Journal articles on the topic 'Supernova remnants'
To see the other types of publications on this topic, follow the link: Supernova remnants.
Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles
Consult the top 50 journal articles for your research on the topic 'Supernova remnants.'
Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.
You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.
Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.
1
Kirshner, Robert P. "Supernova Remnants and their Supernovae." International Astronomical Union Colloquium 101 (1988): 1–14. http://dx.doi.org/10.1017/s0252921100102027.
Full textAbstract:
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.
2
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.
Full text
3
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.
Full textAbstract:
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.
4
Vink, Jacco. "Supernova Remnants: An Introductory Review." Symposium - International Astronomical Union 218 (2004): 57–64. http://dx.doi.org/10.1017/s0074180900180581.
Full textAbstract:
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?
5
Falle, S. A. E. G. "Supernova Remnants." International Astronomical Union Colloquium 120 (1989): 152–63. http://dx.doi.org/10.1017/s0252921100023678.
Full textAbstract:
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.
6
Chevalier, R. A. "The Early Evolution of Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 31–42. http://dx.doi.org/10.1017/s0252921100102076.
Full textAbstract:
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.
7
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.
Full textAbstract:
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.
8
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.
Full textAbstract:
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.
9
Green, D. A. "Historical Supernovae and their Remnants." Highlights of Astronomy 12 (2002): 350–53. http://dx.doi.org/10.1017/s1539299600013721.
Full textAbstract:
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.
10
Wang, Zhenru. "Historical Supernovae and Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 323–31. http://dx.doi.org/10.1017/s0252921100008174.
Full textAbstract:
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.
11
Sasaki, Manami. "GALACTIC AND EXTRAGALACTIC SUPERNOVA REMNANTS AS SITES OF PARTICLE ACCELERATION." Acta Polytechnica 53, A (December 18, 2013): 612–16. http://dx.doi.org/10.14311/ap.2013.53.0612.
Full textAbstract:
Supernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into the acceleration of particles to high energies. This paper reviews the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implications for Galactic cosmic ray distribution are discussed.
12
Dwek, Eli. "Infrared Emission from Dust in Supernovae and Supernova Remnants." Symposium - International Astronomical Union 135 (1989): 479–86. http://dx.doi.org/10.1017/s0074180900125471.
Full textAbstract:
The need to replenish the reservoir of interstellar dust grains that are continuously being destroyed in the interstellar medium, and the presence of isotopic anomalies in meteorites, suggest that supernovae may be important sources of interstellar dust. Infrared observations of supernovae or their unmixed ejecta may provide the first direct evidence for newly-formed grains in this environment. The recently discovered supernova, SN 1987A, currently offers the best prospects for observing the actual process of dust formation in a supernova.In contrast, supernova remnants constitute the most important grain destruction mechanism in the galaxy. Interstellar dust swept up by the expanding blast wave is predominantly heated and destroyed by collisions with a shocked x-ray emitting plasma. Infrared observations of remnants can therefore provide valuable information on the interaction between dust particles and a hot gas. This interaction can best be studied in supernova remnants detected with the Infrared Astronomical Satellite (IRAS). This paper reviews what we have learned so far on the subjects of grain formation and destruction by studying the infrared emission from supernovae and supernova remnants.
13
Vink, Jacco. "Supernova remnants and the origin of cosmic rays." Proceedings of the International Astronomical Union 9, S296 (January 2013): 305–14. http://dx.doi.org/10.1017/s1743921313009630.
Full textAbstract:
AbstractSupernova remnants have long been considered to be the dominant sources of Galactic cosmic rays. For a long time the prime evidence consisted of radio synchrotron radiation from supernova remnants, indicating the presence of electrons with energies of several GeV. However, in order to explain the cosmic ray energy density and spectrum in the Galaxy supernova remnant should use 10% of the explosion energy to accelerate particles, and about 99% of the accelerated particles should be protons and other atomic nuclei.Over the last decade a lot of progress has been made in providing evidence that supernova remnant can accelerate protons to very high energies. The evidence consists of, among others, X-ray synchrotron radiation from narrow regions close to supernova remnant shock fronts, indicating the presence of 10-100 TeV electrons, and providing evidence for amplified magnetic fields, gamma-ray emission from both young and mature supernova remnants. The high magnetic fields indicate that the condition for accelerating protons to >1015 eV are there, whereas the gamma-ray emission from some mature remnants indicate that protons have been accelerated.
14
Lorimer, D. R., and R. Ramachandran. "Puzzling Pulsars and Supernova Remnants." International Astronomical Union Colloquium 177 (2000): 491–92. http://dx.doi.org/10.1017/s0252921100060383.
