Relevant bibliographies by topics / Supernova remnants

Academic literature on the topic 'Supernova remnants'

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Published: 4 June 2021
Last updated: 30 July 2024

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Journal articles on the topic "Supernova remnants"

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Kirshner, Robert P. "Supernova Remnants and their Supernovae." International Astronomical Union Colloquium 101 (1988): 1–14. http://dx.doi.org/10.1017/s0252921100102027.

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AbstractObserving supernova remnants provides important clues to the nature of supernova explosions. Conversely, the late stages of stellar evolution and the mechanism of supernova explosions affect supernova remnants through circumstellar matter, stellar remnants, and nucleosynthesis. The elements of supernova classification and the connection between supernova type and remnant properties are explored. A special emphasis is placed on SN 1987a which provides a unique opportunity to learn the connection between the star that exploded (whose name we know) and the remnant that will develop in our lifetimes.
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Weiler, Kurt W., and Richard A. Sramek. "Supernovae and Supernova Remnants." Annual Review of Astronomy and Astrophysics 26, no. 1 (September 1988): 295–341. http://dx.doi.org/10.1146/annurev.aa.26.090188.001455.

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Gomez, H. L., S. A. Eales, and L. Dunne. "Smoking supernovae." International Journal of Astrobiology 6, no. 2 (February 28, 2007): 159–67. http://dx.doi.org/10.1017/s1473550407003552.

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AbstractThe question ‘Are supernovae important sources of dust?’ is a contentious one. Observations with the Infrared Astronomical Satellite (IRAS) and the Infrared Space Observatory (ISO) only detected very small amounts of hot dust in supernova remnants. Here, we review observations of two young Galactic remnants with the Submillimetre Common User Bolometer Array (SCUBA), which imply that large quantities of dust are produced by supernovae. The association of dust with the Cassiopeia A remnant is in question owing to the contamination of foreground material. In this paper, we compare the emission from cold dust with CO emission towards Kepler’s supernova remnant. We detect very little CO at the location of the submillimetre peaks. A comparison of masses from the CO and the dust clouds are made, and we estimate the 3σ upper limit on the gas-to-dust ratios to be in the range 20–60. These results suggest that we cannot yet rule out freshly-formed or swept-up circumstellar dust in Kepler’s supernova remnant.
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Vink, Jacco. "Supernova Remnants: An Introductory Review." Symposium - International Astronomical Union 218 (2004): 57–64. http://dx.doi.org/10.1017/s0074180900180581.

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The two main aspects of supernova remnant research addressed in this review are: I. What is our understanding of the progenitors of the observed remnants, and what have we learned from these remnants about supernova nucleosynthesis? II. Supernova remnants are probably the major source of cosmic rays. What are the recent advances in the observational aspects of cosmic ray acceleration in supernova remnants?
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Falle, S. A. E. G. "Supernova Remnants." International Astronomical Union Colloquium 120 (1989): 152–63. http://dx.doi.org/10.1017/s0252921100023678.

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Abstract.In this review I will concentrate on older remnants, by which I mean those in which radiative cooling is important somewhere and the swept up mass is sufficiently large for the details of the initial explosion not to matter. For such remnants it is the optical emission which is crucial since it allows us to deduce a great deal about the physical state of the emitting gas provided we are careful about how we interprete it. Without discussing any particular remnant in detail, I will consider how large and small scale density variations in the ambient medium affect the appearance and energetics of such remnants.
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Chevalier, R. A. "The Early Evolution of Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 31–42. http://dx.doi.org/10.1017/s0252921100102076.

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AbstractThe density distribution of the supernova ejecta and that of the surrounding medium are the most important parameters for the early evolution of supernova remnants. The distribution of the ejecta depends on the detailed hydrodynamics of the explosion, but the outer parts of a supernova can probably be represented by a steep power law density distribution with radius. Self-similar solutions are especially useful for modeling the interaction of a supernova with its surrounding. The supernova first interacts with mass loss from the progenitor star. Evidence for circumstellar interaction is present in a number of extragalactic supernovae, including SN1987a. The explosions of massive stars probably interact with circumstellar gas for a considerable time while Type Ia supernovae interact more directly with the interstellar medium. X-ray spectroscopy is a good diagnostic for the physical conditions in young supernova remnants and for the composition of the supernova gas.
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Gaensler, B. M., and Simon Johnston. "Do We Expect to See Young Pulsars outside Their Parent Shells?" Publications of the Astronomical Society of Australia 12, no. 1 (April 1995): 76–80. http://dx.doi.org/10.1017/s1323358000020075.

