abstract stringlengths 3 192k | title stringlengths 4 857 |
|---|---|
supernova remnant rx j1713.7-3946 has exhibited the largest surface brightness and a detailed spectral and shell-type morphology, and is one of the brightest tev sources. the recent h.e.s.s. observation of rx j1713.7-3946 revealed a broken power-law gev-tev gamma-ray and a more extended gamma-ray spatial radial profile... | radial profiles of non-thermal emission from supernova remnant rx j1713.7-3946 |
currently there is considerable interest in creating scalable laboratory plasmas to study the mechanisms behind the formation and evolution of astrophysical phenomena such as herbig-haro objects and supernova remnants. laboratory-scaled experiments can provide a well diagnosed and repeatable supplement to direct observ... | role of collisionality and radiative cooling in supersonic plasma jet collisions of different materials |
we present high spatial resolution, integral field spectrograph (ifs) observations of the nearby low-ionization nuclear emission-line region (liner) galaxy ngc 404 at 1.25 μm (j band) and 2.2 μm (k band) near-infrared (nir) wavelengths. although ngc 404 is thought to host an intermediate-mass black hole (bh) at its cen... | widespread shocks in the nucleus of ngc 404 revealed by near-infrared integral field spectroscopy |
up to 1987, supernovae (sne) and supernova remnants (snrs) had been thought to be hostile environments for molecules and dust grains. fast-moving electrons in young sne can destroy molecules, and strong x-ray radiation and shocks can destroy molecules and dust grains in snrs. that concept was broken by detection of co,... | dust and molecular formation in supernovae |
context. messier 81 has the nearest active nucleus with broad hα emission. a detailed study of this galaxy's centre is important for understanding the innermost structure of the agn phenomenon.aims: our goal is to seek previously undetected structures using additional techniques to reanalyse a data cube obtained with t... | a hot bubble at the centre of m 81 |
tycho's supernova remnant (snr) is well-established as a source of particle acceleration to very high energies. constraints from numerous studies indicate that the observed gamma-ray emission results primarily from hadronic processes, providing direct evidence of highly relativistic ions that have been accelerated by t... | erratum: "a cr-hydro-nei model of the structure and broadband emission from tycho\'s supernova remnant" (2014, apj, 783, 33) |
using data from the galactic arecibo l-band feed array continuum transit survey, we report the discovery of two previously unidentified, very compressed, thin, and straight polarized filaments approximately centered at galactic coordinates, (l, b) = (182.°5, - 4.°0), which we call g182.5-4.0. using data from the isaac ... | discovery of a filamentary synchrotron structure connected to the coherent magnetic field in the outer galaxy |
laming predicted that the narrow balmer line core of the ∼3000 km s-1 shock in the sn 1006 remnant would be significantly polarized due to electron and proton impact polarization. here, based on deep spectrally resolved polarimetry obtained with the european southern observatory (eso)’s very large telescope (vlt), we r... | discovery of polarized line emission in sn 1006 |
we present a multiwavelength examination of the supernova remnant (snr) s26 in the nearby galaxy ngc 300 using data from chandra x-ray observatory, xmm-newton x-ray observatory, hubble space telescope (hst), the very large array, and the australia telescope compact array. we simultaneously fit all of the available x-ra... | multiwavelength study of the x-ray bright supernova remnant n300-s26 in ngc 300 |
we discuss the recent developments in the theory of diffusive shock acceleration (dsa) by using both first-principle kinetic plasma simulations and analytical theory based on the solution of the convection/diffusion equation. in particular, we show how simulations reveal that the spectra of accelerated particles are si... | the issue with diffusive shock acceleration |
young supernova remnants are the sources of a broadband nonthermal synchrotron continuum emission from radio to x-rays produced by accelerated electrons. diffusive shock acceleration (dsa) of relativistic particles is accompanied by strong amplification of the turbulent magnetic field. this is an intrinsic feature of a... | polarized synchrotron x-ray emission from supernova shells: xipe/ixpe perspective |
knowledge about the magnetic fields in supernova remnants (snrs) is of paramount importance for constraining galactic cosmic ray acceleration models. it could also indirectly provide information on the interstellar magnetic fields. in this paper, we predict the faraday dispersion functions (fdfs) of snrs for the first ... | on the potential of faraday tomography to identify shock structures in supernova remnants |
