A Cr-K EMISSION LINE SURVEY IN YOUNG SUPERNOVA REMNANTS WITH<i>CHANDRA</i>

Yang, Xuejuan; Tsunemi, H.; Lu, F. J.; Chen, L.

doi:10.1088/0004-637x/692/1/894

Cited by 18 publications

(16 citation statements)

References 33 publications

(68 reference statements)

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“…Since no photon emissivity data existed for the He-like stages of Co or Mn, Hwang et al (2000) estimated emissivities by interpolating the emissivity data generated for Ca, Fe, Ni by the Raymond and Smith thermal models Raymond & Smith 1977; these were then used to infer the abundances of these elements. Subsequently, Cr line emission has been reported for W49B, Tycho's SNR, Kepler's SNR, and Cas A with Chandra observations (Yang et al 2009). Generally the Cr ion states (as estimated by the centroid energy of the Cr emission in these moderate-resolution CCD spectra) track the ion stages of Fe in the same objects and range from an estimated Ne-like to He-like ions.…”

Section: Introductionmentioning

confidence: 94%

Electron-impact excitation of H-like Cr, Mn, Fe, Co, and Ni for applications in modeling X-ray astrophysical sources

Malespin

Ballance

Pindzola

et al. 2011

A&A

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Context. Accurate atomic data for the less abundance Fe-peak elements are required for use in X-ray astrophysical studies. Aims. We calculate high quality electron-impact excitation collision strengths and effective collision strengths for hydrogenic Cr, Mn, Fe, Co, and Ni. Methods. We use the Dirac R-matrix method, the intermediate coupling frame transformation R-matrix method, the semi-relativistic distorted-wave method and the fully-relativistic distorted-wave method to calculate collision strengths for each of the ions. The ADAS collisional-radiative codes are used to produce photon emissivity coefficients for each ion. Results. Results are presented for atomic energy levels, spontaneous emission coefficients, electron-impact excitation collision strengths and associated effective collision strengths for each of the five species under consideration. We find relativistic effects can contribute an approximate 10% increase to the background cross section in relation to semi-relativistic collision calculations. We also confirm that radiation damping plays a prominent role for certain near threshold resonances. In order check the integration of our results within collisional-radiative modeling codes, we have used the ADAS package for some preliminary modeling of photon emissivities. The atomic data shall be made available online through the OPEN-ADAS site and the CFADC database

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Section: Introductionmentioning

confidence: 94%

Electron-impact excitation of H-like Cr, Mn, Fe, Co, and Ni for applications in modeling X-ray astrophysical sources

Malespin

Ballance

Pindzola

et al. 2011

A&A

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“…However, recently Tamagawa et al (2009) reported the detection of chromium (Cr, Z = 24) and manganese (Mn, Z = 25) Kα line emission from Tycho's SNR using Suzaku data ( Fig. 23, see also Yang et al, 2009). The nucleosynthesis of Mn is influenced by the presence of the neutron rich element 22 Ne, whose abundance is determined by the metallicity of the white dwarf progenitor.…”

