EXPANSION VELOCITY OF EJECTA IN TYCHO's SUPERNOVA REMNANT MEASURED BY DOPPLER BROADENED X-RAY LINE EMISSION

Hayato, Asami; Yamaguchi, Hiroya; Tamagawa, Toru; Katsuda, Satoru; Hwang, U.; Hughes, John P.; Ozawa, Masanao; Bamba, Aya; Kinugasa, K.; Terada, Y.; Furuzawa, Akihiro; Kunieda, H.; Makishima, Kazuo

doi:10.1088/0004-637x/725/1/894

Cited by 105 publications

(113 citation statements)

References 38 publications

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“…In the literature different techniques have been adopted to provide an estimate of such a distance, always returning a value ranging between 2 and 5 kpc (see Hayato et al 2010, for a review). Kinematic methods give a distance of 2.5−3 kpc (Tian & Leahy 2011).…”

Section: Modeling Tychomentioning

confidence: 99%

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Morlino

Caprioli

2012

A&A

299

313

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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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Section: Modeling Tychomentioning

confidence: 99%

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Morlino

Caprioli

2012

A&A

299

313

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“…We found that Fe Kα is broadened by 101 +33 −27 eV (1-σ), for the first time from SN 1006. If this width is owing to the Doppler broadening of ejecta, as is the case of Tycho (Hayato et al 2010), the expansion velocity in the line of sight should be ∼ 3000 km s −1 . This value is consistent with that of Katsuda et al (2013), in which they measured the proper motion of the NW rim in X-ray.…”

Section: Three-dimensional Geometry Of Sn 1006mentioning

confidence: 99%

Asymmetric Ejecta Distribution in Sn 1006

Uchida

Yamaguchi

Koyama

2013

ApJ

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We present the results from deep X-ray observations (∼ 400 ks in total) of SN 1006 by the X-ray astronomy satellite Suzaku. The thermal spectrum from the entire supernova remnant (SNR) exhibits prominent emission lines of O, Ne, Mg, Si, S, Ar, Ca, and Fe. The observed abundance pattern in the ejecta components is in good agreement with that predicted by a standard model of Type Ia supernovae (SNe). The spatially resolved analysis reveals that the distribution of the O-burning and incomplete Si-burning products (Si, S, and Ar) is asymmetric, while that of the C-burning products (O, Ne, and Mg) is relatively uniform in the SNR interior. The peak position of the former is clearly shifted by 5 ′ (∼3.2 pc at a distance of 2.2 kpc) to the southeast from the SNR's geometric center. Using the SNR age of ∼1000 yr, we constrain the velocity asymmetry (in projection) of ejecta to be ∼3100 km s −1 . The abundance of Fe is also significantly higher in the southeast region than in the northwest region. Given that the non-uniformity is observed only among the heavier elements (Si through Fe), we argue that SN 1006 originates from an asymmetric explosion, as is expected from recent multi-dimensional simulations of Type Ia SNe, although we cannot eliminate the possibility that an inhomogeneous ambient medium induced the apparent non-uniformity. Possible evidence for the Cr K-shell line and line broadening in the Fe K-shell emission is also found.

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“…H i absorption studies (Tian & Leahy 2011) favor a distance on the near side of the Perseus arm (2.5 to 3 kpc). On the other hand, Hayato et al (2010) measured the shocked ejecta velocity to be about 4700 km s −1 for Si, S, and Ar. They concluded that the distance is 3 to 5 kpc on consideration of the measured proper motion.…”

Section: Introductionmentioning

confidence: 99%

FERMI LARGE AREA TELESCOPE DETECTION OF THE YOUNG SUPERNOVA REMNANT TYCHO

Giordano

Naumann-Godó

Ballet

et al. 2011

ApJ

159

137

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After almost three years of data taking in sky-survey mode, the Fermi Large Area Telescope has detected γ -ray emission toward Tycho's supernova remnant (SNR). The Tycho SNR is among the youngest remnants in the Galaxy, originating from a Type Ia Supernova in AD 1572. The γ -ray integral flux from 400 MeV up to 100 GeV has been measured to be (3.5 ± 1.1 stat ± 0.7 syst )× 10 −9 cm −2 s −1 with a photon index of 2.3 ± 0.2 stat ± 0.1 syst . A simple model consistent with TeV, X-ray, and radio data is sufficient to explain the observed emission as originating from π 0 decays as a result of cosmic-ray acceleration and interaction with the ambient medium.

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EXPANSION VELOCITY OF EJECTA IN TYCHO's SUPERNOVA REMNANT MEASURED BY DOPPLER BROADENED X-RAY LINE EMISSION

Cited by 105 publications

References 38 publications

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Strong evidence for hadron acceleration in Tycho’s supernova remnant

Asymmetric Ejecta Distribution in Sn 1006

FERMI LARGE AREA TELESCOPE DETECTION OF THE YOUNG SUPERNOVA REMNANT TYCHO

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