Full textAbstract:
AbstractThe fact that the majority of the youngest radio pulsars are surrounded by expanding supernova remnants is strong evidence that neutron stars are produced in the supernovae of massive stars. In many cases, the pulsar appears significantly offset from the geometric centre of the supernova remnant, indicating that the neutron star has moved away from the site of the explosion with a substantial space velocity since birth. Here we show that the these offsets show an overwhelming preference for one sign in terms of Galactic longitude, a result that has important implications for the number of genuine associations. The origin of this statistically significant effect may lie in a differential Galactic rotational velocity between stars and gas in the interstellar medium.
15
Chiotellis, A., D. Kosenko, K. M. Schure, and J. Vink. "Progenitor's Signatures in Type Ia Supernova Remnants." Proceedings of the International Astronomical Union 7, S281 (July 2011): 331–34. http://dx.doi.org/10.1017/s1743921312015311.
Full textAbstract:
AbstractThe remnants of Type Ia supernovae (SNe Ia) can provide important clues about their progenitor histories. We discuss two well-observed supernova remnants (SNRs) that are believed to have resulted from SNe Ia, and use various tools to shed light on the possible progenitor histories. We find that Kepler's SNR is consistent with a symbiotic binary progenitor consisting of a white dwarf and an AGB star. Our hydrosimulations can reproduce the observed kinematic and morphological properties. For Tycho's remnant we use the characteristics of the X-ray spectrum and kinematics to show that the ejecta has likely interacted with dense circumstellar gas.
16
Badenes, Carles, Eduardo Bravo, and Kazimierz J. Borkowski. "Thermonuclear Supernova Explosions and Their Remnants: The Case of Tycho." International Astronomical Union Colloquium 192 (2005): 233–38. http://dx.doi.org/10.1017/s0252921100009246.
Full textAbstract:
SummaryWe propose to use the thermal X-ray emission from young supernova remnants (SNRs) originated in Type Ia supernovae (SNe) to extract relevant information concerning the explosion mechanism. We focus on the differences between numerical 1D and 3D explosion calculations, and the impact that these differences could have on the modeling of young SNRs. We use the remnant of the Tycho supernova (SN 1572) as a test case to compare with our predictions, discussing the observational features that allow to accept or discard a given model.
17
Arbutina, B., D. Urošević, and B. Vukotić. "High supernova rate and enhanced star-formation triggered in M81-M82 encounter." Proceedings of the International Astronomical Union 2, S237 (August 2006): 391. http://dx.doi.org/10.1017/s1743921307001792.
Full textAbstract:
It is a general belief that the starburst activity of a nearby galaxy M82 was triggered in a close encounter with its massive companion M81, a few tens of million years ago. Despite the lack of supernovae observed, multiwavelength radio observations of M82 discovered a considerable number of compact supernova remnant candidates. We use these remnants to estimate the supernova rate (SNR) and the enhanced star-formation (SFR) rate in M82, and compare them with rates in normal galaxies.
18
McKee, Christopher F. "Supernova Remnant Shocks in an Inhomogeneous Interstellar Medium." International Astronomical Union Colloquium 101 (1988): 205–22. http://dx.doi.org/10.1017/s0252921100102386.
Full textAbstract:
AbstractThe inhomogeneity of the interstellar medium (ISM) has a profound effect on the propagation of the interstellar shock generated by a supernova and on the appearance of the resulting supernova remnant (SNR). Low mass supernovae produce remnants that interact with the “pristine” ISM, which has density inhomogeneities (clouds) on a wide range of scales. The shock compresses and accelerates the clouds it encounters; inside the blast wave, the clouds are hydrodynamically unstable, and mass is injected from the clouds into the intercloud medium. Embedded clouds interact thermally with the shock also, adding mass to the hot intercloud medium via thermal evaporation or subtracting it via condensation and thermal instability. Mass injection into the hot intercloud medium, whether dynamical or thermal, leads to infrared emission as dust mixes with the hot gas and is thermally sputtered. The remnants of massive supernovae interact primarily with circumstellar matter and with interstellar material which has been processed by the ionizing radiation and wind of the progenitor star. After passing through any circumstellar material which may be present, the shock encounters a cavity which tends to “muffle” the SNR. The remnants of massive supernovae therefore tell us more about the late stages of the evolution of massive stars than about the ISM.
19
Fryer, Chris L. "Compact Remnant Constraints on the Core-Collapse Engine." Proceedings of the International Astronomical Union 16, S363 (June 2020): 19–32. http://dx.doi.org/10.1017/s1743921322000527.
Full textAbstract:
AbstractThe convection-enhanced neutrino-driven supernova engine’s success in explaining a myriad of supernova properties has set it as the standard engine behind supernova. However, due to the success of rotationally-powered engines in explaining astrophysical transients like gamma-ray bursts, these engines have been revived as possible drivers of normal supernovae, competing with this standard engine. In this paper, these competing engines, and the constraints placed by compact remnant observations on these engines, are reviewed. We find that, with these constraints, such rotationally-powered engines can explain less than 1% of the current supernova remnants. In addition, we find that the remnant mass distribution can be used to constrain properties of the convection-enhanced neutrino-driven engine, helping astronomers understand the nature of convection in this engine.
