SWIFT
                    /BAT DETECTION OF HARD X-RAYS FROM TYCHO'S SUPERNOVA REMNANT: EVIDENCE FOR TITANIUM-44

Supernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into the acceleration of particles to high energies. This paper reviews the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implications for Galactic cosmic ray distribution are discussed.

Download Full-text

Numerically investigating the morphology of the supernova remnant SN 1006 in the ambient medium with a density discontinuity

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3214 ◽

2019 ◽

Vol 491 (2) ◽

pp. 2460-2464 ◽

Cited By ~ 2

Author(s):

Jun Fang ◽

Jingwen Yan ◽

Lu Wen ◽

Chunyan Lu ◽

Huan Yu

Keyword(s):

Supernova Remnant ◽

Ambient Medium ◽

X Rays ◽

X Ray ◽

North West ◽

Density Discontinuity ◽

North East ◽

The North ◽

South West ◽

Type Ia

ABSTRACT Multiband observations on the Type Ia supernova remnant SN 1006 indicate peculiar properties in its morphologies of emission in the radio, optical, and X-ray bands. In the hard X-rays, the remnant is bilateral with two opposite bright limbs with prominent protrusions. Moreover, a filament has been detected at the radio, optical, and soft X-ray wavelengths. The reason for these peculiar features in the morphologies of the remnant is investigated using 3D HD simulations. With the assumption that the supernova ejecta are evolved in the ambient medium with a density discontinuity, the radius of the remnant’s boundary is smaller in the tenuous medium, and the shell consists of two hemispheres with different radii. Along particular line of sights, protrusions appear on the periphery of the remnants since the emission from the edge of the hemisphere with a larger radius is located outside that from the shell of the small hemisphere. Furthermore, the north-west filament of SN 1006 arises as a result of the intersection of the line of sight and the shocked material near the edges of the two hemispheres. It can be concluded that the protrusions on the north-east and south-west limbs and the north-west filament in the morphologies of SN 1006 can be reproduced as the remnants interacting with the medium with a density discontinuity.

Download Full-text

XMM-Newton and Fermi/LAT view on the supernova remnant 3C434.1

Astronomy and Astrophysics ◽

10.1051/0004-6361/201935487 ◽

2019 ◽

Vol 631 ◽

pp. A179

Author(s):

V. Doroshenko ◽

D. Malyshev ◽

G. Pühlhofer ◽

B. Dincel ◽

M. Sasaki ◽

...

Keyword(s):

Power Law ◽

Supernova Remnant ◽

X Rays ◽

Significant Excess ◽

X Ray ◽

Thermal Origin

We report on XMM-Newton observations of the supernova remnant (SNR) 3C434.1 (G94.0+1.0), the first in X-rays since the ROSAT era. Our analysis confirms the thermal origin of the observed extended X-ray emission, whose morphology appears more complex than previously reported. In particular, part of the shell shows a significantly harder spectrum which is consistent with a power law, and it is, therefore, likely of non-thermal origin. Motivated by these finding, we revisited the GeV observations of the field taken with the Fermi observatory. A significant excess associated with the remnant was detected, which is likely associated with non-thermal X-ray emission from part of the shell. The analysis of the Fermi data resulted in the serendipity discovery of GeV emission from the nearby SNR G093.7-00.2. Finally, we searched for a possible compact remnants within the shell, however, no obvious candidates could be identified due to the fairly large positional uncertainties.

Download Full-text

Fast-moving pulsars as probes of interstellar medium

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1601 ◽

2020 ◽

Vol 497 (3) ◽

pp. 2605-2615

Author(s):

Maxim V Barkov ◽

Maxim Lyutikov ◽

Dmitry Khangulyan

Keyword(s):

Interstellar Medium ◽

Fast Moving ◽

Supernova Remnant ◽

Characteristic Length ◽

Line Emission ◽

Bow Shock ◽

Spatial Inhomogeneity ◽

X Rays ◽

Forward Shock ◽

Bow Shocks

ABSTRACT Pulsars moving through interstellar medium (ISM) produce bow shocks detected in hydrogen H α line emission. The morphology of the bow shock nebulae allows one to probe the properties of ISM on scales ∼0.01 pc and smaller. We performed 2D relativistic magnetohydrodynamic modelling of the pulsar bow shock and simulated the corresponding H α emission morphology. We find that even a mild spatial inhomogeneity of ISM density, δρ/ρ ∼ 1, leads to significant variations of the shape of the shock seen in H α line emission. We successfully reproduce the morphology of the Guitar Nebula. We infer quasi-periodic density variations in the warm component of ISM with characteristic length of ∼0.1 pc. Structures of this scale might be also responsible for the formation of the fine features seen at the forward shock of Tycho supernova remnant (SNR) in X-rays. Formation of such short periodic density structures in the warm component of ISM is puzzling, and bow-shock nebulae provide unique probes to study this phenomenon.