abstract—giant h i shells of several hundred parsecs and larger observed in nearby galaxies with a moderate inclination ($i \lesssim $ 50°) are formed by multiple supernova explosions in stellar clusters. to estimate the total energy of these supernovae the relation obtained for the evolution of a single supernova in a... | energy budget in supernovae-driven h i shells |
the collisional pumping of oh masers in non-dissociative c-type shocks near supernova remnants is considered. the emergence of maser emission in oh lines is investigated for various shock parameters—the shock speed, the preshock gas density, the cosmic-ray ionization rate, and the magnetic field strength. the largest o... | collisional pumping of oh masers near supernova remnants |
models for supernova remnant (snr) evolution can be used to determine the energy of the explosion, the age of the snr, and the density of the surrounding medium by matching observations. observed snr properties derived from the x-ray spectrum include the electron temperature (kte) and emission measure (em) of the shock... | the effects of elemental abundances on fitting supernova remnant models to data |
relativistic particle acceleration in collisionless shocks of supernova remnants is accompanied with magnetic field amplification by cosmic ray (cr) driven plasma instabilities. bell’s fast cr-current instability is predicted to produce turbulence with a non-zero mean electric field in the shock precursor. we present a... | monte carlo modelling of particle acceleration in collisionless shocks with effective mean electric field |
thermal x-ray emission from young supernova remnants (snrs) is usually dominated by the emission lines of the supernova ejecta, which are widely believed to be crossed and thus heated by the inward-propagating reverse shock (rs). previous works using x-ray imaging data have shown that the ejecta are heated by the rs by... | reverse-shock in tycho’s supernova remnant |
this paper reports on the suzaku result of the galactic supernova remnant (snr) g337.2-0.7. the x-ray spectrum is well explained by three components in ionizing phase. one is a plasma with a low temperature kt = 0.70_{-0.03}^{+0.02}kev, solar abundances, and an ionization parameter n_et = 5.7^{+0.7}_{-0.4}× 10^{11}s cm... | x-ray study of the supernova remnant g337.2-0.7 |
we report new co observations and a detailed molecular-line study of the mixed morphology supernova remnant g359.1-0.5, which contains six oh (1720 mhz) masers along the radio shell, indicative of shock-cloud interaction. observations of 12co and 13co j:1-0 lines were performed in a ∼38 × 38 arcmin area with the on-the... | molecular environments of the supernova remnant g359.1-0.5 |
we present an unbiased spectroscopic study of the galactic supernova remnant (snr) cygnus loop using the large sky area multi-object fiber spectroscopic telescope (lamost) dr5. lamost features both a large field of view and a large aperture, which allow us to simultaneously obtain 4000 spectra at ∼3700-9000 šwith r ≈ 1... | unbiased spectroscopic study of the cygnus loop with lamost. i. optical properties of emission lines and the global spectrum |
we present the first ccd images of the vro 42.05.01 (g 166.0+4.3) supernova remnant in hα+[n ii], [o iii] 5007 and [s ii] at a moderate angular resolution. low and high-dispersion spectroscopy was also performed at selected areas around this extended remnant. diagnostic diagrams of the line intensities from the present... | a deep optical study of the supernova remnant g 166+4.3 (vro) |
the sprite cubesat is a recently selected nasa astrophysics mission designed to measure ionizing radiation escape from star-forming galaxies, and to map far-ultraviolet (1000 - 1750 å) emission from shocked regions in supernova remnants. the instrument leverages a number of new technologies identified for future large ... | high-sensitivity far-ultraviolet imaging spectroscopy with the sprite cubesat |
we performed near-infrared line mapping of the supernova remnant ic 443 with the irsf 1.4-m telescope, using the narrow-band filters tuned for [fe ii] 1.257 μm, [fe ii] 1.644 μm, and paβ. we detected the [fe ii] and paβ emissions from a very wide area of the observed region (30‧ ×35‧). these line intensity maps reveal ... | a study of iron and dust in the supernova remnant ic 443 |
plasma effects, such as the multi-component kinetic diffusion and self-generated electromagnetic fields, are recognized as a pivotal key to understanding the physics of interface evolution in inertial confinement fusion and supernova remnants. in this work, a two-dimensional hybrid fluid-pic code is used to investigate... | ion kinetic effects on the evolution of richtmyer–meshkov instability and interfacial mix |
the fast stellar winds of massive stars, along with supernovae, determine the dynamics within the star-forming regions. within a compact star cluster, counterpropagating supersonic mhd shock flows associated with winds and supernova remnants can provide favorable conditions for efficient fermi i particle acceleration u... | wind of a young massive star colliding with a supernova remnant shell |
