Novel Approach to Register Multi-Platform Point Clouds for Rockfall Monitoring
Point cloud produced from technologies such as terrestrial laser scanning (TLS) and photogrammetry (terrestrial and aerial) are widely used in rockfall monitoring applications due to the wealth of data they provide. In such applications, the acquisition and registration of multi-epoch point clouds is necessary. In addition, point clouds can be derived from different sensors (e.g., lasers versus digital cameras) and different platforms (terrestrial versus aerial). Therefore, registration methods should be able to support multi-platform datasets. Currently, registration of multi-platform datasets is done with manual intervention, and automatic registration is difficult. While registration of TLS point clouds can be achieved by targets that are not on the rock surface, this is not the case for photogrammetric methods, as ground control points (GCPs) should be located on the rock surface. Such GCPs can be lost or destroyed with time, and re-establishing them is difficult. Automated registration often relies on feature-based algorithms with refinement using the iterative closest point (ICP) algorithm. This paper presents a novel registration approach of multi-epoch and multi-platform point clouds to support rockfall monitoring applications. The registration method is based on edges that are detected in the different datasets using α-molecules. The paper shows application examples of the novel approach at different rock slopes in Colorado. Results demonstrate that the developed method in many cases performs better than the well-known ICP method and can be used to register point clouds and support rockfall monitoring
3D non-LTE spectrum synthesis for Type Ia supernovae
Despite the importance of Type Ia supernovae as standard candles for
cosmology and to the chemical evolution of the Universe, we still have no
consistent picture of the nature of these events. Much progress has been made
in the hydrodynamical explosion modelling of supernovae Ia in the last few
years and fully 3-D explosion models are now available. However those
simulations are not directly comparable to observations: to constrain explosion
models, radiative transfer calculations must be carried out. We present a new
3-D Monte Carlo radiative transfer code which allows forward modelling of the
spectral evolution of Type Ia supernovae from first principles, using
hydrodynamical explosion models as input. Here, as a first application, we
calculate line-of-sight dependent colour light curves for a toy model of an
off-centre explosion.Comment: 4 pages, 1 figure, presented at the conference "Probing Stellar
Populations out to the Distant Universe" (Cefalu, Italy, Sept. 2008
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae
Gravitational settling of 22Ne in cooling white dwarfs can affect the outcome
of thermonuclear supernovae. We investigate how the supernova energetics and
nucleosynthesis are in turn influenced by this process. We use realistic
chemical profiles derived from state-of-the-art white dwarf cooling sequences.
The cooling sequences provide a link between the white dwarf chemical structure
and the age of the supernova progenitor system. The cooling sequence of a 1
M_sun white dwarf was computed until freezing using an up-to-date stellar
evolutionary code. We computed explosions of both Chandrasekhar mass and
sub-Chandrasekhar mass white dwarfs, assuming spherical symmetry and neglecting
convective mixing during the pre-supernova carbon simmering phase to maximize
the effects of chemical separation. Neither gravitational settling of 22Ne nor
chemical differentiation of 12C and 16O have an appreciable impact on the
properties of Type Ia supernovae, unless there is a direct dependence of the
flame properties (density of transition from deflagration to detonation) on the
chemical composition. At a fixed transition density, the maximum variation in
the supernova magnitude obtained from progenitors of different ages is ~0.06
magnitudes, and even assuming an unrealistically large diffusion coefficient of
22Ne it would be less than ~0.09 mag. However, if the transition density
depends on the chemical composition (all other things being equal) the oldest
SNIa can be as much as 0.4 magnitudes brighter than the youngest ones (in our
models the age difference is 7.4 Gyr). In addition, our results show that 22Ne
sedimentation cannot be invoked to account for the formation of a central core
of stable neutron-rich Fe-group nuclei in the ejecta of sub-Chandrasekhar
models, as required by observations of Type Ia supernovae.Comment: 8 pages, 8 figures, 3 tables, accepted for Astronomy and
Astrophysics. Revised version with corrected typo
500 Days of SN 2013dy: spectra and photometry from the ultraviolet to the infrared
SN 2013dy is a Type Ia supernova for which we have compiled an extraordinary
dataset spanning from 0.1 to ~ 500 days after explosion. We present 10 epochs
of ultraviolet (UV) through near-infrared (NIR) spectra with HST/STIS, 47
epochs of optical spectra (15 of them having high resolution), and more than
500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and
slowly declining light curve (delta m(B) = 0.92 mag), shallow Si II 6355
absorption, and a low velocity gradient. We detect strong C II in our earliest
spectra, probing unburned progenitor material in the outermost layers of the SN
ejecta, but this feature fades within a few days. The UV continuum of SN
2013dy, which is strongly affected by the metal abundance of the progenitor
star, suggests that SN 2013dy had a relatively high-metallicity progenitor.
