Imprinting knots in a spinor Bose-Einstein condensate via a Raman process without knotted optical fields
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Zekai Chen↗
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Characterization of the Inner Knot of the Crab: the Site of the Gamma-ray Flares?
One of the most intriguing recent discoveries has been the detection of powerful gamma-ray flares from the Crab Nebula. Such events, with a recurrence time of about once per year, can be so dramatic to make the system the brightest source in the gamma‐ray sky as occurred, e.g. in April 2011. These flares challenge our understanding of how pulsar wind nebulae work and defy current astrophysical models for particle acceleration. We present here our study of the inner knot located within a fraction of an arcsecond from the pulsar with the aim of characterizing the feature and asking if this might be the site of the origin of the gamma-ray flares. We took data using Keck, HST, and Chandra obtained as part of our multi‐wavelength campaign to identify the source of the enigmatic flares. We set an upper limit as to the gamma-ray flux from the knot. We also find that the dimensions, surface brightness, flux, etc. of the optical and infrared knot are all correlated with distance from the pulsar. This distance, in turn, varies with time. In addition to this most thorough characterization of the inner knot's properties, we examine the hypothesis that the knot may be the site of the flares by examining the knot separation versus the Fermi/LAT gamma-ray flux. Finally, as part of this research, we make use of a new approach employing singular value decomposition (SVD) for analyzing time series of images and compare the approach to more traditional methods. Our conclusions are only refined but not impacted by using the new approach.
Gamma-ray Flares↗
RGS Observations of Ejecta Knots in Tycho's Supernova Remnant
We present results from XMM-Newton/RGS observations of prominent knots in the southest portion of Tycho's supernova remnant, known to be the remnant of a Type Ia SN in 1572 C.E. By dispersing the photons from these knots out of the remnant with very little emission in front of or behind them, we obtained the nearly uncontaminated spectra of the knots. In the southernmost knot, the RGS successfully resolved numerous emission lines from Si, Ne, O He-alpha and Ly-alpha, and Fe L-shell. This is the first clear detection of O lines in Tycho's SNR. Line broadening was measured to be ~ 3 eV for the O He-alpha and ~ 4:5 eV for Fe L lines. If we attribute the broadening to pure thermal Doppler effects, then we obtain kTO and kTFe to be ~ 400 keV and 1.5 MeV, respectively. These temperatures can be explained by heating in a reverse shock with a shock velocity of ~ 3500 km/s. The abundances obtained from fitting the RGS and MOS data together imply substantially elevated amounts of these materials, confi rming previous studies that the knots are heated by a reverse shock, and thus contain ejecta material from the supernova. We are unable to fi nd a Type Ia explosion model that reproduces these abundances, but this is likely the result of this knot being too small to extrapolate to the entire remnant.
Brian J. Williams↗
Velocity dispersions of knots in Vela X and Puppis A
Very high resolution spectroscopy of optical emission lines indicates that the velocity dispersions of knots in Vela X and Puppis A result primarily from turbulence within the emitting regions. Line-of-sight velocity dispersions (half-widths at half-maximum) for the observed knots in both remnants are about 20-30 km/s. In Vela X, these include thermal velocity dispersions of roughly 16 km/s for hydrogen and 4 km/s for nitrogen. The knots themselves move randomly relative to each other, with speeds up to 30 km/s in Vela X and between 30-80 km/s in Puppis A. Occasionally, diffuse components of the filaments are observed in Puppis A. These diffuse components have velocity dispersions between 55 and 80 km/s, but the relative contributions of turbulent and thermal motions to the dispersions are unknown. The results are compared with theory and previous observations. Direct photographs may be able to show if the forbidden O III knots are less spatially dispersed than the forbidden N II, forbidden S II, forbidden O II, and H I knots.
Shull, P., Jr.↗
The mutual attraction of magnetic knots
It is observed that the magnetic knots associated with active regions on the sun have an attraction for each other during the formative period of the active regions, when new magnetic flux is coming to the surface. The attraction disappears when new flux ceases to rise through the surface. Then the magnetic spots and knots tend to come apart, leading to disintegration of the sunspots previously formed. The dissolution of the fields is to be expected, as a consequence of the magnetic repulsion of knots of like polarity and as a consequence of the hydromagnetic exchange instability. The purpose of this paper is to show that the mutual attraction of knots during the formative stages of a sunspot region may be understood as the mutual hydrodynamic attraction of the rising flux tubes. Two rising tubes attract each other, as a consequence of the wake of the leading tube when one is moving behind the other, and as a consequence of the Bernoulli effect when rising side by side.
Parker, E. N.↗
IUE observations of NGC 1068 - The extremely luminous starburst knots
A complete investigation of the UV characteristics of the starburst knots in the inner 3 kpc region of NGC 1068 mapped by the IUE is presented. It is noted that these knots probably represent the most luminous H II regions yet studied at optical and UV wavelengths. Comparisons suggest that the brightest knot, knot 1, is 30 times brighter than NGC 604 in M33 and has a total luminosity of not less than 10 to the 43rd ergs/s.