the observed hardening of the spectra of cosmic ray protons and helium nuclei is studied within the model of nonlinear diffusive shock acceleration of supernova remnants (snrs). in this model, the injected particles with energies below the spectral " knee" are assumed to be described by two populations with different s... | spectral hardening of cosmic ray protons and helium nuclei in supernova remnant shocks |
we report the results of xmm-newton observations of the galactic mixed-morphology supernova remnant g350.0-2.0. diffuse thermal x-ray emission fills the north-western part of the remnant surrounded by radio shell-like structures. we did not detect any x-ray counterpart of the latter structures, but found several bright... | xmm-newton studies of the supernova remnant g350.0-2.0 |
a large number of supernova remnants (snrs) in our galaxy and galaxies nearby have been resolved in various radio bands. this radio emission is thought to be produced via synchrotron emission from electrons accelerated by the shock that the supernova ejecta drives into the external medium. here we consider the sample o... | radio snrs in the magellanic clouds as probes of shock microphysics |
extragalactic jets are launched from the innermost regions of galaxies, near the central supermassive black hole. as they propagate, they must cross the whole galaxy, and in this process they interact with a variety of obstacles; including gas clouds, populations of stars or even supernova remnants. the interaction bet... | the interaction of agn jets with obstacles |
the supernova remnant (snr) n49b in the large magellanic cloud is a peculiar example of a core-collapse snr that shows the shocked metal-rich ejecta enriched only in mg without evidence for a similar overabundance in o and ne. based on archival chandra data, we present results from our extensive spatially resolved spec... | spatial distribution of mg-rich ejecta in lmc supernova remnant n49b |
we searched for x-ray supernova remnants (snrs) in the starburst region of m 82, using archival data from the chandra x-ray observatory with a total effective exposure time of 620 ks with an x-ray spectroscopic selection. strong line emission from fe xxv at 6.7 kev is a characteristic spectral feature of hot, shocked g... | x-ray supernova remnants in the starburst region of m 82 |
dense, fast-moving ejecta knots in supernova remnants are prime sites for molecule and dust formation. we present sofia far-ir spectrometer fifi-ls observations of co-rich knots in cas a which cover a ~1 square arc minute area of the northern shell, in the [o iii] 52 and 88 micron and [o i] 63 micron lines. the fifi-ls... | sofia far-infrared [o iii] and [o i] observations of dense co-knots in the supernova remnant cassiopeia a: multi-phase ejecta |
we present spectroscopic observations of the supernova remnant snr 0509-67.5 in the large magellanic cloud. we used the integral field-unit muse on the very large telescope to spectrally and spatially resolve the fast balmer shocks around the remnant. we show some preliminary results of the resolved broad h$\alpha$-lin... | using balmer lines to unveil the presence of cosmic rays in the supernova remnant snr 0509-67.5 |
class i methanol masers (cimms) and 1720 mhz oh masers are believed to arise from a common collisional pumping mechanism, and both trace shocked gas regions in supernova remnants (snrs). however, their coexistence in star formation regions (sfrs) and their association with a front of bipolar outflow (a source of shock-... | search for collisionally pumped 1720 mhz oh masers in star-forming regions: a vla survey of 18 cm oh masers toward 80 class i methanol masers |
we present an analysis of x-ray observations made with asca and xmm-newton of the galactic supernova remnant (snr) g311.5-0.3. prior infrared and radio observations of this snr have revealed a shell-like morphology at both wavelengths. the spectral index of the radio emission is consistent with synchrotron emission, wh... | asca and xmm-newton observations of the galactic supernova remnant g311.5-0.3 |
supernova remnants (snrs) can radiate their energy across the whole electromagnetic spectrum, but they are principally radio emitters, and investigations in the radio range have provided deep insight into the properties, the evolutionary characteristics, and the physical processes at play. radio observations permit to ... | radio emission from supernova remnants |
a mixed hydrogen and helium (h + he) spectrum with a clear steepening at ∼ 700 tev has been detected by the argo-ybj experiments. in this paper, we demonstrate that the observed h + he spectrum can be reproduced well with a model of cosmic rays escaping from the supernova remnants (snrs) in our galaxy. in this model, p... | a possible explanation of the knee of cosmic light component spectrum from 100 tev to 3 pev |