20
Reynolds, Stephen P. "Small-Scale Structure in Young Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 331–34. http://dx.doi.org/10.1017/s0252921100102593.
Full textAbstract:
AbstractRecent VLA observations of the shell supernova remnant SN 1006 AD (Reynolds and Gilmore 1986) and the Crablike remnant 3C 58 (SN 1181 AD?; Reynolds and Aller 1987) show features at high resolution that contain information on details of particle acceleration and transport in the remnants. Thin arcs at the edge of SN 1006 require time-variable particle acceleration and/or magnetic field amplification. Filaments in 3C 58 probably result from interaction of pulsar-generated relativistic fluid with filaments of thermal gas formed early in the remnant’s life by cooling or dynamical instabilities. Their sharp edges imply efficient scattering by Alfvén waves; as much as 1% of the large-scale magnetic energy density may be in magnetic turbulence on length scales of 1011 cm.
21
Walker, A., and W. J. Zealey. "Searching for Supernova Remnants." Publications of the Astronomical Society of Australia 15, no. 1 (1998): 79–82. http://dx.doi.org/10.1071/as98079.
Full textAbstract:
AbstractThe UKST/AAO Galactic Plane Hα Survey has the potential to discover many new objects not visible on red plates taken in past surveys. Recent radio surveys have identified large numbers of new supernova remnants, very few of which have been optically identified. Here we will discuss our plans to use this survey to search for optical emission from both new and known supernova remnants. Observations of these objects in the optical and radio wavelengths will reveal important information about the physical and chemical properties of supernova remnants, and their role in the evolution of the galaxy. We also present a composite image of a newly discovered Hα shell around the Coalsack, named the Coalsack Loop. This object has been detected in radio emission and may represent the remains of an old supernova remnant.
22
Chevalier, Roger A. "Compact Objects in Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 399–406. http://dx.doi.org/10.1017/s0252921100008253.
Full textAbstract:
Core collapse in very massive stars can lead to a central black hole that swallows the rest of the star and in less massive stars to a central neutron star and explosion. There is probably an intermediate mass range that gives an explosion and a central black hole; supernova remnants with no observable central object are candidates. The association of pulsars with Type II supernovae gives an estimate of the pulsar power to be expected in a supernova, but the uncertainty in the initial pulsar periods gives a wide range in possible powers. The relativistic wind bubble model for the Crab Nebula has steadily developed and there are now predictions regarding particle acceleration in the optical wisps. The bubble model with expansion into supernova gas can also be applied to other young pulsar nebulae.
23
Ballet, J. "Supernova remnants." EAS Publications Series 7 (2003): 217. http://dx.doi.org/10.1051/eas:2003042.
Full text
24
Jane Arthur, S. "Supernova explosions in stellar wind bubbles." Symposium - International Astronomical Union 148 (1991): 331–33. http://dx.doi.org/10.1017/s0074180900200715.
Full textAbstract:
Type II supernovae play a major role in the dynamics of the interstellar medium. The interstellar medium in which such supernovae evolve is often considerably modified by the strong stellar winds both from the progenitor and other nearby stars. The result is that the appearance and energetics of the remnants can be very different from that of remnants in a uniform medium. In this paper we will consider the evolution of supernova remnants in stellar wind bubbles including the effect of departures from spherical symmetry. The aim is to understand both the appearance of such remnants and their effect on the overall energetics of the interstellar medium.
25
Fransson, Claes. "The Early Evolution of Supernova Remnants." International Astronomical Union Colloquium 89 (1986): 141–65. http://dx.doi.org/10.1017/s0252921100086061.
Full textAbstract:
In his review in 1972 Woltjer [1] divided the evolution of supernova remnants into three different phases, the free expansion phase, the adiabatic Sedov phase and the radiative phase, when cooling of the gas becomes important. The first of these was only briefly discussed and little connection between the supernova explosion and the remnant phase was made. The reason for this is also easy to understand in view of the difficulty of determining the type of explosion even for well-known, young remnants like Cas A, Tycho, Kepler and the Crab remnant.This situation has changed considerably during the last five years or so, mainly due to observations with new instruments like VLA, IUE and Einstein. With these, as well as large optical and infrared telescopes, the information about the supernova explosion and the early evolution of the supernova remnant has increased dramatically, and a more or less new picture of the explosion has emerged. Instead of a free expansion into a virtual vacuum, with few observational consequences, the supernova undergoes a complex interaction with its immediate surroundings, with a wealth of observational information. In this stage both the structure of the supernova ejecta and the circumstellar medium is crucial for the observational properties. Perhaps, the most interesting aspect of it is that we in this way can bridge the gap between the supernova explosion and the remnant stage.
26
Milisavljevic, Dan, and Robert A. Fesen. "Autopsy of the Supernova Remnant Cassiopeia A." Proceedings of the International Astronomical Union 9, S296 (January 2013): 155–59. http://dx.doi.org/10.1017/s1743921313009393.
