X-ray spectra of the Cassiopeia A and TYCHO supernova remnants and their element abundances

Tsunemi, H.; Yamashita, K.; Masai, K.; Hayakawa, S.; Koyama, K.

doi:10.1086/164337

Cited by 44 publications

(30 citation statements)

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“…The upper boundary of the velocity range corresponds approximately to the location at which the convective deflagration front freezes. As shown in figure 3, the resultant spectrum agrees well with the spectrum observed with the satellite Tenma (Tsunemi et al 1986), if the interstellar hydrogen column density, % , to Tycho is taken to be about 1 x 1 0 " cm" . For a conventional value of % = 3 xlO^-1 cm" , the calculated photon fluxes below 2.5 keV are larger than the observed fluxes by up to a factor of 1.8.…”

Section: The Remnant Of Sn 1572 (Tycho)supporting

confidence: 71%

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The X-ray Emission from SN 1987A and the Remnant of SN 1572 (Tycho)

Itoh

Masai

Nomoto

1988

International Astronomical Union Colloquium

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The thermal X-ray emission from SN 1987A may be enhanced to a detectable level when the blast shock hits the circumstellar medium which has formed in the red-supergiant stage of the progenitor.The X-ray spectrum of Tycho observed with the satellite Tenma can be explained approximately within the context of a carbon deflagration model for Type la supernovae, if the ejecta are assumed to be mixed partially.

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Section: The Remnant Of Sn 1572 (Tycho)supporting

confidence: 71%

“…The observed outer radius and thickness of the reverse shock wave (Seward et al 1983) and the observed continuum spectrum (Tsunemi et al 1986) are reproduced approximately for an age of 411 yr, by assuming an ambient density of 1.3 amu cm"3. Then the distance to Tycho is obtained as 2.43 kpc.…”

Section: The Remnant Of Sn 1572 (Tycho)mentioning

confidence: 81%

The X-ray Emission from SN 1987A and the Remnant of SN 1572 (Tycho)

Itoh

Masai

Nomoto

1988

International Astronomical Union Colloquium

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“…Many works have focused on these emission lines from young SNRs, e.g. W49B (Hwang et al 2000a;Miceli et al 2006), Tycho (Tsunemi et al 1986;Hwang et al 1997), Cas A (Tsunemi et al 1986;Holt et al 1994;Hughes et al 2000;Hwang et al 2000b) and Kepler (Hatsukade et al 1990; Kinugasa & Tsunemi, 1999;Cassam-Chenaï et al 2004;Reynolds et al 2007). Comparision of the abundance pattern of an SNR with the theoretical predictions could be used to constrain the properties of the corresponding supernova (SN) (e.g., Hughes et al 1995;Rakowski et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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

Yang¹,

Tsunemi²,

Lu³

et al. 2009

ApJ

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We performed a Cr-K emission line survey in young supernova remnants (SNRs) with the Chandra archival data. Our sample includes W49B, Cas A, Tycho and Kepler. We confirmed the existence of the Cr line in W49B and discovered this emission line in the other three SNRs. The line center energies, equivalent widths (EWs) and fluxes of the Cr lines are given. The Cr in Cas A is in a high ionization state while that in Tycho and Kepler is in a much lower one. We find a good positive correlation between Cr and Fe line center energies, suggesting a common origin of Cr and Fe in the nucleosynthesis, which is consistent with the theoretical predictions. We propose that the EW ratio between Cr and Fe can be used as a supplementary constraint on the progenitors' properties and the explosion mechanism.

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“…They compute that 20 keV electrons having a proportion of 1 % of the total number of electrons are sufficient to explain the OVII lines as observed in Puppis-A. Further evidence for NEI conditions in Tycho and Cas-A has been obtained from the EXOSAT and Tenma (Tsunemi et al 1986) observations of the Fe-K line. Both experiments have measured consistently a line energy significantly lower than the value expected from CEI which is based upon a temperature derived from the high energy continuum.…”

mentioning

confidence: 94%

“…Similiar spectra are available for Cas-A, Kepler, RCW 103 and W49B and a detailed account of the EXOSAT spectra is given by Smith (1987). Tsunemi et al (1986) have published the Tenma GSPC energy spectra of Cas-A and Tycho which extend to some lower energies to include the Si-K lines (see figure *f). The emission from shell type remnants is considered to originate from an optically thin plasma, which has been heated to X-ray temperatures by shock waves.…”

mentioning

confidence: 99%