X-Ray Measured Dynamics of Tycho's Supernova Remnant

Katsuda, Satoru; Petre, Robert; Hughes, John P.; Hwang, U.; Yamaguchi, Hiroya; Hayato, Asami; Mori, Koji; Tsunemi, H.

doi:10.1088/0004-637x/709/2/1387

Cited by 98 publications

(127 citation statements)

References 45 publications

(60 reference statements)

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“…Interestingly, the expansion rate of Tycho in the eastern part, where the ejecta are very close to the shock front, is also much lower than expected for a SNR expanding in a homogeneous medium (Katsuda et al 2010). It is, therefore, possible that also in Tycho the initial stratification is no longer visible, as the layers have been squeezed together due to the presence of a strong density gradient, and perhaps even mixed due hydrodynamical instabilities.…”

Section: Comparison Of the Stratification With Other Type Ia Supernovmentioning

confidence: 89%

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Kosenko

Helder

Vink

2010

A&A

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We present a detailed analysis of the XMM-Newton and Chandra X-ray data of the young type Ia supernova remnant SNR 0519-69.0, which is situated in the Large Magellanic Cloud. We used data from both the Chandra ACIS and XMM-Newton EPIC MOS instruments, and high resolution X-ray spectra obtained with the XMM-Newton reflection grating spectrometer (RGS). Our analysis of the spatial distribution of X-ray line emission using the Chandra data shows that there is a radial stratification of oxygen, intermediate mass elements (IME) and iron, with the emission from more massive elements peaking more toward the center. Using a deprojection technique we measure a forward shock radius of 4.0 ± 0.3 pc and a reverse shock radius of 2.7 ± 0.4 pc. We took the observed stratification of the shocked ejecta into account in the modeling of the X-ray spectra, for which we used multicomponent non-equilibrium ionization models, with the components corresponding to layers dominated by one or two elements. An additional component was added in order to represent the shocked interstellar medium, which mostly contributed to the continuum emission. This multicomponent model fits the data adequately, and was also employed to characterize the spectra of distinct regions extracted from the Chandra data. From our spectral analysis we find that the approximate fractional masses of shocked ejecta for the most abundant elements are: M O ≈ 32%, M Si/S ≈ 7%/5%, M Ar+Ca ≈ 1% and M Fe ≈ 55%. From the continuum component we derive a circumstellar density of n H = 2.4 ± 0.2 cm −3 . This density, together with the measurements of the forward and reverse shock radii suggest an age of 0519-69.0 of 450 ± 200 yr, somewhat lower than, but consistent with the age estimate based on the extent of the light echo (600 ± 200 yr). Finally, from the high resolution RGS spectra we measured a Doppler broadening of σ = 1873 ± 50 km s −1 , from which we derive a forward shock velocity of v FS = 2770 ± 500 km s −1 . We discuss our results in the context of single degenerate explosion models, using semi-analytical and numerical modeling, and compare the characteristics of 0519-69.0 with those of other type Ia supernova remnants.

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Section: Comparison Of the Stratification With Other Type Ia Supernovmentioning

confidence: 89%

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Kosenko

Helder

Vink

2010

A&A

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“…Tycho is no exception, showing evidence of narrow nonthermal X-ray rims pointing to magnetic fields as large as a few hundred μG (Hwang et al 2002;Bamba et al 2005;Warren et al 2005;Katsuda et al 2010;Eriksen et al 2011). We model magnetic field amplification due to resonant streaming instability as in Caprioli et al (2009a), i.e., by assuming that saturation is achieved when P w P cr /2M A , where P w and P cr are the pressure in Alfvén waves and in CRs, normalized to the ram pressure ρ 0 V 2 sh , and M A is the Alfvénic Mach number (43) in Caprioli et al 2009a) as…”

Section: Magnetic Field Amplificationmentioning

confidence: 99%

“…High-resolution X-ray maps reveal strong nonthermal emission concentrated in thin filaments (Hwang et al 2002;Bamba et al 2005;Warren et al 2005;Katsuda et al 2010;Eriksen et al 2011). The thickness of these filaments is usually interpreted as severe synchrotron losses of high-energy electrons radiating in a strong magnetic field (e.g.…”