Full textAbstract:
AbstractThree-dimensional kinematic reconstructions of optically emitting ejecta in the young Galactic supernova remnant Cassiopeia A (Cas A) are discussed. The reconstructions encompass the remnant's faint outlying ejecta knots, including the exceptionally high-velocity NE and SW streams of debris often referred to as ‘jets’. The bulk of Cas A's ejecta are arranged in several circular rings with diameters between approximately 30″ (0.5 pc) and 2′ (2 pc). We suggest that similar large-scale ejecta rings may be a common phenomenon of young core-collapse remnants and may explain lumpy emission line profile substructure sometimes observed in spectra of extragalactic core-collapse supernovae years after explosion. A likely origin for these large ejecta rings is post-explosion input of energy from plumes of radioactive 56Ni-rich ejecta that rise, expand, and compress non-radioactive material to form bubble-like structures.
27
Lopez, Laura A. "What Shapes Supernova Remnants?" Proceedings of the International Astronomical Union 9, S296 (January 2013): 239–44. http://dx.doi.org/10.1017/s1743921313009538.
Full textAbstract:
AbstractEvidence has mounted that Type Ia and core-collapse (CC) supernovae (SNe) can have substantial deviations from spherical symmetry; one such piece of evidence is the complex morphologies of supernova remnants (SNRs). However, the relative role of the explosion geometry and the environment in shaping SNRs remains an outstanding question. Recently, we have developed techniques to quantify the morphologies of SNRs, and we have applied these methods to the extensive X-ray and infrared archival images available of Milky Way and Magellanic Cloud SNRs. In this proceeding, we highlight some results from these studies, with particular emphasis on SNR asymmetries and whether they arise from “nature” or “nurture”.
28
Asvarov, Abdul I. "“Hypernova” Radio Remnants." Symposium - International Astronomical Union 214 (2003): 137–40. http://dx.doi.org/10.1017/s0074180900194288.
Full textAbstract:
If recently discovered hypernova events are intrinsically energetic explosions of stars with a kinetic energy output of EK ≳ 1052 ergs than they can produce very large diameter (up to 500 pc) nonthermal radio shells. The properties of such shells are modelled and compared with the observational data on the large diameter supernova remnants (SNRs). One real candidate for the hypernova remnant is found. This is the supernova remnant N7793-S26 in the galaxy NGC 7793 (Pannuti et al. 2002).
29
Velusamy, T. "Guest Stars: Historical Supernovae and Remnants." International Astronomical Union Colloquium 91 (1987): 265–70. http://dx.doi.org/10.1017/s0252921100106153.
Full textAbstract:
Supernova explosions occur in massive stars in their final stages of stellar evolution. The explosion leaves behind a collapsed object, usually a neutron star observable as a pulsar, and an expanding outer envelope of the star observable as a supernova remnant (SNR). Because of the large amount of energy in the range of 1050 −1052 ergs released in the explosion, the energy radiated by the exploded star is equivalent to that of millions of normal stars. Thus a "new star" seems to appear and is easily visible to the naked eye for several months. Astronomers have estimated that in our galaxy such supernova explosions occur once about every 50 years. In ancient times, the occurrence of supernova might have been noticed as appearance of a bright new star which faded away into obscruity after a few months. Thus the ‘guest stars’ in the ancient records are indeed possible occurrences of supernova explosions in the galaxy. The guest star of 1054 A.D., well recorded by Chinese and Japanese astronomers is the best known historic supernova (Brecher et al. 1983; and references therein); today its remnants the Crab Nebula and the pulsar are observable over the entire electromagnetic spectrum from radio to γ-rays. Of the 150 SNRs known in our galaxy, only about 10 have been identified with guest stars of historical supernovae.
30
Weinberger, Christoph, Roland Diehl, Moritz M. M. Pleintinger, Thomas Siegert, and Jochen Greiner. "44Ti ejecta in young supernova remnants." Astronomy & Astrophysics 638 (June 2020): A83. http://dx.doi.org/10.1051/0004-6361/202037536.
