361 research outputs found
Spectral Signatures of Gravitationally Confined Thermonuclear Supernova Explosions
We consider some of the spectral and polarimetric signatures of the
gravitational confined detonation scenario for Type Ia supernova explosions. In
this model, material produced by an off-center deflagration (which itself fails
to produce the explosion) forms a metal-rich atmosphere above the white dwarf
surface. Using hydrodynamical simulations, we show that this atmosphere is
compressed and accelerated during the subsequent interaction with the supernova
ejecta. This leads ultimately to the formation of a high-velocity pancake of
metal-rich material that is geometrically detached from the bulk of the ejecta.
When observed at the epochs near maximum light, this absorbing pancake produces
a highly blueshifted and polarized calcium IR triplet absorption feature
similar to that observed in several Type~Ia supernovae. We discuss the
orientation effects present in our model and contrast them to those expected in
other supernova explosion models. We propose that a large sample of
spectropolarimetric observations can be used to critically evaluate the
different theoretical scenarios.Comment: 4 pages, 3 figures. To appear in ApJ Letters. For higher resolution
images and movies see http://panisse.lbl.gov/~dnkasen/gcd.htm
Two-Dimensional Hydrodynamic Models of Super Star Clusters with a Positive Star Formation Feedback
Using the hydrodynamic code ZEUS, we perform 2D simulations to determine the
fate of the gas ejected by massive stars within super star clusters. It turns
out that the outcome depends mainly on the mass and radius of the cluster. In
the case of less massive clusters, a hot high velocity ( km
s) stationary wind develops and the metals injected by supernovae are
dispersed to large distances from the cluster. On the other hand, the density
of the thermalized ejecta within massive and compact clusters is sufficiently
large as to immediately provoke the onset of thermal instabilities. These
deplete, particularly in the central densest regions, the pressure and the
pressure gradient required to establish a stationary wind, and instead the
thermally unstable parcels of gas are rapidly compressed, by a plethora of
re-pressurizing shocks, into compact high density condensations. Most of these
are unable to leave the cluster volume and thus accumulate to eventually feed
further generations of star formation.
The simulations cover an important fraction of the parameter-space, which
allows us to estimate the fraction of the reinserted gas which accumulates
within the cluster and the fraction that leaves the cluster as a function of
the cluster mechanical luminosity, the cluster size and heating efficiency.Comment: Accepted for publication in ApJ; 27 pages, 9 figures, 1 tabl
Crushing of interstellar gas clouds in supernova remnants II. X-ray emission
AIMS. We study and discuss the time-dependent X-ray emission predicted by hydrodynamic modeling of the interaction of a SNR shock wave with an interstellar gas cloud. The scope includes: 1) to study the correspondence between modeled and X-ray emitting structures, 2) to explore two different physical regimes in which either thermal conduction or radiative cooling plays a dominant role, and 3) to investigate the effects of the physical processes at work on the emission of the shocked cloud in the two different regimes. METHODS. We use a detailed hydrodynamic model, including thermal conduction and radiation, and explore two cases characterized by different Mach numbers of the primary shock: M = 30 in which the cloud dynamics is dominated by radiative cooling and M = 50 dominated by thermal conduction. From the simulations, we synthesize the expected X-ray emission, using available spectral codes. RESULTS. The morphology of the X-ray emitting structures is significantly different from that of the flow structures originating from the shock-cloud interaction. The hydrodynamic instabilities are never clearly visible in the X-ray band. Shocked clouds are preferentially visible during the early phases of their evolution. Thermal conduction and radiative cooling lead to two different phases of the shocked cloud: a cold cooling dominated core emitting at low energies and a hot thermally conducting corona emitting in the X-ray band. The thermal conduction makes the X-ray image of the cloud smaller, more diffuse, and shorter-lived than that observed when thermal conduction is neglected
3D AMR hydrosimulations of a compact source scenario for the Galactic Centre cloud G2
The nature of the gaseous and dusty cloud G2 in the Galactic Centre is still
under debate. We present three-dimensional hydrodynamical adaptive mesh
refinement (AMR) simulations of G2, modeled as an outflow from a "compact
source" moving on the observed orbit. The construction of mock
position-velocity (PV) diagrams enables a direct comparison with observations
and allow us to conclude that the observational properties of the gaseous
component of G2 could be matched by a massive () and slow ()
outflow, as observed for T Tauri stars. In order for this to be true, only the
material at larger () distances from the source must be
actually emitting, otherwise G2 would appear too compact compared to the
observed PV diagrams. On the other hand, the presence of a central dusty source
might be able to explain the compactness of G2's dust component. In the present
scenario, 5-10 years after pericentre the compact source should decouple from
the previously ejected material, due to the hydrodynamic interaction of the
latter with the surrounding hot and dense atmosphere. In this case, a new
outflow should form, ahead of the previous one, which would be the smoking gun
evidence for an outflow scenario.Comment: resubmitted to MNRAS after referee report, 16 pages, 11 figure
Crushing of interstellar gas clouds in supernova remnants. I. The role of thermal conduction and radiative losses
We model the hydrodynamic interaction of a shock wave of an evolved supernova
remnant with a small interstellar gas cloud like the ones observed in the
Cygnus loop and in the Vela SNR. We investigate the interplay between radiative
cooling and thermal conduction during cloud evolution and their effect on the
mass and energy exchange between the cloud and the surrounding medium. Through
the study of two cases characterized by different Mach numbers of the primary
shock (M = 30 and 50, corresponding to a post-shock temperature K and K, respectively), we explore two
very different physical regimes: for M = 30, the radiative losses dominate the
evolution of the shocked cloud which fragments into cold, dense, and compact
filaments surrounded by a hot corona which is ablated by the thermal
conduction; instead, for M = 50, the thermal conduction dominates the evolution
of the shocked cloud, which evaporates in a few dynamical time-scales. In both
cases we find that the thermal conduction is very effective in suppressing the
hydrodynamic instabilities that would develop at the cloud boundaries.Comment: 18 pages, 11 figures, A&A in press, full res. paper at
http://www.astropa.unipa.it/Library/OAPA_preprints/orl_AA_2896.ps.g
Can Light Echoes Account for the Slow Decay of Type IIn Supernovae?
