249 research outputs found
Exploring the perceptions of cognitive and affective capabilities of four, real, physical robots with a decreasing degree of morphological human likeness.
A Catalog of Near Infrared Spectra from Type Ia Supernovae
We present forty-one near infrared (NIR, 0.7-2.5 microns) spectra from normal
Type Ia supernovae (SNe Ia) obtained at epochs ranging from fourteen days
before to seventy-five days with respect to the maximum light date in the
V-band. All data were obtained at the IRTF using the SpeX instrument. We
identify many spectral features, measure the Doppler velocities, and discuss
the chemical distribution of explosion products in SNe Ia. We describe
procedures for smoothing data, fitting continua, and measuring absorption
features to insure consistency for measurement and analysis.
This sample provides the first opportunity to examine and compare a large
number of SNe Ia in this wavelength region. NIR data are a rich source of
information about explosion products whose signatures are blended or obscured
in other spectral regions and NIR observations probe a greater radial depth
than optical wavelengths. We analyze similarities and differences in the
spectra and we show that the progressive development of spectral features for
normal SNe Ia in the NIR is consistent with time.
Measured Doppler velocities indicate that burning products in SNe Ia are
distributed in distinct layers with no large scale mixing. Carbon is not
detected in these data, in agreement with previous results with NIR data
establishing very low limits on carbon abundance in SNe Ia. Carbon burning
products, O and Mg, are plentiful in the outer layers suggesting that the
entire progenitor is burned in the explosion. The data provide a resource for
investigations of cross-correlations with other data libraries that may further
constrain SN Ia physics and improve the effectiveness of SNe Ia as cosmological
distance indicators.Comment: Accepted to The Astronomical Journal: 81 pages, 6 tables, 21 figure
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
Jet-Induced Explosions of Core Collapse Supernovae
We numerically studied the explosion of a supernova caused by supersonic jets
present in its center. The jets are assumed to be generated by a
magneto-rotational mechanism when a stellar core collapses into a neutron star.
We simulated the process of the jet propagation through the star, jet
breakthrough, and the ejection of the supernova envelope by the lateral shocks
generated during jet propagation. The end result of the interaction is a highly
nonspherical supernova explosion with two high-velocity jets of material moving
in polar directions, and a slower moving, oblate, highly distorted ejecta
containing most of the supernova material. The jet-induced explosion is
entirely due to the action of the jets on the surrounding star and does not
depend on neutrino transport or re-acceleration of a stalled shock. The jet
mechanism can explain the observed high polarization of Type Ib,c and Type II
supernovae, pulsar kicks, very high velocity material observed in supernova
remnants, indications that radioactive material was carried to the
hydrogen-rich layers in SN1987A, and some others observations that are very
difficult or impossible to explain by the neutrino energy deposition mechanism.
The breakout of the jet from a compact, hydrogen- deficient core may account
for the gamma-ray bursts and radio outburst associated with SN1998bw/GRB980425.Comment: 14 pages, LaTeX, aaspp4.sty, epsf.sty, submitted to ApJ Let
COMPTEL upper limits for the 56Co gamma-ray emission from SN1998bu
Supernova 1998bu in the galaxy M96 was observed by COMPTEL for a total of 88
days starting 17 days after the explosion. We searched for a signal in the 847
keV and 1238 keV lines of radioactive 56Co from this type Ia supernova. Using
several different analysis methods, we did not detect SN1998bu. Our
measurements should have been sensitive enough to detect 60Co gamma-rays as
predicted from supernova models. Our 2-sigma flux limit is 2.3 10^{-5} photons
cm^{-2} s^{-1}; this would correspond to 0.35 solar mass of ejected 56Ni, if
SN1998bu were at a distance of 11.3 Mpc and transparent to MeV gamma rays for
the period of our measurements. We discuss our measurements in the context of
common supernova models, and conclude disfavoring a supernova event with large
mixing and major parts of the freshly-generated radioactivity in outer layers.Comment: 8 pages, 6 EPS-figures, Latex2e, aa.cls needed, accepted for
publication in A&
A Study of Carbon Features in Type Ia Supernova Spectra
One of the major differences between various explosion scenarios of Type Ia
supernovae (SNe Ia) is the remaining amount of unburned (C+O) material and its
velocity distribution within the expanding ejecta. While oxygen absorption
features are not uncommon in the spectra of SNe Ia before maximum light, the
presence of strong carbon absorption has been reported only in a minority of
objects, typically during the pre-maximum phase. The reported low frequency of
carbon detections may be due to low signal-to-noise data, low abundance of
unburned material, line blending between C II 6580 and Si II 6355, ejecta
temperature differences, asymmetrical distribution effects, or a combination of
these. However, a survey of published pre-maximum spectra reveals that more SNe
Ia than previously thought may exhibit C II 6580 absorption features and relics
of line blending near 6300 Angstroms. Here we present new SN Ia observations
where spectroscopic signatures of C II 6580 are detected, and investigate the
presence of C II 6580 in the optical spectra of 19 SNe Ia using the
parameterized spectrum synthesis code, SYNOW. Most of the objects in our sample
that exhibit C II 6580 absorption features are of the low-velocity gradient
subtype. Our study indicates that the morphology of carbon-rich regions is
consistent with either a spherical distribution or a hemispheric asymmetry,
supporting the recent idea that SN Ia diversity may be a result of off-center
ignition coupled with observer line-of-sight effects.Comment: 10 papges, 9 figures, 3 table
Optical polarimetric monitoring of the type II-plateau SN 2005af
Aims. Core-collapse supernovae may show significant polarization that implies
non-spherically symmetric explosions. We observed the type II-plateau SN 2005af
using optical polarimetry in order to verify whether any asphericity is present
in the supernova temporal evolution. Methods. We used the IAGPOL imaging
polarimeter to obtain optical linear polarization measurements in R (five
epochs) and V (one epoch) broadbands. Interstellar polarization was estimated
from the field stars in the CCD frames. The optical polarimetric monitoring
began around one month after the explosion and lasted ~30 days, between the
plateau and the early nebular phase. Results. The weighted mean observed
polarization in R band was [1.89 +/- 0.03]% at position angle (PA) 54 deg.
