Doppler-broadened iron x-ray lines from tycho's supernova remnant

Akihiro Furuzawa, Daisuke Ueno, Asami Hayato, Midori Ozawa, Toru Tamagawa, Aya Bamba, John P. Hughes, Hideyo Kunieda, Kazuo Makishima, Stephen S. Holt, Una Hwang, Kenzo Kinugasa, Robert Petre, Keisuke Tamura, Hiroshi Tsunemi, Shigeo Yamauchi

Research output: Contribution to journalArticle

13 Citations (Scopus)

Abstract

We use Suzaku observations to measure the spatial variation of the Fe Kα line with radius in the Tycho supernova remnant. The Fe line widths show a significant decrease from a FWHM value of 210 eV at the center to 130 eV at the rim. Over the same radial range the line center energy remains nearly constant. These observations are consistent with a scenario in which the shell of Fe-emitting ejecta in Tycho is expanding at speeds of 2800-3350 km s -1. The minimum line width we measure is still a factor of two larger than expected from a single component plasma emission model. If thermal Doppler broadening is the dominant additional source of broadening, we infer an ion temperature of (1-3) × 1010 K.

Original languageEnglish
JournalAstrophysical Journal
Volume693
Issue number2
DOIs
Publication statusPublished - 01-01-2009

Fingerprint

supernova remnants
ejecta
spatial variation
shell
plasma
iron
K lines
ion
ion temperature
rims
energy
x rays
temperature
radii
speed

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Furuzawa, A., Ueno, D., Hayato, A., Ozawa, M., Tamagawa, T., Bamba, A., ... Yamauchi, S. (2009). Doppler-broadened iron x-ray lines from tycho's supernova remnant. Astrophysical Journal, 693(2). https://doi.org/10.1088/0004-637X/693/2/L61
Furuzawa, Akihiro ; Ueno, Daisuke ; Hayato, Asami ; Ozawa, Midori ; Tamagawa, Toru ; Bamba, Aya ; Hughes, John P. ; Kunieda, Hideyo ; Makishima, Kazuo ; Holt, Stephen S. ; Hwang, Una ; Kinugasa, Kenzo ; Petre, Robert ; Tamura, Keisuke ; Tsunemi, Hiroshi ; Yamauchi, Shigeo. / Doppler-broadened iron x-ray lines from tycho's supernova remnant. In: Astrophysical Journal. 2009 ; Vol. 693, No. 2.
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author = "Akihiro Furuzawa and Daisuke Ueno and Asami Hayato and Midori Ozawa and Toru Tamagawa and Aya Bamba and Hughes, {John P.} and Hideyo Kunieda and Kazuo Makishima and Holt, {Stephen S.} and Una Hwang and Kenzo Kinugasa and Robert Petre and Keisuke Tamura and Hiroshi Tsunemi and Shigeo Yamauchi",
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Furuzawa, A, Ueno, D, Hayato, A, Ozawa, M, Tamagawa, T, Bamba, A, Hughes, JP, Kunieda, H, Makishima, K, Holt, SS, Hwang, U, Kinugasa, K, Petre, R, Tamura, K, Tsunemi, H & Yamauchi, S 2009, 'Doppler-broadened iron x-ray lines from tycho's supernova remnant', Astrophysical Journal, vol. 693, no. 2. https://doi.org/10.1088/0004-637X/693/2/L61

Doppler-broadened iron x-ray lines from tycho's supernova remnant. / Furuzawa, Akihiro; Ueno, Daisuke; Hayato, Asami; Ozawa, Midori; Tamagawa, Toru; Bamba, Aya; Hughes, John P.; Kunieda, Hideyo; Makishima, Kazuo; Holt, Stephen S.; Hwang, Una; Kinugasa, Kenzo; Petre, Robert; Tamura, Keisuke; Tsunemi, Hiroshi; Yamauchi, Shigeo.

In: Astrophysical Journal, Vol. 693, No. 2, 01.01.2009.

Research output: Contribution to journalArticle

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T1 - Doppler-broadened iron x-ray lines from tycho's supernova remnant

AU - Furuzawa, Akihiro

AU - Ueno, Daisuke

AU - Hayato, Asami

AU - Ozawa, Midori

AU - Tamagawa, Toru

AU - Bamba, Aya

AU - Hughes, John P.

AU - Kunieda, Hideyo

AU - Makishima, Kazuo

AU - Holt, Stephen S.

AU - Hwang, Una

AU - Kinugasa, Kenzo

AU - Petre, Robert

AU - Tamura, Keisuke

AU - Tsunemi, Hiroshi

AU - Yamauchi, Shigeo

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AB - We use Suzaku observations to measure the spatial variation of the Fe Kα line with radius in the Tycho supernova remnant. The Fe line widths show a significant decrease from a FWHM value of 210 eV at the center to 130 eV at the rim. Over the same radial range the line center energy remains nearly constant. These observations are consistent with a scenario in which the shell of Fe-emitting ejecta in Tycho is expanding at speeds of 2800-3350 km s -1. The minimum line width we measure is still a factor of two larger than expected from a single component plasma emission model. If thermal Doppler broadening is the dominant additional source of broadening, we infer an ion temperature of (1-3) × 1010 K.

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