Bruhweiler, F. C.↗
Chandra X-ray Observation of a Mature Cloud-Shock Interaction in the Bright Eastern Knot of Puppis A
We present Chandra X-ray images and spectra of the most prominent cloud-shock interaction region in the Puppis A supernova remnant. The Bright Eastern Knot (BEK) has two main morphological components: (1) a bright compact knot that lies directly behind the apex of an indentation in the eastern X-ray boundary and (2) lying 1 westward behind the shock, a curved vertical structure (bar) that is separated from a smaller bright cloud (cap) by faint diffuse emission. Based on hardness images and spectra, we identify the bar and cap as a single shocked interstellar cloud. Its morphology strongly resembles the "voided sphere" structures seen at late times in Klein et al. experimental simulat.ions of cloud-shock interactions, when the crushing of the cloud by shear instabilities is well underway. We infer an intera.ction time of roughly cloud-crushing timescales, which translates to 2000-4000 years, based on the X-ray temperature, physical size, and estimated expansion of the shocked cloud. This is the first X-ray identified example of a cloud-shock interaction in this advanced phase. Closer t o the shock front, the X-ray emission of the compact knot in the eastern part of the BEK region implies a recent interaction with relatively denser gas, some of which lies in front of the remnant. The complex spatial relationship of the X-ray emission of the compact knot to optical [O III] emission suggests that there are multiple cloud interactions occurring along the line of sight.
Hwang, Una↗
Some properties of the knots in the M87 jet
Photographs taken in 1956 by Baade show the knots in the jet of M87 to be polarized. In 1978, these plates were repeated under conditions as identical as possible. A careful comparison indicates that the polarization and intensity of the knots have changed in the 22 year interval. Emission lines in the nucleus of M87 not previously seen have been revealed by extensive 5 m SIT spectroscopy. The same spectroscopy with galaxy subtracted, however, has failed to reveal any features in the jet. The known optical and radio properties of the jet are reviewed. A coincidence is found in almost all of the defining properties of BL Lacertae objects with the properties of the knots in the jet. Statistical studies of the distribution of BL Lacertae objects near bright galaxies reveals a marginally significant excess of such associations.
Sulentic, J. W.↗
The chemical abundances of the Cassiopeia A fast-moving knots - Explosive nucleosynthesis on a minicomputer
A simplified nuclear reaction network for explosive nucleosynthesis calculations is described in which only the most abundant nuclear species and the most important reactions linking these species are considered. This scheme permits the exploration of many cases without excessive computational effort. Good agreement with previous calculations employing more complex reaction networks is obtained. This scheme is applied to the observed chemical abundances of the fast-moving knots in the supernova remnant Cassiopeia A and it is found that a wide range of initial conditions could yield the observed abundances. The abundances of four of the knots with significant and different amounts of elements heavier than oxygen are consistent with an origin in material of the same initial composition but processed at different peak temperatures and densities. Despite the observed high oxygen abundances and low abundances of light elements in the knots, they did not necessarily undergo incomplete oxygen burning; in fact, it is not even necessary that oxygen have been present in the initial composition. The agreement between the calculated and observed chemical abundances in Cas A and similar supernova remnants depends primarily upon the relevant nuclear physics and does not provide strong evidence in favor of any particular model of the supernova event.
Johnston, M. D.↗
Velocity dispersions of knots in the Cygnus Loop and IC 443
Very high resolution spectroscopy of optical emission lines indicates that the velocity dispersions of knots in Cygnus Loop and IC 443 filaments result primarily from turbulence within the emitting regions. Line-of-sight velocity dispersions (half-widths at half-maximum) for the observed knots are on the order of 10-30 km/s, including associated thermal velocity dispersions of roughly 15 km/s for hydrogen, 6 km/s for oxygen, and 4 km/s for nitrogen. The knots themselves move randomly relative to each other with speeds of 10-30 km/s. Occasionally, diffuse components of the filaments are observed. These diffuse components have velocity dispersions between 60 and 85 km/s, but the relative contributions of turbulent and thermal motion to the dispersions are unkown.
Shull, P., Jr.↗
Resolution of compact knots in Cassiopeia A
Observations of the young supernova remnant Cassiopeia A at a wavelength of 2 cm have resolved small knots. The flux density of these knots decays on a 1/e time scale of about 14 yr. This is faster than the decay of the smooth features. The pressure in these knots can be estimated at 4 x 10 to the 7th dynes/sq cm. This is somewhat greater than the pressure within the smooth component of the supernova remnant.
Arendt, Richard G.↗
Extraordinary line-emitting knots in the Crab Nebula
Extraordinary, semistellar, line-emitting knots are apparent in images of the Crab Nebula which were obtained with the Goddard Fabry-Perot imager at the Michigan-Dartmouth-MIT Observatory. The knots are most prominent for (O III) lambda 5007 emission through a 5.3 A (Full Width at Half Maximum (FWHM)) bandpass centered at 5015.3 A, with representative fluxes of roughly 10(exp -14) ergs/sq cm. They are aligned in arcs, seven to the north and four to the south, from the pulsar. The northern group appears to be in a bounded corridor through the filamentary structure. Measurements over a 2 year baseline yield proper motions of order 0.1 sec/yr, corresponding to transverse velocities of order 900 km/s for a distance of 1830 pc. The knots are characterized by remarkably strong (Ar III) emission, possibly indicating high argon abundances, high gas temperatures, or anomalous physical processes.