Section: Introductionmentioning

confidence: 99%

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Morlino

Caprioli

2012

A&A

289

312

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Context. Very recent gamma-ray observations of G120.1+1.4 (Tycho's) supernova remnant (SNR) by Fermi-LAT and VERITAS have provided new fundamental pieces of information for understanding particle acceleration and nonthermal emission in SNRs. Aims. We want to outline a coherent description of Tycho's properties in terms of SNR evolution, shock hydrodynamics, and multiwavelength emission by accounting for particle acceleration at the forward shock via first-order Fermi mechanism. Methods. We adopt here a quick and reliable semi-analytical approach to nonlinear diffusive shock acceleration. It includes magnetic field amplification due to resonant streaming instability and the dynamical backreaction on the shock of both cosmic rays (CRs) and self-generated magnetic turbulence. Results. We find that Tycho's forward shock accelerates protons up to at least 500 TeV, channelling into CRs about 10% of its kinetic energy. Moreover, the CR-induced streaming instability is consistent with all the observational evidence of very efficient magnetic field amplification (up to ∼300 μG). In such a strong magnetic field, the velocity of the Alfvén waves scattering CRs in the upstream is expected to be enhanced and to make accelerated particles feel an effective compression factor lower than 4, in turn leading to an energy spectrum steeper than the standard prediction ∝E −2 . This effect is crucial for explaining GeV-to-TeV gamma-ray spectrum as the result of neutral pions decay produced in nuclear collisions between accelerated nuclei and the background gas. Conclusions. The self-consistency of such hadronic scenario, along with the inability of the concurrent leptonic mechanism (inverse Compton scattering of relativistic electrons on several photon backgrounds) to reproduce both the shape and the normalization of the detected gamma-ray emission, represents the first clear and direct radiative evidence that hadron acceleration occurs efficiently in young Galactic SNRs.

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“…Nevertheless, Tian & Leahy (2011) suggest that the atomic hydrogen (HI) gas at velocities of −47 to −53 km s −1 , which was once considered to be interacting with the shock waves from the explosion (Reynoso et al 1999), is located in front of Tycho's SNR. These authors also argued that the CO molecular gas at a velocity of ∼ − 64 km s −1 (Lee et al 2004;Cai et al 2009;Xu et al 2011) is not interacting with the remnant either, because the derived gas density from the CO observations (∼ 200 cm −3 ) is much larger than the density referred from the X-ray observations (∼ 0.2 cm −3 ; Katsuda et al 2010). However, the re-analysis of the high-energy observations (including X-and γ-ray data) of Tycho's SNR suggested a denser ambient medium (∼ 4-12 cm −3 on average; Zhang et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Chen¹,

Xiong²,

Yang³

2017

A&A

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Context. The investigation of the interaction between the supernova remnants (SNRs) and interstellar gas is not only necessary to improve our knowledge of SNRs, but also to understand the nature of the progenitor systems. Aims. As a part of the Milky Way Imaging Scroll Painting CO line survey, the aim is to study the interstellar gas surrounding the Galactic historical SNRs. In this work, we present the CO results of Tycho's SNR. Methods. Using the 3×3 Superconducting Spectroscopic Array Receiver (SSAR) at the PMO 13.7-meter telescope, we performed large-field (3 • × 2 • ) and high-sensitivity CO (1-0) molecular line observations toward Tycho's SNR. Results. The CO observations reveal large molecular clouds, stream-like structures, and an inner rim around the remnant. We derived the basic properties (column density, mass, and kinematics) of these objects based on the CO observations. The large molecular clouds individually show an arc toward the remnant center, outlining a large cavity with radii of ∼ 0.3 • × 0.6 • (or 13 pc × 27 pc at a distance of 2.5 kpc) around the remnant. The CO line broadenings and asymmetries detected in the surrounding clouds, the observed expansion of the cavity, in concert with enhanced 12 CO (2-1)/(1-0) intensity ratio detected in previous studies, suggest the interaction of the large cavity with a wind in the region. After excluding the scenario of a large bubble produced by bright massive stars, we suggest that the large cavity could be explained by accretion wind from the progenitor system of Tycho's supernova. Nevertheless, the possibility of the random distribution of a large cavity around Tycho's SNR cannot be ruled out thus far. Further observations are needed to confirm the physical association of the large cavity with Tycho's SNR.

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X-Ray Measured Dynamics of Tycho's Supernova Remnant

Cited by 98 publications

References 45 publications

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

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