The spectra of type IIn supernovae indicate the presence of apre-existing
slow, dense circumstellar wind (CSW). If the CSW extends sufficiently far from
the progenitor star, then dust formation should occur in the wind. The light
from the supernova explosion will scatter off this dust and produce a light
echo. Continuum emission seen after the peak will have contributions from both
this echo as well as from the shock of the ejecta colliding with the CSW, with
a fundamental question of which source dominates the continuum. We calculate
the brightness of the light echo as a function of time for a range of dust
shell geometries, and use our calculations to fit to the light curves of SN
1988Z and SN 1997ab, the two slowest declining IIn supernovae on record. We
find that the light curves of both objects can be reproduced by the echo model.
However, their rate of decay from peak, color at peak and their observed peak
absolute magnitudes when considered together are inconsistent with the echo
model. Furthermore, when the observed values of M are corrected for the
effects of dust scattering, the values obtained imply that these supernovae
have unrealistically high luminosities. We conclude that light echoes cannot
properly account for the slow decline seen in some IIn's, and that the shock
interaction is likely to dominate the continuum emission.Comment: 15 pages, 9 figure
The Post-Pericenter Evolution of the Galactic Center Source G2
In early 2014 the fast-moving near-infrared source G2 reached its closest
approach to the supermassive black hole Sgr A* in the Galactic Center. We
report on the evolution of the ionized gaseous component and the dusty
component of G2 immediately after this event, revealed by new observations
obtained in 2015 and 2016 with the SINFONI integral field spectrograph and the
NACO imager at the ESO VLT. The spatially resolved dynamics of the Br
line emission can be accounted for by the ballistic motion and tidal shearing
of a test-particle cloud that has followed a highly eccentric Keplerian orbit
around the black hole for the last 12 years. The non-detection of a drag force
or any strong hydrodynamic interaction with the hot gas in the inner accretion
zone limits the ambient density to less than a few 10 cm at the
distance of closest approach (1500 ), assuming G2 is a spherical cloud
moving through a stationary and homogeneous atmosphere. The dust continuum
emission is unresolved in L'-band, but stays consistent with the location of
the Br emission. The total luminosity of the Br and L' emission
has remained constant to within the measurement uncertainty. The nature and
origin of G2 are likely related to that of the precursor source G1, since their
orbital evolution is similar, though not identical. Both object are also likely
related to a trailing tail structure, which is continuously connected to G2
over a large range in position and radial velocity.Comment: 17 pages, 12 figures; accepted for publication in Ap
Rayleigh-Taylor instability with self-generated magnetic field and thermal conduction in 2D
High energy density laboratory experiments on Rayleigh-Taylor instability (RTI) [1] in nonlinear regime show the plasma behavior significantly different from classical simulation results. We include the effects of self-generated magnetic field and heat conduction in simulations aiming to improve agreement with experiments. We find maximum magnetic fields generated ~11MG (β=0.091) without heat conduction (κ=0), field growth saturated by t=20ns; and ~1.7 MG with heat conduction taken into account. Strong magnetic fields in κ=0 simulations affect flow dynamics, new modes are generated. Effect of weaker magnetic fields in simulations with physical values of κ is insignificant; the main difference with classical RTI simulations is suppressed small scale features. In none of the simulations are mass extensions observed.В экспериментах неустойчивости Рэлея-Тэйлора (НРТ) в лабораториях высоких плотностей энергии [1] поведение жидкости существенно отличается от классических результатов численного моделирования. С целью улучшить согласие с экспериментами мы включили в моделирование эффекты самогенерирующегося магнитного поля и теплопроводности. Максимальное магнитное поле получено ~11 MG (β=0.091) в отсутствие теплопроводности (κ=0), рост поля насыщается к t=20 ns; и ~1.7 MG при учтённой теплопроводности. Сильное магнитное поле в модели с κ=0 меняет динамику неустойчивости, генерируются новые моды. Эффект более слабого поля в моделировании с физическими значениями κ несуществен; основное отличие от классической НРТ заключается в подавлении мелкомасштабных структур. Удлинения РТ структур в моделях не наблюдалось.У експериментах нестійкості Релея-Тейлора (НРТ) в лабораторіях великих щільностей енергії [1] поведінка рідини суттєво відрізняється від класичних результатів чисельного моделювання. Для узгодження з експериментами ми включили в моделювання ефекти магнітного поля, що самогенерується, та теплопровідності. Максимальне магнітне поле одержано ~11 MG (β=0.091) за відсутностю теплопровідності (κ=0), зростання поля насичується до t=20 ns; та ~1.7 MG, коли теплопровідність врахована. Сильне магнітне поле в моделі з κ=0 змінює динаміку нестійкості, генеруються нові моди. Ефект більш слабкого поля при моделюванні з фізичними значеннями κ несуттєвий; головною відмінністю від класичної НРТ є нерозвиненість дрібномасштабних структур. Подовження РТ структур в моделях не помічалося
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