the light emission ("glow") of cold dusty plasma of the remnant of sn 1987a was confirmed by the hubble space telescope observations on 7th january, 1995. in particular, ca i and ca ii lines were recorded and identified in the spectrum of the supernova's envelope. the period of complete hydrogen recombination in the re... | ionisation loss and shock excitation of 4420ca i and 4420ca ii atoms in cold remnants of type ii supernovae |
we present multi-epoch ks band imaging of the supernova remnant cassiopeia a (cas a). the morphology of the emission in this band is generally diffuse and filamentary, consistent with synchrotron radiation observed at radio wavelengths. however, in one region to the southwest of the remnant, compact knots of emission a... | variability in the near-infrared synchrotron emission from cassiopeia a |
we present subarcsecond optical images and low- to moderate-resolution spectra of the compact, x-ray, and optically bright supernova remnant known as s8 in the nearby dwarf galaxy ic 1613. deep hα images of the remnant show a sharply defined crescent-shaped nebula, while narrow passband images reveal a coincident and u... | the nature of the young supernova remnant s8 in the dwarf galaxy ic 1613 |
aims: we investigate thermal and nonthermal radio emission associated with the early formation and evolution phases of young stellar clusters (yscs) selected by their mid-infrared (mir) emission at 24 μm in m 33. we consider regions in their early formation period, which are compact and totally embedded in the molecula... | radio emission during the formation of stellar clusters in m 33 |
ngc 6946, known as the fireworks galaxy because of its high supernova rate and high star formation, is embedded in a very extended h i halo. its northern spiral arm is well detached from the galactic main body. we found that this arm contains a large (∼300 pc in size) red ellipse, named according to a strong contaminat... | imaging and spectroscopic observations of a strange elliptical bubble in the northern arm of the spiral galaxy ngc 6946 |
aims: in a previous paper we investigated the molecular environment toward the eastern border of the supernova remnant (snr) g18.8+0.3. continuing with the study of the surroundings of this snr, we now focus on its southern border, which in the radio continuum emission shows a very peculiar morphology with a corrugated... | the southern molecular environment of snr g18.8+0.3 |
cassiopeia a, the brightest radio supernova remnant (snr) in the sky, has several unique characteristics in comparison to its peers. besides its radio brightness and prominent soft-concave radio spectrum, its γ-ray spectrum appears to have a low-energy cutoff near 2 gev, and it is the only snr with prominent hard x-ray... | mhd simulations of inward shocks in cassiopeia a |
in this paper we determine the shock velocities in the cygnus loop supernova remnant, using proper motions of the filaments in the remnant. the proper motions were measured by comparing the hα images of the remnant observed in two epochs: in 1993 (obtained at kitt peak national observatory), and in 2018 (obtained at na... | proper motion of cygnus loop filaments |
using ground-based and hst images taken in the optical and nir of the cassiopeia a supernova remnant covering the time period 1951 to 2019, together with moderate dispersion optical spectra of selected filaments, we present an investigation of the remnant's reverse shock velocity and the dynamical effects it has on the... | the velocity and dynamical effects of cas a's reverse shock |
η carinae is composed of two very massive stars orbiting each other in 5.5 years. the primary star features the densest known stellar wind, colliding with that expelled by its companion. the wind collision region dissipates energy and accelerates particles up to relativistic energies, producing nonthermal x‑ray and γ‑r... | η carinae: particle acceleration and multimessenger aspects |
we study the large scale interaction of the supernova remnants with clouds of interstellar gas. optical proper motion measurements and hα emission in supernova remnants are discussed, especially for the 1.4 m telescope ``milanković'' and astroclimate conditions at the astronomical station vidojevica near prokuplje, ser... | hydrodynamics of supernova remnants: interaction with interstellar medium |
we present the 2d axisymmetric model of particle acceleration at colliding shocks from supernova remnant and stellar wind from the nearby star. the model is the expansion of the previously developed plane-parallel model and takes into account three three-dimensional structure of the stellar wind and the supernova remna... | 2d axisymmetric model of particle acceleration in colliding shock flows system |
new evidence that galactic cosmic rays (gcr: here protons and nuclei) are accelerated by supernova remnant (snr) shocks has come from recent works combining γ-ray observations in the sub-gev to tev domain, and in the submm-mm domain. the results show an enhanced cr flux in regions of massive star formation in which snr... | observations of supernova remnants and molecular clouds: bridging low and high energy cosmic rays |