After foreground subtraction, the level of the average intrinsic polarization
for SN 2005af was ~0.5% with a slight enhancement during the plateau phase and
a decline at early nebular phase. A rotation in PA on a time scale of days was
also observed. The polarimetric evolution of SN 2005af in the observed epochs
is consistent with an overall asphericity of ~20% and an inclination of ~30
deg. Evidence for a more complex, evolving asphericity, possibly involving
clumps in the SN 2005af envelope, is found.Comment: 6 pages, 5 figures, to be published A&
Neutral and charged excitons interplay in non-uniformly strain-engineered WS2
We investigate the response of excitons in two-dimensional semiconductors to nonuniformity of mechanical strain. In our approach to non-uniform strain-engineering, a WS2 monolayer is suspended over a triangular hole. Large (>2%), strongly non-uniform (>0.28% µm–1), and in-situ tunable strain is induced in WS2 by pressurizing it with inert gas. We observe a pronounced shift of the spectral weight from neutral to charged excitons at the center of the membrane, in addition to well-known strain-dependent bandgap modification. We show that the former phenomenon is a signature of a new effect unique for non-uniform strain: funneling of free carriers towards the region of high strain followed by neutral to charged exciton conversion. Our result establishes non-uniform strain engineering as a novel and useful experimental 'knob' for tuning optoelectronic properties of 2D semiconductors
Interpreting the near-infrared spectra of the 'golden standard' Type Ia supernova 2005cf
We present nine near-infrared (NIR) spectra of supernova (SN) 2005cf at
epochs from -10 d to +42 d with respect to B-band maximum, complementing the
existing excellent data sets available for this prototypical Type Ia SN at
other wavelengths. The spectra show a time evolution and spectral features
characteristic of normal Type Ia SNe, as illustrated by a comparison with SNe
1999ee, 2002bo and 2003du. The broad-band spectral energy distribution (SED) of
SN 2005cf is studied in combined ultraviolet (UV), optical and NIR spectra at
five epochs between ~ 8 d before and ~ 10 d after maximum light. We also
present synthetic spectra of the hydrodynamic explosion model W7, which
reproduce the key properties of SN 2005cf not only at UV-optical as previously
reported, but also at NIR wavelengths. From the radiative-transfer calculations
we infer that fluorescence is the driving mechanism that shapes the SED of SNe
Ia. In particular, the NIR part of the spectrum is almost devoid of absorption
features, and instead dominated by fluorescent emission of both iron-group
material and intermediate-mass elements at pre-maximum epochs, and pure
iron-group material after maximum light. A single P-Cygni feature of Mg II at
early epochs and a series of relatively unblended Co II lines at late phases
allow us to constrain the regions of the ejecta in which the respective
elements are abundant.Comment: 11 pages, 6 figures, accepted for publication in MNRA
Type Ia supernova SN 2003du: optical observations
UBVRI photometry and optical spectra of type Ia supernova SN 2003du obtained
at the Indian Astronomical Observatory for nearly a year since discovery are
presented.
The apparent magnitude at maximum was B=13.53 +/- 0.02 mag, and the colour
(B-V) = -0.08 +/- 0.03 mag. The luminosity decline rate, Delta(m_{15}(B)) =
1.04 +/- 0.04 mag indicates an absolute B magnitude at maximum of M_B = -19.34
+/- 0.3 mag and the distance modulus to the parent galaxy as mu=32.89 +/-
0.4.The light curve shapes are similar, though not identical, to those of SNe
1998bu and 1990N, both of which had luminosity decline rates similar to that of
SN 2003du and occurred in spiral galaxies. The peak bolometric luminosity
indicates that 0.9 Msun mass of 56Ni was ejected by the supernova. The spectral
evolution and the evolution of the Si II and Ca II absorption velocities
closely follows that of SN 1998bu, and in general, is within the scatter of the
velocities observed in normal type Ia supernovae.
The spectroscopic and photometric behaviour of SN 2003du is quite typical for
SNe Ia in spirals.
A high velocity absorption component in the Ca II (H & K) and IR-triplet
features, with absorption velocities of ~20,000 km/s and ~22,000 km/s
respectively, is detected in the pre-maximum spectra of days -11 and -7.Comment: 10 pages, 10 figures; Accepted for publication in A&
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