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AbstractA recent study has indicated that a substantial fraction of young pulsars born in supernovae have travelled outside the boundaries of their corresponding shell supernova remnants. A simple model suggests that this should not be the case, implying either that some postulated pulsar/remnant associations are false, or that pulsars are particularly difficult to detect until they have emerged from their remnants.
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Jacovich, Taylor, Daniel Patnaude, Patrick Slane, Carles Badenes, Shiu-Hang Lee, Shigehiro Nagataki, and Dan Milisavljevic. "Doppler Broadening and Line-of-sight Effects in Core-collapse Supernovae and Young Remnants." Astrophysical Journal 951, no. 1 (July 1, 2023): 57. http://dx.doi.org/10.3847/1538-4357/acd0ad.

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Abstract The dynamics and spectral characteristics of supernova ejecta reveal details of the supernova energetics, explosive nucleosynthesis, and evolution of the progenitor. However, in practice, this important diagnostic information is only derived from CCD-resolution X-ray spectra of shock-heated material. If the spectra were to be observed at higher resolution, then important clues to the explosion energetics would be obvious through measurements of bulk Doppler motions and turbulence in the ejecta. Likewise, the unshocked ejecta in supernovae and young remnants are responsible for obscuring the emission from ejecta on the back side of the remnant. In light of these important effects, we present line-of-sight spectral maps of core-collapse supernova remnant models. We explore the bulk Doppler broadening of spectral lines, including line-of-sight effects. We also explore the time-dependent absorption from both shocked and unshocked ejecta. Finally, we discuss how future X-ray missions such as XRISM and Athena will be able to resolve these effects in nearby and extragalactic supernovae and their remnants.
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Green, D. A. "Historical Supernovae and their Remnants." Highlights of Astronomy 12 (2002): 350–53. http://dx.doi.org/10.1017/s1539299600013721.

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AbstractHistorical records are available for nine supernova explosions seen in our Galaxy over the last two millennia. The observations of these ‘historical’ supernovae are very useful for the modern astrophysical interpretation of the remnants of these supernovae. The ages of the remnants of these historical supernovae are definitively known, which greatly aids understanding of the nature of the remnants. Also, the fact that the parent supernova was seen implies that it was relatively nearby in the Galaxy, giving further constraints on the distance, and hence other properties of their remnants. Here I briefly review the historical supernovae in our Galaxy, in the context of our understanding of their remnants from modern observations.
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Wang, Zhenru. "Historical Supernovae and Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 323–31. http://dx.doi.org/10.1017/s0252921100008174.

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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.
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Dissertations / Theses on the topic "Supernova remnants"

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Graham, J. R. "Dust in supernovae and supernova remnants." Thesis, Imperial College London, 1985. http://hdl.handle.net/10044/1/37710.

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Misanovic, Zdenka. "Search for young galactic supernova remnants." Thesis, The University of Sydney, 2001. http://hdl.handle.net/2123/795.

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A sample of 9 small-diameter radio sources has been selected from the Molonglo Galactic Plane Survey (MGPS) and observed with the Australia Telescope Compact Array (ATCA) in the radio recombination line (RRL) at 5 GHz, in a search for young Galactic SNRs. Since the RRL emission is an unambiguous indicator of a thermal source, this method has been used to eliminate HII regions from the selected sample. In addition, the IRAS and MSX infrared data and spectral index measurements have been combined with the RRL studies to distinguish thermal and non-thermal sources in the selected sample. One source (G282.8-1.2) is identified here as a possible new young Galactic supernova remnant, based on its relatively weak infrared emission, steep radio spectrum and possible x-ray emission. However, the ATCA data are inconclusive and further studies are needed to confirm this result. Radio recombination line emission (H107 alpha) has been detected in 3 of the selected sources, eliminating them from the sample of SNR candidates. In addition, the parameters of the RRL emission from the identified HII regions have been used to estimate their properties. The RRL data are inconclusive for the remaining low brightness, extended sources in the sample. However, some of these sources are likely to be thermal HII regions according to the infrared and spectral index data. The selected method for distinguishing thermal and non-thermal Galactic radio sources seems promising. The selected ATCA configuration was appropriate for imaging relatively bright, compact sources, but a slightly modified observing technique is needed to successfully image low surface brightness, extended sources.
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Misanovic, Zdenka. "A search for young galactic supernova remnants." University of Sydney. Physics, 2001. http://hdl.handle.net/2123/795.

