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Title: FAR-ULTRAVIOLET EMISSION-LINE MORPHOLOGIES OF THE SUPERNOVA REMNANT G65.3+5.7

Abstract

We present the first far-ultraviolet (FUV) emission-line morphologies of the whole region of the supernova remnant (SNR) G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C IV {lambda}{lambda}1548, 1551, He II {lambda}1640, and O III] {lambda}{lambda}1661, 1666 lines appear to be closely related to the optical and/or soft X-ray images obtained in previous studies. Dramatic differences between the C IV morphology and the optical [O III] {lambda}5007 image provide clues to a large resonant-scattering region and a foreground dust cloud. The FUV morphologies also reveal the overall distribution of various shocks in different evolutionary phases and an evolutionary asymmetry between the east and the southwest sides in terms of Galactic coordinates, possibly due to a Galactic density gradient in the global scale. The relative X-ray luminosity of G65.3+5.7 to C IV luminosity is considerably lower than those of the Cygnus Loop and the Vela SNRs. This implies that G65.3+5.7 has almost evolved into the radiative stage in the global sense and supports the previous proposal that G65.3+5.7 has lost its bright X-ray shell and become a member of mixed-morphology SNRs as it has evolved beyond the adiabatic stage.

Authors:
; ; ;  [1];  [2];  [3]
  1. Korea Astronomy and Space Science Institute, 305-348 Daejeon (Korea, Republic of)
  2. Korea Advanced Institute of Science and Technology, 305-701 Daejeon (Korea, Republic of)
  3. Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States)
Publication Date:
OSTI Identifier:
21464707
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 722; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/722/1/388; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; DUSTS; EMISSION; FAR ULTRAVIOLET RADIATION; LUMINOSITY; RESONANCE SCATTERING; SOFT X RADIATION; SUPERNOVA REMNANTS; COSMIC RADIO SOURCES; ELECTROMAGNETIC RADIATION; INELASTIC SCATTERING; IONIZING RADIATIONS; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; PHYSICS; RADIATIONS; SCATTERING; ULTRAVIOLET RADIATION; X RADIATION

Citation Formats

Kim, I -J, Seon, K -I, Shinn, J -H, Han, W, Min, K -W, and Edelstein, J. FAR-ULTRAVIOLET EMISSION-LINE MORPHOLOGIES OF THE SUPERNOVA REMNANT G65.3+5.7. United States: N. p., 2010. Web. doi:10.1088/0004-637X/722/1/388.
Kim, I -J, Seon, K -I, Shinn, J -H, Han, W, Min, K -W, & Edelstein, J. FAR-ULTRAVIOLET EMISSION-LINE MORPHOLOGIES OF THE SUPERNOVA REMNANT G65.3+5.7. United States. https://doi.org/10.1088/0004-637X/722/1/388
Kim, I -J, Seon, K -I, Shinn, J -H, Han, W, Min, K -W, and Edelstein, J. 2010. "FAR-ULTRAVIOLET EMISSION-LINE MORPHOLOGIES OF THE SUPERNOVA REMNANT G65.3+5.7". United States. https://doi.org/10.1088/0004-637X/722/1/388.
@article{osti_21464707,
title = {FAR-ULTRAVIOLET EMISSION-LINE MORPHOLOGIES OF THE SUPERNOVA REMNANT G65.3+5.7},
author = {Kim, I -J and Seon, K -I and Shinn, J -H and Han, W and Min, K -W and Edelstein, J},
abstractNote = {We present the first far-ultraviolet (FUV) emission-line morphologies of the whole region of the supernova remnant (SNR) G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C IV {lambda}{lambda}1548, 1551, He II {lambda}1640, and O III] {lambda}{lambda}1661, 1666 lines appear to be closely related to the optical and/or soft X-ray images obtained in previous studies. Dramatic differences between the C IV morphology and the optical [O III] {lambda}5007 image provide clues to a large resonant-scattering region and a foreground dust cloud. The FUV morphologies also reveal the overall distribution of various shocks in different evolutionary phases and an evolutionary asymmetry between the east and the southwest sides in terms of Galactic coordinates, possibly due to a Galactic density gradient in the global scale. The relative X-ray luminosity of G65.3+5.7 to C IV luminosity is considerably lower than those of the Cygnus Loop and the Vela SNRs. This implies that G65.3+5.7 has almost evolved into the radiative stage in the global sense and supports the previous proposal that G65.3+5.7 has lost its bright X-ray shell and become a member of mixed-morphology SNRs as it has evolved beyond the adiabatic stage.},
doi = {10.1088/0004-637X/722/1/388},
url = {https://www.osti.gov/biblio/21464707}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 722,
place = {United States},
year = {Sun Oct 10 00:00:00 EDT 2010},
month = {Sun Oct 10 00:00:00 EDT 2010}
}