the mechanism of interstellar dust formation is a matter of continuing debate. in the very early universe, some high redshift galaxies are observed to have a substantial amount of dust. this has led to the suggestion that core collapse supernovae must be the producers of much of the dust in the universe. however, most ... | newly formed dust in the core-collapse supernova remnant e0102 |
it is shown that high-energy astrophysical neutrinos observed in the icecube experiment can be produced by protons accelerated in extragalactic type iin supernova remnants by shocks propagating in the dense circumstellar medium. the nonlinear diffusive shock acceleration model is used for description of particle accele... | type iin supernovae as sources of high energy neutrinos |
core-collapse supernovae have been monitored with vlbi from shortly after the explosion to many years thereafter. radio emission is produced as the ejecta hit the stellar wind left over from the dyingstar. images show the details of the interaction as the shock front expands into the circumstellar medium. measurements ... | supernova research with vlbi |
the supernova remnant 0519-69.0 is the second youngest ia remnant in the large magellanic cloud. the typing of the remnant rests primarily on ejecta abundances inferred from x-ray spectra and the balmer-dominated nature of its forward shock. using two narrow-band hα imaging with the hubble space telescope separated by ... | a direct measurement of the forward shock speed in supernova remnant ``0519-69.0'': constraints on the age, ambient density and electron-ion temperature equilibration |
interstellar medium clouds in the w28 region are emitting gamma-rays and it is likely that the w28 supernova remnant is responsible, making w28 a prime candidate for the study of cosmic-ray acceleration and diffusion. understanding the influence of both supernova remnant shocks and cosmic rays on local molecular clouds... | molecular shocks and the gamma-ray clouds of the w28 supernova remnant |
we present multi-epoch, high-resolution (r~230,000), high s/n observations of the interstellar na i absorption toward a sample of 20 stars taken over the past 10 years with the kpno coude feed telescope. these spectra reveal line profile variations (since 2004) in 12 of the 20 stars indicative of na i structure on scal... | a survey of au-scale na i structure in the diffuse ism |
recent gamma-ray observations show that middle aged supernova remnants (snrs) interacting with molecular clouds (mcs) can be sources of both gev and tev emission. based on the mc association, two scenarios have been proposed to explain the observed gamma-ray emission. in one, energetic cosmic ray (cr) particles escape ... | time dependent diffusive shock acceleration and its application to middle aged supernova remnants |
snrpy (super nova remnant python) models supernova remnant (snr) evolution and is useful for understanding snr evolution and to model observations of snr for obtaining good estimates of snr properties. it includes all phases for the standard path of evolution for spherically symmetric snrs and includes alternate evolut... | snrpy: supernova remnant evolution modeling |
thirty years on, sn 1987a continues to develop and, over the last decade in particular, has: revealed the presence of a large centrally concentrated reservoir of dust; shown the presence of molecular species within the ejecta; expanded such that the ejecta structure is angularly resolved; begun the destruction of the c... | supernova 1987a at 30 |
using a specialized technique sensitive to the presence of expanding ionized gas, we have detected a set of three concentric expanding shells in an h ii region in the nearby spiral galaxy m33. after mapping the kinematics in hα with fabry-perot spectroscopy, we used slit spectra to measure the intensities of the [s ii]... | three supernova shells around a young m33 star cluster |
the supernova remnant (snr) 3c434.1 has been extensively studied in the radio band, yet the only x-ray observation of the source dated back to rosat era until recently. only extended thermal emission from shocked material was detected as a consequence. our recent observation of the region with xmm revealed, however, a ... | uncovering the origin of the non-thermal x-ray and the gev emission from the snr 3c434.1 (g94.0+1.0) |
high-resolution chandra x-ray observations of tycho’s supernova remnant (snr 1572) have revealed several series of bright, nearly parallel stripes in some regions of the snr clearly seen in 4-6 kev band images. the observed radiation of tycho’s snr is most likely the synchrotron radiation of electrons with energies wel... | modeling of x-ray images of tycho’s supernova remnant |
the large majority of searches for supernova remnants in nearby galaxies have focused on strong [s ii] emission relative to h-alpha, a key indicator of the shock-heated emission. however, of the 1200 supernova remnants (snrs) detected in this way, only two young core-collapse snrs were found with ages between 50-100 ye... | survey of young supernova remnants in nearby galaxies |
