scholarly journals Chandra Studies of Supernova Remnants and Pulsars

2001 ◽  
Vol 205 ◽  
pp. 358-365
Author(s):  
Patrick Slane ◽  
John P. Hughes ◽  
Cara E. Rakowski ◽  
David N. Burrows ◽  
John A. Nousek ◽  
...  
Keyword(s):  
Time Resolution ◽  
Supernova Remnants ◽  
Angular Resolution ◽  
Fast Time ◽  
X Ray ◽  
Spatially Resolved ◽  
Unique Capability

With sub-arcsecond angular resolution accompanied by fast time resolution and spatially resolved spectral capabilities, the Chandra X-ray Observatory provides a unique capability for the study of supernova remnants (SNRs) and pulsars. Though in its relative infancy, Chandra has already returned stunning images of SNRs which reveal the distribution of ejecta synthesized in the stellar explosions, the distinct properties of the forward and reverse shocks, and the presence of faint shells surrounding compact remnants. Pulsar observations have uncovered jet features as well as small-scaled structures in synchrotron nebulae. In this brief review we discuss results from early Chandra studies of pulsars and SNRs.

General Structure of the X-ray Corona

1994 ◽  
Vol 144 ◽  
pp. 69-76
Author(s):  
L. W. Acton
Keyword(s):  
Time Scales ◽  
Time Resolution ◽  
Angular Resolution ◽  
General Structure ◽  
Coronal Holes ◽  
Active Regions ◽  
X Ray ◽  
Structure Changes

AbstractX-ray images have revealed the corona to comprise four basic morphologies. In order of X-ray luminosity these structures are: (1) Bright, relatively short, X-ray loops in active regions, (2) Less bright and larger X-ray structures of the so-called quiet corona, (3) X-ray bright points, and (4) Coronal holes. The soft X-ray telescope (SXT) onYohkohprovides good angular resolution with much improved time resolution and continuity of coverage as compared to the earlier observations. In the SXT movies these structures often appear to be interacting and change appearance on time scales from seconds to weeks. Flare, flare-like, and eruptive processes continuously alter the general structure of the corona. This paper will comment on the structure, changes and heating of the X-ray corona as revealed by theYohkohobservations.

scholarly journals Probing the effects of hadronic acceleration at the SN 1006 shock front

2013 ◽  
Vol 9 (S296) ◽  
pp. 315-319
Author(s):  
Marco Miceli ◽  
F. Bocchino ◽  
A. Decourchelle ◽  
G. Maurin ◽  
J. Vink ◽  
...  
Keyword(s):  
Particle Acceleration ◽  
Spectral Analysis ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Cosmic Ray ◽  
X Ray ◽  
Spatially Resolved ◽  
Large Program ◽  
Post Shock

AbstractSupernova remnant shocks are strong candidates for being the source of energetic cosmic rays and hadron acceleration is expected to increase the shock compression ratio, providing higher post-shock densities. We exploited the deep observations of the XMM-Newton Large Program on SN 1006 to verify this prediction. Spatially resolved spectral analysis led us to detect X-ray emission from the shocked ambient medium in SN 1006 and to find that its density significantly increases in regions where particle acceleration is efficient. Our results provide evidence for the effects of acceleration of cosmic ray hadrons on the post-shock plasma in supernova remnants.

scholarly journals Chandra and XMM Observations of Galaxy Groups: The Influence of Central AGN at the Low End of the Cluster Mass Scale

2006 ◽  
Vol 2 (S235) ◽  
pp. 255-255
Author(s):  
J. M. Vrtilek ◽  
E. J. O'Sullivan ◽  
L. P. David
Keyword(s):  
Angular Resolution ◽  
Mass Scale ◽  
Heavy Elements ◽  
High Angular Resolution ◽  
Galaxy Interactions ◽  
X Ray ◽  
Galaxy Groups ◽  
Spatially Resolved ◽  
Formation And Evolution ◽  
Spatially Resolved Spectroscopy

AbstractChandra and XMM, offering between them high angular resolution, substantial collecting area, and spatially-resolved spectroscopy at good spectral resolution, have given us the means to discover hitherto unanticipated phenomena, in groups as in clusters, and to explore a new set of issues that bring us closer to understanding the formation and evolution of groups and their constituent galaxies: the distribution of heavy elements, the presence of X-ray cavities and their relation to radio observations, the nature of cooling cores, and X-ray signatures of recent galaxy interactions. We here show Chandra and XMM data selected to illustrate recent results regarding some of these themes.

scholarly journals Комплекс SOLPEX для исследования излучения Солнца в мягком рентгеновском диапазоне волн

