The Morphologies and Kinematics of Supernova Remnants

Lopez, Laura A.; Fesen, Robert A.

doi:10.1007/s11214-018-0481-x

Cited by 33 publications

(33 citation statements)

References 119 publications

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“…Note that we have only considered constant accretion rates here, whereas scenarios with changing accretion rates are more realistic for CCOs, as their environment is highly variable (see, e.g., Vink 2012;Lopez & Fesen 2018). For example, it is possible that the NS initially accretes at very low rates after the nearby environment has been cleared out by the SN shock.…”

Section: Discussionmentioning

confidence: 99%

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Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Wijngaarden

Chang

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A critical relation in the study of neutron star cooling is the one between surface temperature and interior temperature. This relation is determined by the composition of the neutron star envelope and can be affected by the process of diffusive nuclear burning (DNB), which occurs when elements diffuse to depths where the density and temperature are sufficiently high to ignite nuclear burning. We calculate models of H-He and He-C envelopes that include DNB and obtain analytic temperature relations that can be used in neutron star cooling simulations. We find that DNB can lead to a rapidly changing envelope composition and prevents the build-up of thermally stable hydrogen columns y H 10 7 g cm −2 , while DNB can make helium envelopes more transparent to heat flux for surface temperatures T s 2× 10 6 K. We perform neutron star cooling simulations in which we evolve temperature and envelope composition, with the latter due to DNB and accretion from the interstellar medium. We find that a time-dependent envelope composition can be relevant for understanding the longterm cooling behaviour of isolated neutron stars. We also report on the latest Chandra observations of the young neutron star in the Cassiopeia A supernova remnant; the resulting 13 temperature measurements over more than 18 years yield a ten-year cooling rate of ≈ 2%. Finally, we fit the observed cooling trend of the Cassiopeia A neutron star with a model that includes DNB in the envelope.

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Section: Discussionmentioning

confidence: 99%

“…Furthermore, when considering central compact objects (CCOs), the NS is within a supernova remnant, for which the distribution and composition differ from the ISM (see, e.g. Vink 2012; Lopez & Fesen 2018). Following classical accretion physics (see, e.g.…”

Section: Ism Accretion Ratesmentioning

confidence: 99%

Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Wijngaarden

Chang

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…To make major progress, we need observations that reveal the 3D structure of SNRs, as was done for Cas A (DeLaney et al 2010;Milisavljevic & Fesen 2015). See Lopez & Fesen (2018) for the exciting prospects in the X-ray domain. This will realize the full potential of 3D simulations, from the SN to the SNR.…”

Section: Resultsmentioning

confidence: 99%

“…1 Energetic particles radiate at both ends of the spectrum: electrons produce synchrotron radiation in a magnetic field, from radio to gamma energies, and inverse Compton radiation on the ambient photon fields, in -rays; protons induce pion decay from collisions with ambient matter, which also produces -ray photons. See Reynolds (2008) and Vink (2012) for reviews of observations from the high-energy perspective, and Lopez & Fesen (2018) for a review focused on morphology and kinematics. 2 1 The shocked ejecta can also be detected in the optical: see the discovery by Seitenzahl et al (2019).…”

Section: Introduction To Supernova Remnantsmentioning

confidence: 99%

Modeling and simulations of supernova remnants: A short review focused on recent progress in morphological studies

Ferrand

2020

Astron Nachr

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Supernova remnants (SNRs) are the outcome of supernovae (SNe, either core collapse or thermonuclear). The remnant results from the interaction between the stellar ejecta and the ambient medium around the progenitor star. Young SNRs are characterized by strong shocks that heat and ionize the gas, generate magneto‐hydrodynamic turbulence, and accelerate particles to relativistic energies. They radiate at all wavelengths, especially in the X‐ray domain, where spectro‐imaging observations can provide a wealth of information. This paper presents recent progress in the modeling of SNRs, particularly by means of numerical simulations, and with a focus on three‐dimensional aspects. In the first part we will consider SNRs as producers of cosmic rays (CRs). If SNRs are accelerators efficient enough to power the Galactic component of CRs, this must have a visible impact on their dynamics and, therefore, on the thermal emission from the plasma, as well as on their non‐thermal emission. In the second part we will consider SNRs as probes of the explosion mechanism. The time has come to connect multidimensional simulations of SNe and simulations of SNRs, opening the possibility to study the explosion mechanism via the dynamics and morphology of SNRs.

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“…For SNR, spatially resolved high resolution spectroscopy provided by Athena X‐IFU will enable the derivation of 3D maps for the different synthesized elements in the ejected material. The morphology of SNRs is indeed a clue to SN type, explosion mechanism, and progenitor (e.g., see, the review by Lopez & Fesen . More precisely, the morphology and asymmetries in the ejection of the supernova material are intimately related to the properties of the explosion mechanism, whose understanding is still incomplete.…”

Section: Breakthroughs Expected From Athena On the Astrophysics Of Exmentioning

confidence: 99%

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

et al. 2020

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The properties (temperature, density, chemical composition, velocity) of hot astrophysical plasma and the physical processes affecting them (heating/cooling, turbulence, shocks, acceleration) can be probed by high‐resolution X‐ray spectroscopy, to be complemented by high‐spatial‐resolution imaging. The paper presents the status of the European Space Agency's Advanced Telescope for High Energy Astrophysics (Athena) mission, particularly focusing on the science performance of its two focal‐plane instruments for studies of extended X‐ray sources: the wide‐field imager and the X‐ray integral field unit. This paper then provides a brief summary of the breakthroughs expected with Athena on the astrophysics of hot plasma, building on the vast heritage of the discoveries and revolutionary results obtained by Chandra and XMM‐Newton in this field. As of November 12, 2019, Athena successfully concluded its feasibility study, and has since then moved into the definition phase, with a launch date scheduled in the early 2030s.

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The Morphologies and Kinematics of Supernova Remnants

Cited by 33 publications

References 119 publications

Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Modeling and simulations of supernova remnants: A short review focused on recent progress in morphological studies

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

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The Morphologies and Kinematics of Supernova Remnants

Cited by 33 publications

References 119 publications

Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Diffusive nuclear burning in cooling simulations and application to new temperature data of the Cassiopeia A neutron star

Modeling and simulations of supernova remnants: A short review focused on recent progress in morphological studies

The Athena space X‐ray observatory and the astrophysics of hot plasma†

Contact Info

Product

Resources

About

The Athena space X‐ray observatory and the astrophysics of hot plasma^†