thanks to its large size, its location well out of the galactic plane, and its high brightness, the middle-age snr cygnus loop is well suited for observations across the entire electromagnetic spectrum. in the radio band, this snr presents a very characteristic morphology with a large northern circular shell and a bubb... | new high-frequency radio observations of the cygnus loop supernova remnant |
we report on reshocked rayleigh-taylor instability (rti) experiments fielded on the orion laser. these experiments build from a platform qualified on the luli2000 facility which allowed to perform high energy density (hed) experiments in scaled conditions for supernovae remnants evolution. a low density foam is used to... | reshocked rayleigh-taylor instabilities experiments on orion |
supernova remnants provide crucial information on the physics of the underlying explosions, the nature of any associated relic compact objects, and the injection metal-enriched material and energetic particles into the host galaxy. because of the high temperatures produced by fast shocks in snrs, x-ray observations pro... | xmm-newton observations of supernova remnants |
we propose a deep (800 ks) chandra legacy observation of n132d, the brightest supernova remnant in the local group. it will permit an unprecedented look at the spatial distribution of iron and other heavy elements in the ejecta from this prototypical core-collapse supernova (impossible with other current x-ray missions... | a legacy observation of n132d, the most luminous snr in the local group |
collisionless shocks are ubiquitous in astrophysical plasmas and are known to be important in magnetic field amplification and in the acceleration of both high-energy electrons and protons (cosmic rays). while the theory of diffusive shock acceleration (dsa) is well established, the details of particle injection into d... | simulations of particle acceleration in collisionless shocks for conditions relevant to nif experiments |
wide-field hα images of the radio faint galactic supernova remnant g182.4+4.2 reveal a surprisingly extensive and complex optical emission structure with an unusual series of broad and diffuse filaments along the remnant's southwestern limb. deep [o iii] images reveal no appreciable remnant emission with the exception ... | discovery of extensive optical emission from the extremely radio faint galactic supernova remnant g182.4+4.3 |
we perform long-term, hydrodynamical simulations of supernova remnants in 3 dimensions. continuing the simulations of a.wongwathanarat "3d long-time ccsn simulations: from shock revival to shock break-out" we follow the evolution of the shock and the ejecta during the first few months after the explosion. the explosion... | the first few months of a supernova remnant |
i will outline the updated demographics on multi-wavelength surveys of extragalactic supernova remnant (snr) populations in order to probe their properties (e.g. line ratios, luminosities, densities, temperatures) and their connection. with these studies we are allowed to cover a wider range of environments and interst... | snr populations in our galaxy and beyond: bridging the gap |
core-collapse supernova remnants (cc-snrs) show strong anisotropies inthe ejecta that can trace pristine structures in the explosion.vela snrshows ejecta shrapnel beyond the main shock shell. we have shown thattwo of them (a,g), located in opposite directions of the snr center,aresi-rich,while all the other shrapnel sh... | dynamics and energetics of the jet-like structure in the vela snr |
radiative shocks are relevant to a variety of astrophysical phenomena, such as supernova remnants and accretion shocks. experiments to understand the structure and radiation transport in radiative shocks inform the interpretation of observational data and improve simulation codes. a recent discovery science campaign me... | radiative shock properties using x-ray thomson scattering and self-emission measurements on the national ignition facility |
near the center of the oxygen-rich supernova remnant puppis a, a highly unusual structure exists consisting of multiple irregular rings of metal-rich material propagating at high radial velocities, was detected 30 years ago. these structures have thus far only been detected at visible wavelengths, and appear to be asso... | rings of metal-rich ejecta in puppis a: hints of a supernova interaction in a binary? |
that snrs accelerate particles to cr energies is no longer in doubt, but there are many questions yet to be answered. we still lack detailed knowledge about the efficiency of the process of particle acceleration at snr shocks, the effect of cr production on the evolution of snrs, and the properties of magnetic fields i... | a hard (x-ray) look at the sw region of snr rcw 86 |
magnetic field amplification by streaming instabilities is central to many astrophysical scenarios, from supernova remnant shocks to gamma-ray bursts. it can also be important in advanced laboratory concepts for inertial fusion and compact radiation sources. the weibel, or current filamentation, instability is often th... | magnetic field amplification by a nonlinear electron streaming instability |