2019 ◽  
Vol 89 (12) ◽  
pp. 1832
Author(s):  
С.В. Кузин ◽  
А.С. Кириченко ◽  
M. Steslicki ◽  
J. Sylwester ◽  
M. Siarkowski ◽  
...  
Keyword(s):  
Time Resolution ◽  
Angular Resolution ◽  
Focal Length ◽  
Space Station ◽  
Pinhole Camera ◽  
International Space ◽  
X Ray ◽  
Spectral Diagnostics ◽  
Input Filter ◽  
Fast Rotating

Abstract The SOLPEX complex consists of two instruments for recording soft X-ray radiation from the Sun and is a part of the KORTES equipment, which will be installed on board the International Space Station. The first instrument is a fast-rotating multi-crystalagg spectrometer designed to record solar spectra in the range of 0.4–23 Å with a time resolution of no less than 0.1 s. The second instrument is a pinhole camera with a focal length of 58 cm. The camera has a field of viewof 2° × 2°, angular resolution of 2 arcmin, and time resolution up to 0.2 s. The energy range is determined by the input filter and is 1–10 keV; the energy resolution is 0.5 keV. The combination of these two instruments makes it possible to locate hot solar sources in the corona, determine their speed, and conduct spectral diagnostics.

scholarly journals Active gas features in three HSC-SSP CAMIRA clusters revealed by high angular resolution analysis of MUSTANG-2 SZE and XXL X-ray observations

2020 ◽  
Vol 501 (2) ◽  
pp. 1701-1732
Author(s):  
Nobuhiro Okabe ◽  
Simon Dicker ◽  
Dominique Eckert ◽  
Tony Mroczkowski ◽  
Fabio Gastaldello ◽  
...  
Keyword(s):  
Large Scale ◽  
Angular Resolution ◽  
Major Axis ◽  
High Angular Resolution ◽  
X Ray ◽  
Spatially Resolved ◽  
Sunyaev Zel'dovich Effect ◽  
Major Merger ◽  
Resolution Analysis ◽  
A Minor

ABSTRACT We present results from simultaneous modelling of high angular resolution GBT/MUSTANG-2 90 GHz Sunyaev–Zel’dovich effect (SZE) measurements and XMM-XXL X-ray images of three rich galaxy clusters selected from the HSC-SSP Survey. The combination of high angular resolution SZE and X-ray imaging enables a spatially resolved multicomponent analysis, which is crucial to understand complex distributions of cluster gas properties. The targeted clusters have similar optical richnesses and redshifts, but exhibit different dynamical states in their member galaxy distributions: a single-peaked cluster, a double-peaked cluster, and a cluster belonging to a supercluster. A large-scale residual pattern in both regular Compton-parameter y and X-ray surface brightness distributions is found in the single-peaked cluster, indicating a sloshing mode. The double-peaked cluster shows an X-ray remnant cool core between two SZE peaks associated with galaxy concentrations. The temperatures of the two peaks reach ∼20–30 keV in contrast to the cool core component of ∼2 keV, indicating a violent merger. The main SZE signal for the supercluster is elongated along a direction perpendicular to the major axis of the X-ray core, suggesting a minor merger before core passage. The SX and y distributions are thus perturbed at some level, regardless of the optical properties. We find that the integrated Compton y parameter and the temperature for the major merger are boosted from those expected by the weak-lensing mass and those for the other two clusters show no significant deviations, which is consistent with predictions of numerical simulations.

scholarly journals Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant

2018 ◽  
Vol 618 ◽  
pp. A155 ◽  
Author(s):  
Iurii Sushch ◽  
Robert Brose ◽  
Martin Pohl
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Supernova Remnants ◽  
High Energy ◽  
Radial Dependence ◽  
Electromagnetic Spectrum ◽  
X Ray ◽  
Spatially Resolved ◽  
Magnetic Field Profile ◽  
Broadband Emission

Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source, making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution one-dimensional (1D) hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field, which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.

scholarly journals Upgrade of the SPECIES beamline at the MAX IV Laboratory

2021 ◽  
Vol 28 (2) ◽  
pp. 588-601
Author(s):  
Esko Kokkonen ◽  
Felipe Lopes da Silva ◽  
Mikko-Heikki Mikkelã ◽  
Niclas Johansson ◽  
Shih-Wen Huang ◽  
...  
Keyword(s):  
Storage Ring ◽  
Time Resolution ◽  
Photoelectron Spectroscopy ◽  
Vacuum Ultraviolet ◽  
Ambient Pressure ◽  
Elevated Pressure ◽  
X Ray ◽  
X Ray Scattering ◽  
Unique Capability ◽  
Ray Scattering

The SPECIES beamline has been transferred to the new 1.5 GeV storage ring at the MAX IV Laboratory. Several improvements have been made to the beamline and its endstations during the transfer. Together the Ambient Pressure X-ray Photoelectron Spectroscopy and Resonant Inelastic X-ray Scattering endstations are capable of conducting photoelectron spectroscopy in elevated pressure regimes with enhanced time-resolution and flux and X-ray scattering experiments with improved resolution and flux. Both endstations offer a unique capability for experiments at low photon energies in the vacuum ultraviolet and soft X-ray range. In this paper, the upgrades on the endstations and current performance of the beamline are reported.