Macalpine, Gordon M.↗
The Origin of the Iron-Rich Knot in Tycho's Supernova Remnant
X-ray observations of supernova remnants (SNRs) allow us to investigate the chemical inhomogeneity of ejecta, offering unique insight into the nucleosynthesis in supernova explosions. Here we present detailed imaging and spectroscopic studies of the Fe knot located along the eastern rim of the Type Ia SNR Tycho ( SN 1572) using Suzaku and Chandra long-exposure data. Surprisingly, the Suzaku spectrum of this knot shows no emission from Cr, Mn, or Ni, which is unusual for the Fe-rich regions in this SNR. Within the framework of the canonical delayed-detonation models for SN Ia, the observed mass ratios M(sub Cr)/M(sub Fe) is less than 0.023, M(sub Mn)/M(sub Fe) is less than 0.012, and M(sub Ni)/M(sub Fe) is less than 0.029 (at 90% confidence) can only be achieved for a peak temperature of (5.3 - 5.7) x 10(exp. 9) K and a neutron excess of approximately less than 2.0 x 10(exp. -3). These constraints rule out the deep, dense core of a Chandrasekhar-mass white dwarf as the origin of the Fe knot and favor either incomplete Si burning or an Alpha-rich freeze-out regime, probably close to the boundary. An explosive He burning regime is a possible alternative, although this hypothesis is in conflict with the main properties of this SNR.
ISM supernova remnants↗
Design considerations for attaining 250-knot test velocities at the aircraft landing dynamics facility
Preliminary design studies are presented which consider the important parameters in providing 250 knot test velocities at the Aircraft Landing Dynamics Facility. Four major components of this facility are: the hydraulic jet catapult, the test carriage structure, the reaction turning bucket, and the wheels. Using the hydraulic-jet catapult characteristics, a target design point was selected and a carriage structure was sized to meet the required strength requirements. The preliminary design results indicate that to attain 250 knot test velocities for a given hydraulic jet catapult system, a carriage mass of 25,424 kg (56,000 lbm.) cannot be exceeded.
Gray, C. E., Jr.↗
Spontaneous formation of knots in relativistic flows - A model for variability in compact synchrotron sources
A model is proposed in which regions of enhanced synchrotron emission are formed via radiative thermal instabilities in relativistic flows. A perturbed volume in which the magnetic field is enhanced by a few tens of a percent relative to the steady value collapses due to the increased cooling rate and consequent loss in pressure. The collapse further increases the magnetic field, leading to even shorter radiative lifetimes. The instability progresses in this way until either the external electron pressure is balanced by the perturbed magnetic pressure or the overall expansion of the flow becomes important. A fluid-dynamical treatment of the instability is performed, and the results are shown to apply to flux variations and formation of knots in the relativistic flows which are thought to occur in quasars and active galactic nuclei. The knots possess the same kinematic properties as the collimated flow and can thus be responsible for the apparent superluminal motions observed in compact radio sources.
Marscher, A. P.↗
Observations of infrared emission from a fast-moving knot in Cassiopeia A
Broadband (10 microns) and spectroscopic (8.99, 10.52 and 12.81 microns) scans were made of the metal-rich knots in Cas A using instrumentation at the NASA IR Telescope Facility. The observations were performed to distinguish between thermal continuum emission and other features of the metal-rich knots. A faint, forbidden Si IV line was detected, and upper limits were set on the forbidden Ar III and forbidden Ne II emissions, which are now expected to be completely due to lines that may be accessible to the 12 microns sensor on the IRAS. The implications of the measurements for the interpretation of broadband data on metal-rich remnants are discussed.
Dinerstein, Harriet L.↗
Structure and dynamics of the plasma tail of comet P/Halley. I - Knot event on December 31, 1985
On the basis of about 500 photographs of comet Halley taken by many observers, Saito et al. (1986) classified the detected disturbances of the plasma tail as outstanding rays, streamer, helix, kink, arcade, and disconnection event (DE). In this paper, the interaction of the solar wind with the plasma tail of Comet P/Halley is examined by using results of observations by the Sakigake spacecraft of the December 31, 1985 event, which included various disturbances and one DE-like knot. On the basis of twenty photographs taken on December 31 by Japanese astronomers, the dynamic pressure model proposed by Saito et al. (1986) is examined, and the mechnism of the knot event that appeared in the plasma tail of the comet on December 31, is explained.
Saito, T.↗
First results from the Goddard High-Resolution Spectrograph - Ultraviolet spectra of a starburst knot in NGC 1068
This paper presents UV spectroscopy of a circumnuclear starburst knot in the Seyfert 2 galaxy NGC 1068, a close-by active galaxy which has some of the most luminous known starburst knots. The spectrum shows the presence of several thousand O and B stars which appear to have formed about 3 million years ago.
Hutchings, J. B.↗