Full textAbstract:
Context. Tracing unstable isotopes produced in supernova nucleosynthesis provides a direct diagnostic of supernova explosion physics. Theoretical models predict an extensive variety of scenarios, which can be constrained through observations of the abundant isotopes 56Ni and 44Ti. Direct evidence of the latter was previously found only in two core-collapse supernova events, and appears to be absent in thermonuclear supernovae. Aims. We aim to to constrain the supernova progenitor types of Cassiopeia A, SN 1987A, Vela Jr., G1.9+0.3, SN1572, and SN1604 through their 44Ti ejecta masses and explosion kinematics. Methods. We analyzed INTEGRAL/SPI observations of the candidate sources utilizing an empirically motivated high-precision background model. We analyzed the three dominant spectroscopically resolved de-excitation lines at 68, 78, and 1157 keV emitted in the decay chain of 44Ti→44Sc→44Ca. The fluxes allow the determination of the production yields of 44Ti. Remnant kinematics were obtained from the Doppler characteristics of the lines. Results. We find a significant signal for Cassiopeia A in all three lines with a combined significance of 5.4σ. The fluxes are (3.3 ± 0.9) × 10−5 ph cm−2 s−1, and (4.2 ± 1.0) × 10−5 ph cm−2 s−1 for the 44Ti and 44Sc decay, respectively. This corresponds to a mass of (2.4 ± 0.7) × 10−4 M⊙ and (3.1 ± 0.8) × 10−4 M⊙, respectively. We obtain higher fluxes for 44Ti with our analysis of Cassiopeia A than were obtained in previous analyses. We discuss potential differences. We interpret the line width from Doppler broadening as expansion velocity of (6400 ± 1900) km s−1. We do not find any significant signal for any other candidate sources. Conclusions. We obtain a high 44Ti ejecta mass for Cassiopeia A that is in disagreement with ejecta yields from symmetric 2D models. Upper limits for the other core-collapse supernovae are in agreement with model predictions and previous studies. The upper limits we find for the three thermonuclear supernovae (G1.9+0.3, SN1572 and SN1604) consistently exclude the double detonation and pure helium deflagration models as progenitors.
31
Ruffini, Nicholas J., and Andrew R. Casey. "A hyper-runaway white dwarf in Gaia DR2 as a Type Iax supernova primary remnant candidate." Monthly Notices of the Royal Astronomical Society 489, no. 1 (August 9, 2019): 420–26. http://dx.doi.org/10.1093/mnras/stz2176.
Full textAbstract:
ABSTRACT Observations of stellar remnants linked to Type Ia and Type Iax supernovae are necessary to fully understand their progenitors. Multiple progenitor scenarios predict a population of kicked donor remnants and partially burnt primary remnants, both moving with relatively high velocity. But only a handful of examples consistent with these two predicted populations have been observed. Here we report the likely first known example of an unbound white dwarf that is consistent with being the fully cooled primary remnant to a Type Iax supernova. The candidate, LP 93-21, is travelling with a galactocentric velocity of $v_{\textrm {gal}} \simeq 605\, {\rm km}\, {\rm s}^{-1}$, and is gravitationally unbound to the Milky Way. We rule out an extragalactic origin. The Type Iax supernova ejection scenario is consistent with its peculiar unbound trajectory, given anomalous elemental abundances are detected in its photosphere via spectroscopic follow-up. This discovery reflects recent models that suggest stellar ejections likely occur often. Unfortunately the intrinsic faintness of white dwarfs, and the uncertainty associated with their direct progenitor systems, makes it difficult to detect and confirm such donors.
32
Petre, R. "Supernova Remnants in the Magellanic Clouds." Symposium - International Astronomical Union 190 (1999): 74–77. http://dx.doi.org/10.1017/s0074180900117425.
Full textAbstract:
Over the past decade, substantial progress has been made in understanding the properties of Magellanic Cloud supernova remnants and their role in the ISM. Among the notable results are the “typing” of progenitors via the X-ray spectra of their remnants, the use of X-ray spectra to measure ISM abundances, and the discovery of remnants with unique properties. I summarize recent studies of MC SNRs, and describe how a refined understanding of the SNR population requires consideration of the unique attributes of each remnant.
33
Aschenbach, B. "Morphology and Physics of Supernova Remnants." Highlights of Astronomy 9 (1992): 223–28. http://dx.doi.org/10.1017/s1539299600008960.
Full textAbstract:
AbstractSpectrally resolved X-ray images of the Cygnus Loop and the Vela supernova remnant have been obtained during the ROSAT all sky survey. The remnants show highly filamentary brightness distributions. Temperatures between 1·106 K and 10·106 K have been measured. Both remnants show significant deviation from thermal pressure equilibrium. The highest pressure excursions of up to a factor of 50 are associated with the X-ray brightest filaments. Pressure variations are expected for very recently shocked clouds, on a smaller scale though. In a limited search of the all sky survey data 14 extended objects have been found, which have tentatively been identified as previously unknown supernova remnants. A total number of ~ 60 new remnants are expected from the analysis of the full sky.
34
Wardle, Mark, and Korinne McDonnell. "OH Masers and Supernova Remnants." Proceedings of the International Astronomical Union 8, S287 (January 2012): 441–48. http://dx.doi.org/10.1017/s1743921312007491.