scholarly journals Mapping the gas thermodynamic properties of the massive cluster merger MOO J1142+1527 at z = 1.2

2020 ◽  
Vol 228 ◽  
pp. 00026
Author(s):  
F. Ruppin ◽  
R. Adam ◽  
P. Ade ◽  
P. André ◽  
A. Andrianasolo ◽  
...  
Keyword(s):  
Thermodynamic Properties ◽  
Angular Resolution ◽  
Morphological Properties ◽  
Line Of Sight ◽  
High Angular Resolution ◽  
Signal To Noise ◽  
X Ray ◽  
Spatially Resolved ◽  
Multi Wavelength ◽  
Massive Cluster

We present the results of the analysis of the very massive cluster MOO J1142+1527 at a redshift z = 1.2 based on high angular resolution NIKA2 Sunyaev-Zel’dovich (SZ) and Chandra X-ray data. This multi-wavelength analysis enables us to estimate the shape of the temperature profile with unprecedented precision at this redshift and to obtain a map of the gas entropy distribution averaged along the line of sight. The comparison between the cluster morphological properties observed in the NIKA2 and Chandra maps together with the analysis of the entropy map allows us to conclude that MOOJ1142+1527 is an on-going merger hosting a cool-core at the position of the X-ray peak. This work demonstrates how the addition of spatially-resolved SZ observations to low signal-to-noise X-ray data can bring valuable insights on the intracluster medium thermodynamic properties at z > 1.

scholarly journals X-ray Spectroscopy of the Southwest Cygnus Loop

2004 ◽  
Vol 218 ◽  
pp. 81-82
Author(s):  
D. A. Leahy
Keyword(s):  
Supernova Remnants ◽  
The South ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved ◽  
Analysis Of The Images ◽  
The Right ◽  
Western Limb

The Cygnus Loop is one of the nearest supernova remnants (440 pc) and has been studied extensively in radio through X-ray wavelengths. An unusual bright “V”-shaped region on the south-western limb (near RA 20h46m and Decl. +30°) was revealed in ROSAT PSPC observations of the Cygnus Loop. The left side of the “V” has one of the highest hardness ratios (0.9–2 keV / 0.1–0.4 keV) in the Cygnus Loop whereas the right side has one of the lowest. Images and spatially resolved spectra were obtained using Chandra ACIS observations. Some results of analysis of the images and spectra are presented here.

scholarly journals Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin

2019 ◽  
Vol 629 ◽  
pp. A51 ◽  
Author(s):  
Ping Zhou ◽  
Jacco Vink ◽  
Samar Safi-Harb ◽  
Marco Miceli
Keyword(s):  
Supernova Remnants ◽  
Supernova Explosion ◽  
Mass Range ◽  
Large Mass ◽  
Explosion Energy ◽  
X Ray ◽  
Spatially Resolved ◽  
Normal Mass ◽  
Solar Abundances ◽  
Progenitor Stars

Magnetars are regarded as the most magnetized neutron stars in the Universe. Aiming to unveil what kinds of stars and supernovae can create magnetars, we have performed a state-of-the-art spatially resolved spectroscopic X-ray study of the supernova remnants (SNRs) Kes 73, RCW 103, and N49, which host magnetars 1E 1841−045, 1E 161348−5055, and SGR 0526−66, respectively. The three SNRs are O- and Ne-enhanced and are evolving in the interstellar medium with densities of > 1 − 2 cm−3. The metal composition and dense environment indicate that the progenitor stars are not very massive. The progenitor masses of the three magnetars are constrained to be < 20 M⊙ (11–15 M⊙ for Kes 73, ≲13 M⊙ for RCW 103, and ∼13 − 17 M⊙ for N49). Our study suggests that magnetars are not necessarily made from very massive stars, but originate from stars that span a large mass range. The explosion energies of the three SNRs range from 1050 erg to ∼2 × 1051 erg, further refuting that the SNRs are energized by rapidly rotating (millisecond) pulsars. We report that RCW 103 is produced by a weak supernova explosion with significant fallback, as such an explosion explains the low explosion energy (∼1050 erg), small observed metal masses (MO ∼ 4 × 10−2 M⊙ and MNe ∼ 6 × 10−3 M⊙), and sub-solar abundances of heavier elements such as Si and S. Our study supports the fossil field origin as an important channel to produce magnetars, given the normal mass range (MZAMS <  20 M⊙) of the progenitor stars, the low-to-normal explosion energy of the SNRs, and the fact that the fraction of SNRs hosting magnetars is consistent with the magnetic OB stars with high fields.

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