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A sample of 9 small-diameter radio sources has been selected from the Molonglo Galactic Plane Survey (MGPS) and observed with the Australia Telescope Compact Array (ATCA) in the radio recombination line (RRL) at 5 GHz, in a search for young Galactic SNRs. Since the RRL emission is an unambiguous indicator of a thermal source, this method has been used to eliminate HII regions from the selected sample. In addition, the IRAS and MSX infrared data and spectral index measurements have been combined with the RRL studies to distinguish thermal and non-thermal sources in the selected sample. One source (G282.8-1.2) is identified here as a possible new young Galactic supernova remnant, based on its relatively weak infrared emission, steep radio spectrum and possible x-ray emission. However, the ATCA data are inconclusive and further studies are needed to confirm this result. Radio recombination line emission (H107 alpha) has been detected in 3 of the selected sources, eliminating them from the sample of SNR candidates. In addition, the parameters of the RRL emission from the identified HII regions have been used to estimate their properties. The RRL data are inconclusive for the remaining low brightness, extended sources in the sample. However, some of these sources are likely to be thermal HII regions according to the infrared and spectral index data. The selected method for distinguishing thermal and non-thermal Galactic radio sources seems promising. The selected ATCA configuration was appropriate for imaging relatively bright, compact sources, but a slightly modified observing technique is needed to successfully image low surface brightness, extended sources.
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Arthur, Sarah Jane. "Supernova remnants in inhomogeneous media." Thesis, University of Leeds, 1991. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.293739.

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Kilpatrick, Charles Donald, and Charles Donald Kilpatrick. "New Observational Insight on Shock Interactions Toward Supernovae and Supernova Remnants." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621574.

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Supernovae (SNe) are energetic explosions that signal the end of a star's life. These events and the supernova remnants (SNRs) they leave behind play a central role in stellar feedback by adding energy and momentum and metals to the interstellar medium (ISM). Emission associated with these feedback processes, especially atomic and molecular line emission as well as thermal and nonthermal continuum emission is known to be enhanced in regions of high density, such as dense circumstellar matter (CSM) around SNe and molecular clouds (MCs). In this thesis, I begin with a brief overview of the physics of SN shocks in Chapter 1, focusing on a foundation for studying pan-chromatic signatures of interactions between SNe and dense environments. In Chapter 2, I examine an unusual SN with signatures of CSM interaction in the form of narrow lines of hydrogen (Type IIn) and thermal continuum emission. This SN appears to belong to a class of Type Ia SNe that shares spectroscopic features with Type IIn SNe. I discuss the difficulties of decomposing spectra in a regime where interaction occurs between SN ejecta and CSM, potentially confusing the underlying SN type. This is followed by a discussion of rebrightening that occurred at late-time in 𝐵 and 𝑉 band photometry of this SN, possibly associated with clumpy or dense CSM at large distances from the progenitor. In Chapter 3, I examine synchrotron emission from Cassiopeia A, observed in the 𝐾ₛ band over multiple epochs. The synchrotron emission is generally diffuse over the remnant, but there is one location in the southwest portion of the remnant where it appears to be enhanced and entrained as knots of emission in the SNR ejecta. I evaluate whether the 𝐾ₛ band knots are dominated by synchrotron emission by comparing them to other infrared and radio imaging that is known to be dominated by synchrotron emission. Concluding that they are likely synchrotron-emitting knots, I measure the magnetic field strength and electron density required for their evolution over the ~ 10 yr baseline they were observed and find 𝐵 ≈ 1.3-5.8 mG and 𝑛ₑ≈ 1,000-15,000 cm⁻³. The magnetic field strengths appear enhanced beyond values required by the adiabatic strong shock limit, arguing in favor of other forms of magnetic field amplification in the shock. In Chapter 4, I again discuss Cassiopeia A and interaction between the remnant and nearby MCs as seen at mid-infrared and millimeter wavelengths. I report detection of a SNR-MC interaction and analyze its signatures in broadened molecular lines. I extend this analysis in Chapter 5 to a large survey for SNR-MC interactions in the ¹²CO 𝐽=2-1 line. Although broadened ¹²CO 𝐽=2-1 line emission should be detectable toward virtually all SNR-MC interactions, I find relatively few examples; therefore, the number of interactions is low. This result favors mechanisms other than supernova feedback as the basic trigger for star formation. In addition, I find no significant association between TeV gamma-ray sources and MC interactions, contrary to predictions that SNR-MC interfaces are the primary venues for cosmic ray acceleration. I end this dissertation in Chapter 6 with a brief summary of my results and two extensions of this work: examining the late-time radio light curves of CSM-interacting SNe for signatures of radio synchrotron emission and dense or clumpy CSM at large distances from the progenitor and re-observing SNR-MC interactions in ¹²CO 𝐽=3-2 in order to verify the presence of shock-heated molecular gas and perform a census on the densities and temperatures of post-shock molecular gas.
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Hwang, Una. "X-ray studies of supernova remnants." Thesis, Massachusetts Institute of Technology, 1994. http://hdl.handle.net/1721.1/26858.