Download Full-text

Search for Nonthermal X-Rays from Supernova Remnant Shells

Symposium - International Astronomical Union ◽

10.1017/s0074180900114573 ◽

1998 ◽

Vol 188 ◽

pp. 117-120

Author(s):

R. Petre ◽

J. Keohane ◽

U. Hwang ◽

G. Allen ◽

E. Gotthelf

Keyword(s):

Radio Emission ◽

Supernova Remnants ◽

Supernova Remnant ◽

Cosmic Ray ◽

High Energy ◽

X Rays ◽

X Ray ◽

Nonthermal Radio ◽

Cosmic Ray Acceleration ◽

Nonthermal Radio Emission

The suggestion that the shocks of supernova remnants (SNR's) are cosmic ray acceleration sites dates back more than 40 years. While observations of nonthermal radio emission from SNR shells indicate the ubiquity of GeV cosmic ray production, there is still theoretical debate about whether SNR shocks accelerate particles up to the well-known “knee” in the primary cosmic ray spectrum at ~3,000 TeV. Recent X-ray observations of SN1006 and other SNR's may have provided the missing observational link between SNR shocks and high energy cosmic ray acceleration. We discuss these observations and their interpretation, and summarize our ongoing efforts to find evidence from X-ray observations of cosmic ray acceleration in the shells of other SNR's.

Download Full-text

Historical Supernovae and Supernova Remnants

International Astronomical Union Colloquium ◽

10.1017/s0252921100008174 ◽

1996 ◽

Vol 145 ◽

pp. 323-331 ◽

Cited By ~ 2

Author(s):

Zhenru Wang

Keyword(s):

Tang Dynasty ◽

Supernova Remnants ◽

Supernova Remnant ◽

High Energy ◽

X Rays ◽

Supernovae And Supernova Remnants ◽

X Ray ◽

The Tang Dynasty ◽

High Energy Emission ◽

The Relationship

The oldest historical supernova (SN), recorded by ancient Chinese in 14th Century B.C. on pieces of tortoise shells or bones, is identified with the aid of modern space γ-ray observations. Hard X-rays with energy up to 20 keV were observed from IC 443 by the X-ray satellite Ginga. We infer from these observations the age of IC 443 is ∼ 1000 — 1400 yrs. The result supports the hypothesis that IC 443 is the remnant of the historical SN 837 that occurred during the Tang Dynasty. The association between the supernova remnant (SNR) CTB 80 and SN 1408 has been hotly debated for about ten years and is briefly reviewed and discussed here. A new picture is presented to explain this association. High energy emission from historical SNRs can persist in a multiphase interstellar medium (ISM). As a result, the study of the relationship between SNRs and ancient guest stars has gained new vitality.

Download Full-text

Synchrotron Models for X-Rays from the Supernova Remnant SN 1006

The Astrophysical Journal ◽

10.1086/309936 ◽

1996 ◽

Vol 459 (1) ◽

Cited By ~ 107

Author(s):

Stephen P. Reynolds

Keyword(s):

Supernova Remnant ◽

X Rays

Download Full-text

Temporal and spatial variation of synchrotron X-ray stripes in Tycho’s supernova remnant

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psaa075 ◽

2020 ◽

Vol 72 (5) ◽

Author(s):

Masamune Matsuda ◽

Takaaki Tanaka ◽

Hiroyuki Uchida ◽

Yuki Amano ◽

Takeshi Go Tsuru

Keyword(s):

Surface Brightness ◽

Supernova Remnant ◽

Time Variability ◽

X Rays ◽

Temporal And Spatial Variation ◽

Proton Acceleration ◽

X Ray ◽

Temporal And Spatial ◽

Imaging And Spectroscopy ◽

The Magnetic Field

Abstract The synchrotron X-ray “stripes” discovered in Tycho’s supernova remnant (SNR) have been attracting attention as they may be evidence for proton acceleration up to PeV. We analyzed Chandra data taken in 2003, 2007, 2009, and 2015 for imaging and spectroscopy of the stripes in the southwestern region of the SNR. Comparing images obtained at different epochs, we find that time variability of synchrotron X-rays is not limited to two structures previously reported but is more common in the region. Spectral analysis of nine bright stripes reveals not only their time variabilities but also a strong anti-correlation between the surface brightness and photon indices. The spectra of the nine stripes have photon indices of Γ = 2.1–2.6 and are significantly harder than those of the outer rim of the SNR in the same region with Γ = 2.7–2.9. Based on these findings, we indicate that the magnetic field is substantially amplified, and suggest that particle acceleration through a stochastic process may be at work in the stripes.

Download Full-text

N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

Symposium - International Astronomical Union ◽

10.1017/s0074180900034458 ◽

1983 ◽

Vol 101 ◽

pp. 573-577

Author(s):

G. Pizzichini ◽

T. L. Cline ◽

U. D. Desai ◽

B. J. Teegarden ◽

W. D. Evans ◽

...

Keyword(s):

High Resolution ◽

Supernova Remnant ◽

Gamma Ray ◽

Large Magellanic Cloud ◽

X Rays ◽

Radio Image ◽

Gamma Ray Burst ◽

X Ray ◽

Preliminary Results ◽

Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

Download Full-text