non-thermal particles are common in the universe and are observed in solar winds, supernova remnants, gamma ray bursts, and elsewhere. one of the methods used to explain how the particles are accelerated is the second order fermi mechanism. while less efficient than diffusive shock acceleration, the ubiquitous nature o... | flash simulations that model laser-driven plasma experiments aiming to study second order fermi acceleration at the gsi helmholtz centre for heavy ion research |
two outstanding questions about the physics of interstellar shock waves are 1) the degree of thermal equilibration among electrons and different ions and 2) efficiency of transfer of energy from the thermal plasma to energetic particles---cosmic rays. those questions are closely related in that both processes depend up... | thermal equilibration and cosmic-ray acceleration in astrophysical shocks: uv spectra of the sn1006 remnant |
in this talk, a three-dimensional core-collapse supernova simulation of a progenitor star that has its hydrogen envelope stripped is discussed. the explosion is triggered by means of a parametric neutrino engine. large-scale explosion asymmetries seeded by small-scale random perturbations develop during the stalled sho... | a three-dimensional core-collapse supernova model resembling cassiopeia a |
we present measurements of the expansion of kepler's supernova remnant (snr) over three epochs of chandra x-ray observations from 2000, 2006, and 2014. kepler's snr provides an important opportunity for studying the expansion rate of the forward shock front of a type ia supernova. as the remnant of a historical superno... | a 14-year proper motion study of the forward shock of kepler's supernova remnant |
in the x-ray emission of supernovae remnants, the shocked interstellar medium, the shocked ejecta and the synchrotron possess a different spatial and spectral signature, but are closely entangled. extracting the intrinsic spatial and spectral information of the individual components from this data is a challenging task... | revisiting the ejecta asymmetries in casa with a novel method for component separation in x-rays |
the ejecta in supernova remnants is the most direct link to information about the progenitor system of the pre-supernova star. the abundances of various elements, the spatial velocity of the ejecta blobs, the temperature of the reverse-shocked plasma; all of these are important diagnostics from the ejecta. in this talk... | what we can learn from ejecta in supernova remnants |
we present an update on the design and projected capabilities of the supernova remnants and proxies for re-ionization testbed experiment (sprite). sprite is a 6u cubesat designed to survey ionizing radiation emission from low-redshift star-forming galaxies, and to map far-uv (100 - 175 nm) emission from shock fronts in... | probing the structure and ionizing spectrum of galaxies with the sprite cubesat |
one aim of supernova remnant (snr) evolution models is to deduce fundamental properties of a supernova (sn) explosion from the current state of its snr. the snr hot plasma is characterized by its observed x-ray spectrum: electron temperature, emission measure and abundances. this plasma is heated by the snr forward sho... | population analysis of supernova remnants in the galaxy using evolutionary models |
it has now been well established the core collapse supernovae (sn) create significant quantities of dust. the dust is formed in cold, dense ejecta clumps and has been observed in several young supernova remnants such as cas a. much of the dust detected in supernova remnants, however has not yet encountered the reverse ... | simulating the evolution of supernova created dust: decoupling, destruction and escape |
collisionless shocks are ubiquitous in astrophysical plasmas and are known to be important in magnetic field amplification and in the acceleration of both high-energy electrons and protons (cosmic rays). while the theory of diffusive shock acceleration (dsa) is well established, the details of particle injection into d... | simulations of electron injection in collisionless shocks for conditions relevant to nif experiments |
we present a model for the seeding and evolution of magnetic fields in protogalaxies. supernova sn explosions during the assembly of a protogalaxy provide magnetic seed fields, which are subsequently amplified by compression, shear flows and random motions. our model explains the origin of strong magnetic fields of mic... | a supernova scenario for magnetic fields and rotation measures in galaxies |
the nature and physical environments of snrs are diverse, and for this reason, the understanding of the properties of nearby snrs is useful in interpreting the emission from snrs in remote galaxies where we cannot resolve them. in this regard, the lmc is a unique place to study snrs due to its proximity, location, and ... | a multi-wavelength study of n63a: a supernova remnant within an h ii region in the large magellanic cloud |