Full textAbstract:
AbstractOH(1720 MHz) masers are created by the interaction of supernova remnants with molecular clouds. These masers are pumped by collisions in warm, shocked molecular gas with OH column densities in the range 1016–1017, cm−2. Excitation calculations suggest that inversion of the 6049 MHz OH line may occur at the higher column densities that have been inferred from main-line absorption studies of supernova remnants with the Green Bank Telescope. OH(6049 MHz) masers have therefore been proposed as a complementary indicator of remnant-cloud interaction.This motivated searches for 6049 MHz maser emission from supernova remnants using the Parkes 63 m and Effelsberg 100 m telescopes, and the Australia Telescope Compact Array. A total of forty-one remnants have been examined by one or more of these surveys, but without success. To check the accuracy of the OH column densities inferred from the single-dish observations we modelled OH absorption at 1667 MHz observed with the Very Large Array towards three supernova remnants, IC 443, W44 and 3C 391. The results are mixed – the OH column is revised upwards in IC443, downwards in 3C391, and is somewhat reduced in W44. We conclude that OH columns exceeding 1017 cm−2 are indeed present in some supernova remnants and so the lack of any detections is not explained by low OH column density. We discuss the possibility that non-local line overlap is responsible for suppressing the inversion of the 6049 MHz line.
35
Manchester, RN. "Bi-annular Structure in Supernova Remnants." Australian Journal of Physics 40, no. 6 (1987): 823. http://dx.doi.org/10.1071/ph870823.
Full textAbstract:
In many supernova remnants the radio structure contains loop features. It is proposed that these loop features are generally due to an enhancement of the shell emission in two co-axial rings. This bi-annu1ar enhancement is closely related to the <;ylindrica1 or barrel morphology possessed by most remnants and is probably formed early in the life of the remnant.
36
Meyer, D. M.-A., M. Pohl, M. Petrov, and L. Oskinova. "Non-thermal radio supernova remnants of exiled Wolf–Rayet stars." Monthly Notices of the Royal Astronomical Society 502, no. 4 (February 17, 2021): 5340–55. http://dx.doi.org/10.1093/mnras/stab452.
Full textAbstract:
ABSTRACT A signification fraction of Galactic massive stars (${\ge}8\, \rm M_{\odot }$) are ejected from their parent cluster and supersonically sail away through the interstellar medium (ISM). The winds of these fast-moving stars blow asymmetric bubbles thus creating a circumstellar environment in which stars eventually die with a supernova explosion. The morphology of the resulting remnant is largely governed by the circumstellar medium of the defunct progenitor star. In this paper, we present 2D magneto-hydrodynamical simulations investigating the effect of the ISM magnetic field on the shape of the supernova remnants of a $35\, \mathrm{M}_{\odot }$ star evolving through a Wolf–Rayet phase and running with velocity 20 and $40\, \rm km\, \rm s^{-1}$, respectively. A $7\, \mu \rm G$ ambient magnetic field is sufficient to modify the properties of the expanding supernova shock front and in particular to prevent the formation of filamentary structures. Prior to the supernova explosion, the compressed magnetic field in the circumstellar medium stabilizes the wind/ISM contact discontinuity in the tail of the wind bubble. A consequence is a reduced mixing efficiency of ejecta and wind materials in the inner region of the remnant, where the supernova shock wave propagates. Radiative transfer calculations for synchrotron emission reveal that the non-thermal radio emission has characteristic features reflecting the asymmetry of exiled core-collapse supernova remnants from Wolf–Rayet progenitors. Our models are qualitatively consistent with the radio appearance of several remnants of high-mass progenitors, namely the bilateral G296.5+10.0 and the shell-type remnants CTB109 and Kes 17, respectively.
37
Lozinskaya, TA, and NN Chugaj. "Relationship between Supernova Type and Their Remnants." Australian Journal of Physics 40, no. 6 (1987): 767. http://dx.doi.org/10.1071/ph870767.
Full textAbstract:
The genetic relationship between supernovae (SNe) and -supernova remnants (SNRs) is an important factor in understanding the nature of both phenomena. We present here some new results on SNe and SNRs and discuss their implications in the SN-SNR relationship.
38
Petre, R. "X-Ray Spectroscopy of Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 357–68. http://dx.doi.org/10.1017/s0252921100008216.
Full textAbstract:
X-ray spectroscopy can provide vital information about the progenitors and environments of supernova remnants. Plasma diagnostics and spectral modelling can be used to infer the energy of the remnant, the density and composition of the surrounding medium, and the degree of equilibrium in the shock heated gas. A new generation of X-ray spectrometers, the first of which was the Broad-Band X-Ray Telescope (BBXRT), has improved our ability to make precise measurements of X-ray line fluxes and energies. We summarize the results obtained from the BBXRT mission. These include a definitive measurement of the Fe K line centroid in the Tycho remnant, production of the first narrow-band X-ray maps (of Puppis A) and the first measurement of an electron-ion equipartition timescales in evolved remnants.
39
Kesteven, MJ, JL Caswell, RS Roger, DK Milne, RF Haynes, and KJ Wellington. "Supernova Remnants with Jets." Australian Journal of Physics 40, no. 6 (1987): 855. http://dx.doi.org/10.1071/ph870855.