Section: Type Ia Supernova Remnants 81 X-ray Spectroscopy Of Type Iamentioning

confidence: 99%

Supernova remnants: the X-ray perspective

Vink

2011

Astron Astrophys Rev

425

323

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Supernova remnants are beautiful astronomical objects that are also of high scientific interest, because they provide insights into supernova explosion mechanisms, and because they are the likely sources of Galactic cosmic rays. X-ray observations are an important means to study these objects. And in particular the advances made in X-ray imaging spectroscopy over the last two decades has greatly increased our knowledge about supernova remnants. It has made it possible to map the products of fresh nucleosynthesis, and resulted in the identification of regions near shock fronts that emit X-ray synchrotron radiation. Since X-ray synchrotron radiation requires 10-100 TeV electrons, which lose their energies rapidly, the study of X-ray synchrotron radiation has revealed those regions where active and rapid particle acceleration is taking place.In this text all the relevant aspects of X-ray emission from supernova remnants are reviewed and put into the context of supernova explosion properties and the physics and evolution of supernova remnants. The first half of this review has a more tutorial style and discusses the basics of supernova remnant physics and X-ray spectroscopy of the hot plasmas they contain. This includes hydrodynamics, shock heating, thermal conduction, radiation processes, non-equilibrium ionization, He-like ion triplet lines, and cosmic ray acceleration. The second half offers a review of the advances made in field of X-ray spectroscopy of supernova remnants during the last 15 year. This period coincides with the availability of X-ray imaging spectrometers. In addition, I discuss the results of high resolution X-ray spectroscopy with the Chandra and XMM-Newton gratings. Although these instruments are not ideal for studying extended sources, they nevertheless provided interesting results for a limited number of remnants. These results provide a glimpse of what may be achieved with future microcalorimeters that will be available on board future X-ray observatories. In discussing the results of the last 15 years I have chosen to discuss a few topics that are of particular interest. These include the properties of Type Ia supernova remnants, which appear to be regularly shaped and have stratified ejecta, in contrast to core collapse supernova remnants, which have patchy ejecta distributions. For core collapse supernova remnants I discuss the spatial distribution of fresh nucleosynthesis products, but also their properties in connection to the neutron stars they contain.For the mature supernova remnants I focus on the prototypal supernova remnants Vela and the Cygnus Loop. And I discuss the interesting class of mixed-morphology remnants. Many of these mature supernova remnants contain still plasma with enhanced ejecta abundances. Over the last five years it has also become clear that many mixed-morphology remnants contain plasma that is overionized. This is in contrast to most other supernova remnants, which contain underionized plasmas.This text ends with a review of X-ray synchrotron radiatio...

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“…After submitting our paper for publication, we became aware of an independent paper by Yang et al (2009) on the same subject on the Cr-K line. Their conclusions are very similar to those presented here: Cr and Fe are colocated.…”

Section: Cr-k Linementioning

confidence: 99%

Suzaku X-Ray Imaging and Spectroscopy of Cassiopeia A

Maeda¹,

Uchiyama²,

Bamba³

et al. 2009

Publications of the Astronomical Society of Japan

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Suzaku X-ray observations of a young supernova remnant, Cassiopeia A, were carried out. K-shell transition lines from highly ionized ions of various elements were detected, including Chromium (Cr-Kα at 5.61 keV). The X-ray continuum spectra 1 were modeled in the 3.4-40 keV band, summed over the entire remnant, and were fitted with a simplest combination of the thermal bremsstrahlung and the non-thermal cut-off power-law models. The spectral fits with this assumption indicate that the continuum emission is likely to be dominated by the non-thermal emission with a cut-off energy at > 1 keV. The thermal-to-nonthermal fraction of the continuum flux in the 4-10 keV band is best estimated as ∼0.1. Non-thermal-dominated continuum images in the 4-14 keV band were made. The peak of the non-thermal X-rays appears at the western part. The peak position of the TeV γ-rays measured with HEGRA and MAGIC is also shifted at the western part with the 1-sigma confidence. Since the location of the X-ray continuum emission was known to be presumably identified with the reverse shock region, the possible keV-TeV correlations give a hint that the accelerated multi-TeV hadrons in Cassiopeia A are dominated by heavy elements in the reverse shock region.

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A Cr-K EMISSION LINE SURVEY IN YOUNG SUPERNOVA REMNANTS WITHCHANDRA

Cited by 18 publications

References 33 publications

Electron-impact excitation of H-like Cr, Mn, Fe, Co, and Ni for applications in modeling X-ray astrophysical sources

Electron-impact excitation of H-like Cr, Mn, Fe, Co, and Ni for applications in modeling X-ray astrophysical sources

Supernova remnants: the X-ray perspective

Suzaku X-Ray Imaging and Spectroscopy of Cassiopeia A

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