Examining one of the largest single set of high-resolution spectra for a SN Ia,
we find no evidence of variable absorption from circumstellar material.
Combining our UV spectra, NIR photometry, and high-cadence optical photometry,
we construct a bolometric light curve, showing that SN 2013dy had a maximum
luminosity of 10.0^{+4.8}_{-3.8} * 10^{42} erg/s. We compare the synthetic
light curves and spectra of several models to SN 2013dy, finding that SN 2013dy
is in good agreement with a solar-metallicity W7 model.Comment: 22 pages, 18 figures, replaced with version accecpted for publication
in MNRA
Theory of "ferrisuperconductivity" in
We construct a two component Ginzburg-Landau theory with coherent pair motion
and incoherent quasiparticles for the phase diagram of .
The two staggered superconducting states live at the Brillouin zone center and
the zone boundary, and coexist for temperatures at concentrations
. We predict below
appearance of a charge density wave (CDW) and Be-sublattice distortion. The
distortion explains the SR relaxation anomaly, and Th-impurity mediated
scattering of ultrasound to CDW fluctuations explains the attenuation peak.Comment: 4 pages, 4 eps figures, REVTe
Punctuated Shutdown of Atlantic Meridional Overturning Circulation during Greenland Stadial 1.
The Greenland Stadial 1 (GS-1; ~12.9 to 11.65 kyr cal BP) was a period of North Atlantic cooling, thought to have been initiated by North America fresh water runoff that caused a sustained reduction of North Atlantic Meridional Overturning Circulation (AMOC), resulting in an antiphase temperature response between the hemispheres (the 'bipolar seesaw'). Here we exploit sub-fossil New Zealand kauri trees to report the first securely dated, decadally-resolved atmospheric radiocarbon ((14)C) record spanning GS-1. By precisely aligning Southern and Northern Hemisphere tree-ring (14)C records with marine (14)C sequences we document two relatively short periods of AMOC collapse during the stadial, at ~12,920-12,640 cal BP and 12,050-11,900 cal BP. In addition, our data show that the interhemispheric atmospheric (14)C offset was close to zero prior to GS-1, before reaching 'near-modern' values at ~12,660 cal BP, consistent with synchronous recovery of overturning in both hemispheres and increased Southern Ocean ventilation. Hence, sustained North Atlantic cooling across GS-1 was not driven by a prolonged AMOC reduction but probably due to an equatorward migration of the Polar Front, reducing the advection of southwesterly air masses to high latitudes. Our findings suggest opposing hemispheric temperature trends were driven by atmospheric teleconnections, rather than AMOC changes
Superconductivity and Antiferromagnetism: Hybridization Impurities in a Two-Band Spin-Gapped Electron System
We present the exact solution of a one-dimensional model of a spin-gapped
correlated electron system with hybridization impurities exhibiting both
magnetic and mixed-valence properties. The host supports superconducting
fluctuations, with a spin gap. The localized electrons create a band of
antiferromagnetic spin excitations inside the gap for concentrations x of the
impurities below some critical value x_c. When x = x_c the spin gap closes and
a ferrimagnetic phase appears. This is the first example of an exactly solvable
model with coexisting superconducting and antiferromagnetic fluctuations which
in addition supports a quantum phase transition to a (compensated)
ferrimagnetic phase. We discuss the possible relevance of our results for
experimental systems, in particular the U-based heavy-fermion materials.Comment: 4 page
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