Full textAbstract:
Two examples are given of probable radio jet/supernova remnant associations: G332.4+0�1 and G 315 �8 - O� O. In both cases the jet length is larger than the radius of the remnant's shell, and the jet diameter is barely resolved and substantially less than the observed shell thickness. The jet luminosity is 5-10% that of the shell. The G332�4 +0.1 jet terminates 'in an extended plume whose luminosity is about 50% that of the shell.
40
Long, Knox S. "Supernova Remnants in Nearby Spiral Galaxies." International Astronomical Union Colloquium 145 (1996): 349–56. http://dx.doi.org/10.1017/s0252921100008204.
Full textAbstract:
Large samples of supernova remnants are needed in order to study the global distribution of supernovae in galaxies, for determining how the environment in which a SN explodes affects the appearance of a SNR, for studying abundances and abundance gradients in galaxies, for estimating SN rates, and in order to determine the energetics of SNRs and their expansion. Here we describe techniques which are currently being used to expand SNR samples in nearby spirals.
41
Leahy, D. A., and M. D. Filipović. "Physical Properties of the Supernova Remnant Population in the Small Magellanic Cloud." Astrophysical Journal 931, no. 1 (May 1, 2022): 20. http://dx.doi.org/10.3847/1538-4357/ac6025.
Full textAbstract:
Abstract The X-ray emission from a supernova remnant is a powerful diagnostic of the state of its shocked plasma. The temperature and the emission measure are related to the energy of the explosion, the age of the remnant, and the density of the surrounding medium. Here we present the results of a study of the remnant population of the Small Magellanic Cloud. Progress in X-ray observations of remnants has resulted in a sample of 20 remnants in the Small Magellanic Cloud with measured temperatures and emission measures. We apply spherically symmetric supernova remnant evolution models to this set of remnants to estimate ages, explosion energies, and circumstellar medium densities. The distribution of ages yields a remnant birth rate of ∼1/1200 yr. The energies and densities are well fit with log-normal distributions, with means of 1.6 × 1051 erg and 0.14 cm−3, and 1σ dispersions of a factor of 1.87 in energy and 3.06 in density, respectively.
42
Tsuna, Daichi. "Failed supernova remnants." Publications of the Astronomical Society of Japan 73, no. 3 (May 13, 2021): L6—L11. http://dx.doi.org/10.1093/pasj/psab041.
Full textAbstract:
Abstract In a failed supernova, partial ejection of the progenitor’s outer envelope can occur due to weakening of the core’s gravity by neutrino emission in the protoneutron star phase. We consider emission when this ejecta sweeps up the circumstellar material, analogous to supernova remnants (SNRs). We focus on failed explosions of blue supergiants, and find that the emission can be bright in soft X-rays. Due to its soft emission, we find that sources in the Large Magellanic Cloud (LMC) are more promising for detection than those in the Galactic disk. These remnants are characteristic in their small size (≲10 pc) and slow speed (100s of km s−1) compared to typical SNRs. Although the expected number of detectable sources is small (up to a few by the eROSITA four-year all-sky survey), prospects are better for deeper surveys targeting the LMC. Detection of these “failed SNRs” will realize observational studies of mass ejection following black hole formation.
43
Seward, Frederick D., Paul Gorenstein, and Wallace H. Tucker. "Young Supernova Remnants." Scientific American 253, no. 2 (August 1985): 88–96. http://dx.doi.org/10.1038/scientificamerican0885-88.
Full text
44
Manchester, R. N. "Dating supernova remnants." Nature 356, no. 6371 (April 1992): 660–61. http://dx.doi.org/10.1038/356660a0.
Full text
45
Decourchelle, Anne. "Supernova remnants dynamics." Proceedings of the International Astronomical Union 12, S331 (February 2017): 164–73. http://dx.doi.org/10.1017/s1743921317006342.
Full textAbstract:
AbstractSupernova remnants are the site of a number of physical processes (shock-heating, non-equilibrium ionization, hydrodynamic instabilities, particle acceleration, magnetic field amplification). Their related emission processes provide us with a large set of observational data. Supernova remnants result from the interaction of high-velocity material ejected by the supernova explosion with the medium surrounding the progenitor star. This interaction gives rise to a double-shock structure that lasts for hundreds of years, with a forward shock and a reverse shock compressing and heating to tens million of degrees the surrounding medium and the ejecta, respectively. It is mostly in this phase that young supernova remnants provide information on their explosion mechanism through spectro-imaging observations of the ejected nucleosynthesis products and their dynamics, notably in the X-ray domain. I will review these observations and their implications for our current understanding of the dynamics of supernova remnants. I will conclude on the prospects with future facilities.
46
Różyczka, M. "Multiple-Supernova Remnants." International Astronomical Union Colloquium 120 (1989): 463–73. http://dx.doi.org/10.1017/s0252921100024271.