we investigate spherical collisionless shocks in the presence of an external magnetic field. spherical collisionless shocks are common resultant of interactions between a expanding plasma and a surrounding plasma, such as the solar wind, stellar winds, and supernova remnants. anisotropies often observed in shock propag... | spherical shock in the presence of an external magnetic field |
nustar observations of 44ti have demonstrated the power radioactive nuclei have in constraining aspects of the supernova engine. radioactive nuclei have the potential to probe core-collapse remnants (and neutron star mergers) over a range of ages. radioactive decays produce photons both in the gamma-rays and, through d... | radioactive isotopes in core-collapse remnants |
based on our deep chandra data we present the initial results from our detailed study of the shocked ejecta and circumstellar medium in the textbook-type galactic core-collapse supernova remnant g292.0+1.8. we utilize an adaptive-mesh technique to construct spatial distribution maps of individual ejecta elements (o, ne... | x-ray ejecta and csm distributions in the galactic core-collapse snr g292.0+1.8 |
high-mach-number collisionless shocks are found in planetary systems as well as supernova remnants. these shocks are often associated with strong magnetic fields and it is still not well understood how magnetic fields are amplified at scales of the shock thickness. here we use a set of large-scale particle-in-cell (pic... | magnetic field amplification by weibel instability at planetary high mach-number shocks |
recent nif experiments focus on the generation and diagnosis of collisionless shocks relevant to astrophysical phenomena such as supernova remnants and gamma ray bursts. in the experiments, two opposing cd laser-generated plasmas flow into each other at high velocity ( 1000 km/s). as the ion-ion collisional mean-free-p... | collisionless and kinetic phenomena of interpenetrating plasma streams via neutron self-emission |
astrophysical environments such as supernova remnants and galaxy clusters host nonrelativistic collisionless shocks which can accelerate and heat protons and electrons. these shocks are capable of equilibrating the temperature between the particle species. we use two-dimensional particle-in-cell simulations in order to... | energy partition between ions and electrons in high mach number nonrelativistic collisionless shocks |
some 10-20 kyr ago a pulsar was born from a core collapse event, receiving right away a strong kick. nowadays this pulsar is powering the lighthouse nebula (igr j11014-6103): a complex system of outflows comprising the bow-shock pwn, and two well collimated jets extending perpendicularly to the pulsar's direction of mo... | the lighthouse nebula: a run-away pulsar, its pwn, jets and parent snr |
supernova remnant (snr) n132d, located in the large magellanic cloud, represents a unique opportunity for the study of γ-ray emission from shock accelerated cosmic rays (crs) in another galaxy since it stands as the first and only extra-galactic snr detected in γ-rays. n132d is bright in the x-ray, infrared and radio b... | the monster next door: fermi-lat observations of supernova remnant n132d in the large magellanic cloud |
remnants of type-ia supernovae (ia snrs) are important sources of high energy emission, and contribute significantly of the to the chemical evolution of galaxies. they carry the imprints of their parent explosion, allowing us to clue in on the type-ia progenitor system and explosion channel, which remain some of major ... | constraints on type ia supernova remnants from emission properties and kinematics |
supernovae are known creators of dust in their dense cold ejecta. however it is still uncertain how much of that dust survives and is injected into the interstellar medium. i will present the results of new hydrodynamical simulations using the flash code in which we model the evolution of the clumpy ejecta in the cas a... | survival of dust created in cas a supernova remnant |
we present the first three-dimensional measurements of the velocity of various ejecta knots in tycho's supernova remnant, the remains of sn 1572, known to be a type ia explosion. when the ejecta knots pass through the reverse shock, they become heated to x-ray emitting temperatures, and chandra's unmatched spatial reso... | the three-dimensional motions of the ejecta of tycho's supernova remnant |
new evidence that cosmic rays (hadronic component) are accelerated by supernova remnant shocks all the way from low energies to high energies, has come from recent works combining gamma-ray observations in the sub-gev to tev domain on the one hand, and in the submm-mm domain on the other hand. these observations concer... | observations of supernova remnants and molecular clouds from the mm to the gamma-ray domain: bridging low and high energy cosmic rays |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.