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Schaudel, Daniel. "X-ray Properties of Galactic Supernova Remnants." Diss., lmu, 2003. http://nbn-resolving.de/urn:nbn:de:bvb:19-11097.

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Jones, Laurence Richard. "X-ray emission from galactic supernova remnants." Thesis, University of Leicester, 1986. http://hdl.handle.net/2381/35703.

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X-ray emission from galactic supernova remnants X-ray images and spectra are used to determine the structure and physical conditions of shock heated interstellar gas and stellar ejecta within three galactic supernova remnants (SNRs). Parameters describing the initial supernova explosions (total energy, ejected mass) and ambient interstellar medium (density, homogeneity) are then derived. The interior density of the "middle-aged" SNR W44 is found to be fairly uniform, and inconsistent with the standard Sedov model, but similar to that predicted by models in which thermal conduction and/or heating and evaporation of engulfed, cold, interstellar clouds are important. This expanding bubble of hot, high pressure gas is likely to be an example of the formation of the hot component of interstellar medium, as detected in the vicinity of the Sun. In addition, it is likely that the SNR has collided with a nearby dense molecular cloud. The SNR W49B is found to be probably the remnant of a Type II supernova which occurred in a relatively dense medium 2000-5000 years ago. The abundance of hot iron in the ejecta is consistent with the cosmic value. The youngest SNR studied, SN1006, is found to be the remnant of a Type I supernova which occurred in a region of low, but fairly uniform (to within a factor of 2), interstellar density. Emission from reverse shocked ejecta may be most prominent in a limited area of the SNR, explaining a discrepancy between previous X-ray spectra of the remnant. A common result in all three SNRs is the detection of hot gas at their centres; the likely effects of a reverse shock and thermal conduction within SNRs are emphasized.
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Mogawana, Orapeleng. "Meshless hydrodynamic simulations of young supernova remnants." Master's thesis, Faculty of Science, 2020. http://hdl.handle.net/11427/32810.