Full textAbstract:
ABSTRACTThe present observational and theoretical status of multiple-supernova remnants is briefly reviewed, and evolutionary models of the remnants around OB associations are presented. The remnants are followed for up to almost 30 Myr in various galactic environments (Gaussian or composite disks combined with cold or hot halos). It is found that the presence of a hot halo profoundly modifies the evolution of the remnants, promoting the evaporation of their shells and leading to noneruptive merging of the ejecta with the halo gas. The results also suggest an explanation for the observed deficiency of evolved multiple-supernova remnants.
47
CHANAN, G. "Galactic Supernova Remnants: The Crab Nebula and Related Supernova Remnants." Science 232, no. 4751 (May 9, 1986): 778. http://dx.doi.org/10.1126/science.232.4751.778.
Full text
48
Guseinov, O. H., A. Ankay, and S. O. Tagieva. "Observational data on Galactic supernova remnants III: The supernova remnants within l = 270°-360°." Serbian Astronomical Journal, no. 169 (2004): 65–82. http://dx.doi.org/10.2298/saj0469065g.
Full textAbstract:
We have collected all the available data of Galactic supernova remnants given in the literature. The data of Galactic supernova remnants located in the Galactic longitude interval l=270?-360?in all the spectral bands are represented in this work. We have adopted distance values for the supernova remnants by examining these data. The data of various types of neutron stars connected to these supernova remnants are also displayed. The remarks of some authors and us on the data and some properties of both the supernova remnants and the point sources are also represented.
49
Stone, Alice Griffeth, Heather T. Johnson, John M. Blondin, Richard A. Watson, Kazimierz J. Borkowski, Carla Fröhlich, Ivo R. Seitenzahl, and Stephen P. Reynolds. "Type Ia Supernova Models: Asymmetric Remnants and Supernova Remnant G1.9+0.3." Astrophysical Journal 923, no. 2 (December 1, 2021): 233. http://dx.doi.org/10.3847/1538-4357/ac300f.
Full textAbstract:
Abstract The youngest Galactic supernova remnant, G1.9+0.3, probably the result of a Type Ia supernova, shows surprising anomalies in the distribution of its ejecta in space and velocity. In particular, high-velocity shocked iron is seen in several locations far from the remnant center, in some cases beyond prominent silicon and sulfur emission. These asymmetries strongly suggest a highly asymmetric explosion. We present high-resolution hydrodynamic simulations in two and three dimensions of the evolution from ages of 100 s to hundreds of years of two asymmetric Type Ia models, expanding into a uniform medium. At the age of G1.9+0.3 (about 100 yr), our 2D model shows almost no iron shocked to become visible in X-rays. Only in a much higher-density environment could significant iron be shocked, at which time the model's expansion speed is completely inconsistent with the observations of G1.9+0.3. Our 3D model, evolving the most asymmetric of a suite of Type Ia supernova models from Seitenzahl et al. (2013), shows some features resembling G1.9+0.3. We characterize its evolution with images of composition in three classes: C and O, intermediate-mass elements (IMEs), and iron-group elements (IGEs). From ages of 13 to 1800 yr, we follow the evolution of the highly asymmetric initial remnant as the explosion asymmetries decrease in relative strength, to be replaced by asymmetries due to evolutionary hydrodynamic instabilities. At an age of about 100 yr, our 3D model has comparable shocked masses of C+O, IMEs, and IGEs, with about 0.03 M ⊙ each. Evolutionary changes appear to be rapid enough that continued monitoring with the Chandra X-ray Observatory may show significant variations.
50
Reyes-Iturbide, J., I. Ramírez-Ballinas, M. Rosado, D. Núñez, P. Ambrocio-Cruz, L. Arias, and R. Gabbasov. "Supernova remnant W51C: optical and X-ray emission analysis." Monthly Notices of the Royal Astronomical Society 516, no. 4 (October 4, 2022): 6055–65. http://dx.doi.org/10.1093/mnras/stac2568.
Full textAbstract:
ABSTRACT We present observations of the optical and X-ray emission from the Galactic supernova remnant W51C. From [S ii] Fabry–Pérot interferometry and H α and [S ii] images we detect filaments that are part of the optical counterpart of the supernova remnant. We obtain the kinematic distance to W51C, showing that it is one of the shortest distances reported in the literature. We also estimate other physical properties such as the velocity of the shock induced in the cloudlets emitted at optical wavelengths and the electron density of those cloudlets. From XMM–Newton observatory archival data, we obtain images of the diffuse X-ray emission of this supernova remnant. The spectrum of the X-ray emission is explored to estimate X-ray parameters such as luminosity and temperature of the hot plasma in the supernova remnant. We fit a thermal model with a plasma temperature of 1.4 keV for an X-ray thermal luminosity of 2.0 × 1036 erg s−1. With the parameters described above we test the model proposed by White & Long to explain the mixed morphology observed in W51C. We obtain an initial energy of the supernova explosion of 8.4 × 1050 erg and an age of 13 000 yr. The derived initial energy is typical of supernova remnants, but in disagreement with respect to older estimations that found higher values and suggested that W51C was the result of the explosion of two supernovae.