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31.
Astronomy Letters - We analyze the physical processes that should be taken into account when modeling young type-Ia supernova remnants (SNRs) with ages of several hundred years in which forward... 相似文献
32.
We study analytically the Rayleigh–Taylor instability in expanding supernova gas shell. The instability appears at the inner
shell surface accelerated by blowing pulsar wind. The most dangerous perturbations correspond to wavelengths comparable to
the shell thickness. We analyze the fragility of the supernova remnant shell in function of the initial perturbation amplitude
and the shell thickness. 相似文献
33.
34.
Srinivasan G. Bhattacharya D. Dwarakanath K. S. 《Journal of Astrophysics and Astronomy》1984,5(4):403-423
We conclude that pulsar-driven supernova remnants (SNRs) are extremely rare objects. Indeed an analysis of the known sample
of plerions suggests a very low birthrate ∼ 1 in 240 years. Long-lived and bright plerions like the Crab nebula are likely
to be produced only when the pulsar has an initial period ∼ 10–20 milliseconds and a field ∼ 1012 G. Such pulsars inside rapidly expanding shell remnants should also produce detectable plerions. The extreme rarity of SNRs
with such hybrid morphology leads us to conclude that these pulsars must have been born with an initial period larger than
∼ 35–70 milliseconds.
Joint Astronomy Program, Department of Physics, Indian Institute of Science, Bangalore 560012. 相似文献
35.
I. V. Gosachinskij 《Astronomy Letters》2001,27(4):233-238
Based on RATAN-600 21-cm line observations with an angular resolution of 2.4′ over a wide range of radial velocities, we analyze the neutral-hydrogen distribution in the region of the SNR G78.2+2.1. In addition to an H I shell at low radial velocities immediately surrounding the radio remnant, we detected an extended expanding H I shell, ≈3° in diameter, at a radial velocity of ?25 km s?1, which closely coincides in coordinates and angular sizes with the outer X-ray shell discovered by Lozinskaya et al. (2000). The Hα emission studied by these authors in the SNR region also has a secondary peak at radial velocities from ?45 to ?20 km s?1. Since the radial velocities of these two objects differ significantly, their distances can be assumed to differ as well; i.e., a chance projection of two distinct objects is observed. 相似文献
36.
S. Jane Arthur 《Astrophysics and Space Science》2002,281(1-2):267-270
The radiation produced by the gas cooling behind a fast supernova remnant shock in the interstellar medium is capable of ionizing
the undisturbed medium ahead of the shock wave. In this work I investigate the nonequilibrium evolution of these photoionized
precursor regions by means of radiation-hydrodynamic simulations of supernova remnant evolution.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
37.
N. N. Chugai S. N. Fabrika O. N. Sholukhova V. P. Goranskij P. K. Abolmasov V. V. Vlasyuk 《Astronomy Letters》2005,31(12):792-805
Photometric and spectroscopic observations of the nearby type-IIP supernova 2004dj are presented. The 56Ni mass in the envelope of SN 2004dj was estimated from the light curve to be ≈0.02M⊙. This estimate is confirmed by modeling the Hα luminosity. The Hα emission line exhibits a strong asymmetry characterized by the presence of a blue component in the line with a shift of ?1600 km s?1 at the early nebular phase. A similar asymmetry was found in the Hβ, [O I], and [Ca II] lines. The line asymmetry is interpreted as being the result of asymmetric 56Ni ejecta. The Hα profile and its evolution are reproduced in the model of an asymmetric bipolar 56Ni structure for a spherical hydrogen distribution. The mass of the front 56Ni jet is comparable to that of the central component and twice that of the rear 56Ni jet. We point out that the asymmetric bipolar structure of 56Ni ejecta is also present in SN 1999em, a normal type-IIP supernova. 相似文献
38.
The compact source 0125 + 628 in the centre of the galactic supernova remnant G 127.1 + 0.5 has been re-observed in HI absorption
using the Westerbork Synthesis Radio Telescope (WSRT). The outer arm HI absorption atV = -95km s-1 has been confirmed. The absorption spectrum is similar to that of the nearby extragalactic source 0123 + 633. We discuss
the arguments concerning an extragalactic origin of 0125 + 628 and conclude that it is most likely extragalactic and not an
SS 433 type object.
The National Radio Astronomy Observatory is operated by Associated Universities Inc. under contract with the National Science
Foundation. 相似文献
39.
Radiation from the Magellanic Clouds is discussed from the point of view of near future possibilities in observational γ-ray
astronomy. The γ-ray fluxes expected according to the metagalactic and galactic theories of the origin of cosmic rays are
compared. It is shown that the strongest test of the metagalactic hypothesis will be provided by a determination of the ratio
of γ-ray fluxes from SMC and LMC. The γ-ray luminosity of a typical young supernova remnant that can generate sufficient antiprotons
is estimated. It is shown that such remnants must have a short phase during which they are very powerful γ-ray emitters. 相似文献
40.
The investigation of supernova remnants (SNRs) across the electromagnetic spectrum from radio up to very high energy gamma-rays can serve as a test of the particle acceleration and touches on one of the unresolved problems of modern astrophysics, namely the origin of cosmic rays and the Galaxy's contribution to the overall cosmic ray spectrum. The multiwavelength observations of Cas A SNR demonstrated that structure and spectral features have clear signs of young SNRs and its overall properties make this object the best target to test a hypothesis of cosmic ray origin in SNRs. Studies of Cas A at very high energies by SHALON telescope showed the location of TeV gamma-ray emission region relative to the position of reveres shock. Also, the spectral energy distribution was obtained at high and very high energies. To describe the spectral and structural features of this SNR viewed in non-thermal emission, two approaches involving reverse and also both reverse and forward shocks to the mechanism of diffusive shock acceleration of cosmic rays in Cas A were applied. It is demonstrated that the observational properties of Cas A are well reproduced by the hadronic model with significant contribution of both the forward and reverse shocks in the generation of broadband emission. Calculation results suggest that the very high efficiency of particle acceleration in Cas A, which value is up to 25% of the supernova explosion energy with energy of accelerated particles not exceeding of eV. Whereas, the forward shock model predicts the spectral characteristics of the TeV-gamma-emission corresponding to ones detected at 800 GeV–40 TeV that are the evidence of acceleration of the hadronic cosmic rays in shells of SNRs up to eV 相似文献