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The majority of massive stars end their lives by ejecting their outer envelopes in a corecollapse supernova explosion. The collision of their ejecta with the surrounding circumstellar medium results in the formation of supernova remnants that have been detected at all wavelengths, from radio to gamma-rays. For several dozen supernova remnants, very-long-baseline radio interferometers have spatially resolved the interaction region and directly measured the expansion rates of the shocked gas; many show evidence of the interaction of supernova ejecta with the dense slow winds characteristic of the red supergiant progenitors. Understanding the dynamics and morphology of the interaction region, particularly in young supernova remnants leads to estimates of the total mass of the circumstellar medium, as well as its density distribution around the star given the value of the wind velocity. Here we studied the interaction of the supernova ejecta with different circumstellar environments to investigate the hydrodynamic evolution of young supernova remnants in the SedovTaylor phase. We used the massively parallel, multi-physics magneto-hydrodynamics (MHD) and gravity code, GIZMO, for our simulations. We chose GIZMO for its flexibility in allowing the user to choose different methods to solve the fluid equations, i.e., new Lagrangian Godunovtype schemes, e.g., Meshless Finite Volume (MFV) and Meshless Finite Mass (MFM), as well as various flavors of smoothed particle hydrodynamics (SPH), or Eulerian fixed-grid schemes. Since the majority of previous studies used the latter, we focused on an extensive comparison of all the meshless methods in solving the Sedov-Taylor blastwave test, a problem for which there is an exact solution. For our given compute resources, we found the parameters (e.g., smoothing length, number of neighbours, artificial viscosity, and particle resolution) for each meshless method that gave the best agreement with the exact solution. We then carried out 2D and 3D simulations of the hydrodynamic interaction of the supernova ejecta with varying density profiles assumed for the circumstellar medium, namely: a 1/r 2 density profile, for a typical, spherically symmetric red supergiant stellar wind, and an axisymmetric torus profile, inspired by the observation of a dense, dusty torus of the circumstellar material around the red supergiant, WOH G64 (Ohnaka et al., 2008). Radially assembled Hierarchical Equal Area isoLatitude Pixelization (HEALPix) shells were used to set-up the initial density and velocity profiles for the ejecta, which is marked by a flat inner core and a steeply declining outer edge. The Weighted Voronoi Tessellation code was used to produce the 1/r 2 and axisymmetric torus density distributions. We showed that the growth of Richtmyer-Meshkov instabilities in the 2D and 3D 1/r 2 profiles are visible as early as 20 yrs into the evolution of the remnant and become increasingly unstable up to 100 yr. While 2D simulations of 1/r 2 profiles show the presence of the Richtmyer-Meshkov instabilities in the hot shell of a contact discontinuity, in 3D we see large bubbles and filamentary structure of the instabilities. Our results for the numerical approaches to simulating the systems for the 1/r 2 density cases were broadly consistent with previous studies in the literature where stationary grids were used. Two scenarios with different torus-cavity density contrasts were considered in which we found that the instability rolls along the half-opening angle takes ∼ 40 yr to develop in the axisymmetric torus with smooth density drop, whereas the axisymmetric torus with steep density drop does not develop any instability rolls up to the end of the simulation. We concluded with a discussion of the implications of our models for the morphology of supernova remnants and their expected levels of multi-wavelength emission.
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Dyer, Kristy Kathleen. "Thermal and Non-Thermal Emission in Supernova Remnants." NCSU, 2001. http://www.lib.ncsu.edu/theses/available/etd-20010806-162918.

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Supernova remnants present an excellent opportunity to study the shockacceleration of relativistic particles. X-ray synchrotron emission fromrelativistic electrons should contain important information, butextracting it requires advances in models and observations. I present thefirst test of sophisticated synchrotron models against high resolutionobservations on SN 1006, the first and best example of synchrotron X-rayemission, which has been well observed at radio, X-ray and gamma-raywavelengths. Synchrotron emission can be limited at the highest energies by finite age,radiative losses or electron escape. Earlier calculations suggested thatSN 1006 was escape limited. I adapted an escape-limited synchrotron modelfor XSPEC, and demonstrated that it can account for the dominantlynonthermal integrated spectrum of SN 1006 observed by ASCA-GIS and RXTEwhile constraining the values of the maximum electron energy and otherparameters. Combined with TeV observations, the fits give a mean postshockmagnetic field strength of 9 microgauss and 0.7% of the supernova energyin relativistic electrons. Simultaneous thermal fits gave abundances farabove solar, as might be expected for ejecta but had not previously beenobserved. I created subsets of the escape-limited model to fit spatially resolvedASCA SIS observations. I found only small differences between thenortheast and southwest limbs. A limit of less than 9% was placed on theamount of nonthermal flux elsewhere in the remnant. Important findingsinclude the possibility that rolloff frequency may change across theremnant face, and ruling out cylindrical symmetry for SN 1006 along aNW/SE axis. These models have implications far beyond SN 1006. The only previousmodel available to describe X-ray synchrotron emission was a powerlaw.These new models are superior to powerlaws both for their robustconstraints and because they shed physical insight on the accelerationmechanism. As new instruments increase our spatial and spectral resolutionI predict many more remnants will be found with varying amounts of X-raysynchrotron emission, hidden along with thermal lines and continuum. Theability to separate thermal and nonthermal emission is essential tounderstanding both nonthermal emission as well as the thermal component.

