HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-5<i>6</i>

Temim, Tea; Slane, Patrick; Castro, Daniel; Plucinsky, Paul P.; Gelfand, Joseph D.; Dickel, John R.

doi:10.1088/0004-637x/768/1/61

Cited by 34 publications

(50 citation statements)

References 30 publications

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“…The average radius of the SNR shell in the four panels is 10 pc, 13 pc, 17 pc, and 19 pc, in order of increasing SNR age. sured in Temim et al (2013). In this case, the ratio L X /Ė = 0.00235 is within the range of luminosities observed for other pulsars (Possenti et al 2002).…”

Section: Model Parameterssupporting

confidence: 80%

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Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

Temim

Slane

Plucinsky

et al. 2017

ApJ

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We present a measurement of the proper motion of the presumed pulsar in the evolved composite supernova remnant (SNR) MSH 15-56 whose pulsar wind nebula (PWN) has been disrupted by the supernova (SN) reverse shock. Using Chandra X-ray observations acquired over a baseline of 15 years, we measure a pulsar velocity of 720 +290 −215 km s −1 and a direction of motion of 14 • ± 22• west of south. We use this measurement to constrain a hydrodynamical model for the evolution of this system and find that its morphology is well-described by an SNR expanding in an ambient density gradient that increases from east to west. The effect of the density gradient and the pulsar's motion is an asymmetric interaction between the SN reverse shock and the PWN that displaces the bulk of the PWN material away from the pulsar, towards the northeast. The simulation is consistent with an SNR age of 11,000 years, an SN ejecta mass of 10 M , and an average surrounding density of 0.4cm −3 . However, a combination of a higher SN ejecta mass and ambient density can produce a similar SNR morphology at a later age.

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Section: Model Parameterssupporting

confidence: 80%

“…The mass of the SN ejecta was set to 10 M , the low end value predicted by the models of Sukhbold et al (2016). The minimum ISM density was set to n 0 = 0.1 cm −3 (Temim et al 2013), increasing by a factor of eight in a direction perpendicular to the direction of the pulsar's motion.…”

Section: Model Parametersmentioning

confidence: 99%

Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

Temim

Slane

Plucinsky

et al. 2017

ApJ

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“…5 Note that the obtained velocity of the pulsar is about five times larger than 410 km s −1 reported by Temim et al (2013). This discrepancy may arise from the different assumptions of the pulsar birthplace, the age of the SNR, and the radial velocity of the pulsar.…”

Section: Estimation Of the Proper Motion Velocitymentioning

confidence: 86%

SPATIALLY RESOLVED SPECTROSCOPY OF A PULSAR WIND NEBULA IN MSH 15–56

Yatsu

Asano

Kawai

et al. 2013

ApJ

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We report the study of a pulsar wind nebula (PWN) in the middle-aged supernova remnant (SNR) MSH 15−56. High-resolution X-ray imaging observations using XMM-Newton and Chandra provided clear images of its cometlike structure, as seen in other PWNe moving rapidly through interstellar mediums. At the PWN apex, Chandra detected a point source emitting a power-law spectrum with a photon index of Γ = 1.3. The photon index of the PWN steepens from 1.7 to 2.5 along the flow line from the apex toward the tail, implying that the PWN is powered by the point source. The opening angle of the tail implies a pulsar velocity of v PSR = 1900 km s −1 . We also discovered a thin X-ray filament at the edge of the SNR and just near the PWN. Assuming that the SNR is in the Sedov phase, the shell is expanding at 860 km s −1 , which is consistent with the existence of the non-thermal filament. Based on the physical relationship, the PWN will run through the blast wave in the near future.

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“…Radio observations revealed a SNR shell and a luminous PWN (Dickel et al 2000). It was also detected in Xrays by ROSAT (Kassim et al 1993), ASCA (Plucinsky 1998), XMM-Newton and Chandra (Temim et al 2013). It has clumpy X-ray emission, with enhancement near the PWN.…”

Section: Properties Of the Snrsmentioning

confidence: 95%

“…It has clumpy X-ray emission, with enhancement near the PWN. Temim et al (2013) performed spectral analysis of eight regions in the southwest area of MSH 15−56 using Chandra and XMM-Newton observations, focusing on the pulsar and the surrounding regions. An absorbed, twocomponent model with a power-law and a NEI plasma was needed to accurately fit the spectra.…”

Section: Properties Of the Snrsmentioning

confidence: 99%

Comparing Neutron Star Kicks to Supernova Remnant Asymmetries

Holland-Ashford

Lopez

Auchettl

et al. 2017

ApJ

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Supernova explosions are inherently asymmetric and can accelerate new-born neutron stars (NSs) to hundreds of km s −1 . Two prevailing theories to explain NS kicks are ejecta asymmetries (e.g., conservation of momentum between NS and ejecta) and anisotropic neutrino emission. Observations of supernova remnants (SNRs) can give us insights into the mechanism that generates these NS kicks. In this paper, we investigate the relationship between NS kick velocities and the X-ray morphologies of 18 SNRs observed with the Chandra X-ray Observatory and the Röntgen Satellite (ROSAT). We measure SNR asymmetries using the power-ratio method (a multipole expansion technique), focusing on the dipole, quadrupole, and octupole power-ratios. Our results show no correlation between the magnitude of the power-ratios and NS kick velocities, but we find that for Cas A and G292.0+1.8, whose emission traces the ejecta distribution, their NSs are preferentially moving opposite to the bulk of the X-ray emission. In addition, we find a similar result for PKS 1209-51, CTB 109, and Puppis A; however their emission is dominated by circumstellar/interstellar material, so their asymmetries may not reflect their ejecta distributions. Our results are consistent with the theory that NS kicks are a consequence of ejecta asymmetries as opposed to anisotropic neutrino emission. In the future, additional observations to measure NS proper motions within ejecta-dominated SNRs are necessary to constrain robustly the NS kick mechanism.

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HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

Cited by 34 publications

References 30 publications

Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

SPATIALLY RESOLVED SPECTROSCOPY OF A PULSAR WIND NEBULA IN MSH 15–56

Comparing Neutron Star Kicks to Supernova Remnant Asymmetries

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