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Books on the topic "Supernova remnants"

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Efe, Yazgan, and Ankay Askin, eds. Neutron stars, supernovae and supernova remnants. New York: Nova Science Publishers, 2007.

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Colloquium, International Astronomical Union. Supernova remnants and the interstellar medium. Cambridge: Cambridge University Press, 1988.

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Colloquium, International Astronomical Union. Supernovae and supernova remnants: Proceedings International Astronomical Union Colloquium 145, held in Xian, China, May 24-29, 1993. Cambridge: Cambridge University Press, 1996.

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Beijing Workshop on Supernovae and their remnants (1991). Proceedings of Beijing Workshop on Supernovae and their remnants: Beijing, China, 29 June-3 July 1991. Beijing, People's Republic of China: Published and distributed by International Academic Publishers, 1992.

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Ghavamian, Parviz. New high-energy results on supernova remnants and pulsar wind nebulae. Oxford: Published for the Committee on Space Research [by] Elsevier, 2008.

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Wolfgang, Kundt, ed. Supernova shells and their birth events: Proceedings of a workshop held at the Physikzentrum Bad Honnef, March 7-11, 1988. Berlin: Springer-Verlag, 1988.

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Vink, Jacco. Physics and Evolution of Supernova Remnants. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-55231-2.

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Green, D. A. A catalogue of galactic supernova remnants. [S.l: s.n.], 1987.

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C, Rakowski, Chatterjee S, and COSPAR Scientific Assembly, eds. Young neutron stars and supernova remnants. Kidlington, Oxford, U.K: Published for the Committee on Space Research [by] Elsevier, 2005.

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Lessard, Rodney W. Observations of TeV gamma-rays from supernova remnants. Dublin: University College Dublin, 1996.

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Book chapters on the topic "Supernova remnants"

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Tsunemi, Hiroshi. "Supernovae and supernova remnants." In The Century of Space Science, 937–60. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0320-9_41.

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Montmerle, Thierry. "Supernova Remnants." In Encyclopedia of Astrobiology, 1640–41. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1547.

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Reynolds, Stephen P. "Supernova Remnants." In Astronomy and Astrophysics Library, 439–79. New York, NY: Springer New York, 1988. http://dx.doi.org/10.1007/978-1-4612-3936-9_10.

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Lang, Kenneth R. "Supernova Remnants." In Astrophysical Data, 709–30. New York, NY: Springer US, 1992. http://dx.doi.org/10.1007/978-1-4684-0640-5_27.

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Branch, David, and J. Craig Wheeler. "Supernova Remnants." In Astronomy and Astrophysics Library, 115–34. Berlin, Heidelberg: Springer Berlin Heidelberg, 2017. http://dx.doi.org/10.1007/978-3-662-55054-0_7.

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Bandiera, R. "Plerionic Supernova Remnants." In Physical Processes in Hot Cosmic Plasmas, 325–40. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0545-0_19.

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Aschenbach, B. "Galactic Supernova Remnants." In X-Ray Astronomy in the Exosat Era, 447–65. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5448-9_64.

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Long, Knox S. "Extragalactic Supernova Remnants." In X-Ray Astronomy in the Exosat Era, 531–48. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5448-9_75.

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Danziger, I. J. "Optical Supernova Remnants." In Nucleosynthesis and Its Implications on Nuclear and Particle Physics, 233–42. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4578-4_26.

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Strom, Richard G. "Supernova Remnants II: Shells." In Neutron Stars and Their Birth Events, 263–73. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0515-3_21.

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Conference papers on the topic "Supernova remnants"

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Costantini, M. L. "Neutrinos from Supernovas and Supernova Remnants." In IFAE 2005: XVII Incontri de Fisica delle Alte Energie; 17th Italian Meeting on High Energy Physics. AIP, 2005. http://dx.doi.org/10.1063/1.2125656.

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Chevalier, Roger A. "Supernovae and supernova remnants at high energies." In High−Energy Astrophysics in the 21st Century. AIP, 1990. http://dx.doi.org/10.1063/1.39667.

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Safi-Harb, Samar. "Plerionic supernova remnants." In HIGH ENERGY GAMMA-RAY ASTRONOMY: 5th International Meeting on High Energy Gamma-Ray Astronomy. AIP, 2012. http://dx.doi.org/10.1063/1.4772215.

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Slane, Patrick. "Supernova Remnants and GLAST." In THE FIRST GLAST SYMPOSIUM. AIP, 2007. http://dx.doi.org/10.1063/1.2757267.

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Danziger, I. J. "Abundances in supernova remnants." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37990.

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Gomez, Haley. "Dust in supernova remnants." In The Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments. Trieste, Italy: Sissa Medialab, 2014. http://dx.doi.org/10.22323/1.207.0146.

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Kosenko, D., J. Vink, S. Blinnikov, A. Rasmussen, Stefan Immler, and Kurt Weiler. "Exploration of SN Ia remnants in LMC." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803584.

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Kosenko, D., J. Vink, S. Blinnikov, A. Rasmussen, Stefan Immler, and Kurt Weiler. "Exploration of SN Ia remnants in LMC." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.3682923.

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Drury, L. O’C. "Particle acceleration in supernova remnants." In Particle acceleration in cosmic plasmas. AIP, 1992. http://dx.doi.org/10.1063/1.42727.

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O’C Drury, Luke. "Particle acceleration in supernova remnants." In The international symposium on high energy gamma-ray astronomy. AIP, 2001. http://dx.doi.org/10.1063/1.1370781.

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Reports on the topic "Supernova remnants"

1

Moskalenko, I. V. Hadronic Gamma Rays from Supernova Remnants. Office of Scientific and Technical Information (OSTI), June 2007. http://dx.doi.org/10.2172/908759.

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Porter, Troy A., Igor V. Moskalenko, and Andrew W. Strong. Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field. Office of Scientific and Technical Information (OSTI), August 2006. http://dx.doi.org/10.2172/888781.

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Kaya, Mori, and Christopher Fryer. The High Energy X-ray Probe (HEX-P): Galactic PeVatrons, supernova remnants, pulsar wind nebulae and nuclear astrophysics. Office of Scientific and Technical Information (OSTI), July 2023. http://dx.doi.org/10.2172/2375831.

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Pohl, M., Aous A. Abdo, A. Atoyan, Matthew G. Baring, John Francis Beacom, R. Blandford, Y. Butt, et al. Section on Supernova Remnants and Cosmic Rays of the White Paper on the Status and Future of Ground-Based Gamma-Ray Astronomy. Office of Scientific and Technical Information (OSTI), November 2011. http://dx.doi.org/10.2172/1029164.

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Fryer, Christopher Lee. Supernova Remnant Studies. Office of Scientific and Technical Information (OSTI), October 2016. http://dx.doi.org/10.2172/1330642.

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Combi, J. G337.2+0.1: a New X-Ray Supernova Remnant? Office of Scientific and Technical Information (OSTI), January 2005. http://dx.doi.org/10.2172/839664.

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Eriksen, Kristoffer A., Aimee L. Hungerford, Christopher J. Fontes, Christopher L. Fryer, Jennifer L. Donley, and James P. Colgan. Robust Measurement of Iron Plasma Parameters in Tycho's Supernova Remnant. Office of Scientific and Technical Information (OSTI), April 2013. http://dx.doi.org/10.2172/1074571.

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Abdo, A. Observation of Supernova Remnant IC 443 with the Fermi Large Area Telescope. Office of Scientific and Technical Information (OSTI), December 2012. http://dx.doi.org/10.2172/1057406.

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