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Article: Evolution of the reverse shock emission from SNR 1987A

TitleEvolution of the reverse shock emission from SNR 1987A
Authors
KeywordsCircumstellar Matter
Shock Waves
Supernova Remnants
Supernovae: Individual (Sn 1987A)
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 644 n. 2 II, p. 959-970 How to Cite?
AbstractWe present new (2004 July) G750L and G140L Space Telescope Imaging Spectrograph (STIS) data of the Hα and Lyα emission from supernova remnant (SNR) 1987A. With the aid of earlier data, from 1997 October to 2002 October, we track the local evolution of Lyα emission and both the local and global evolution of Hα emission. The most recent observations allow us to directly compare the Hα and Lyα emission from the same slit position and at the same epoch. Consequently, we find clear evidence that, unlike Hα, Lyα is reflected from the debris by resonant scattering, In addition to emission that we can clearly attribute to the surface of the reverse shock, we also measure comparable emission, in both Hα and Lyα, that appears to emerge from supernova debris interior to the surface. New observations taken through slits positioned slightly eastward and westward of a central slit show a departure from cylindrical symmetry in the Hα surface emission. Using a combination of old and new observations, we construct a light curve of the total Hα flux, F, from the reverse shock, which has increased by a factor of ∼4 over about 8 yr. However, due to large systematic uncertainties, we are unable to discern between the two limiting behaviors of the flux: F ∝ t (self-similar expansion) and F ∝ t 5 (halting of the reverse shock). Such a determination is important for constraining the rate of hydrogen atoms crossing the shock, which is relevant to the question of whether the reverse shock emission will vanish in ≳7 yr. Future deep, low- or moderate-resolution spectra are essential for accomplishing this task. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175050
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHeng, Ken_US
dc.contributor.authorMccray, Ren_US
dc.contributor.authorZhekov, SAen_US
dc.contributor.authorChallis, PMen_US
dc.contributor.authorChevalier, RAen_US
dc.contributor.authorCrotts, APSen_US
dc.contributor.authorFransson, Cen_US
dc.contributor.authorGarnavich, Pen_US
dc.contributor.authorKirshner, RPen_US
dc.contributor.authorLawrence, SSen_US
dc.contributor.authorLundqvist, Pen_US
dc.contributor.authorPanagia, Nen_US
dc.contributor.authorPun, CSJen_US
dc.contributor.authorSmith, Nen_US
dc.contributor.authorSollerman, Jen_US
dc.contributor.authorWang, Len_US
dc.date.accessioned2012-11-26T08:48:58Z-
dc.date.available2012-11-26T08:48:58Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 644 n. 2 II, p. 959-970en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175050-
dc.description.abstractWe present new (2004 July) G750L and G140L Space Telescope Imaging Spectrograph (STIS) data of the Hα and Lyα emission from supernova remnant (SNR) 1987A. With the aid of earlier data, from 1997 October to 2002 October, we track the local evolution of Lyα emission and both the local and global evolution of Hα emission. The most recent observations allow us to directly compare the Hα and Lyα emission from the same slit position and at the same epoch. Consequently, we find clear evidence that, unlike Hα, Lyα is reflected from the debris by resonant scattering, In addition to emission that we can clearly attribute to the surface of the reverse shock, we also measure comparable emission, in both Hα and Lyα, that appears to emerge from supernova debris interior to the surface. New observations taken through slits positioned slightly eastward and westward of a central slit show a departure from cylindrical symmetry in the Hα surface emission. Using a combination of old and new observations, we construct a light curve of the total Hα flux, F, from the reverse shock, which has increased by a factor of ∼4 over about 8 yr. However, due to large systematic uncertainties, we are unable to discern between the two limiting behaviors of the flux: F ∝ t (self-similar expansion) and F ∝ t 5 (halting of the reverse shock). Such a determination is important for constraining the rate of hydrogen atoms crossing the shock, which is relevant to the question of whether the reverse shock emission will vanish in ≳7 yr. Future deep, low- or moderate-resolution spectra are essential for accomplishing this task. © 2006. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectCircumstellar Matteren_US
dc.subjectShock Wavesen_US
dc.subjectSupernova Remnantsen_US
dc.subjectSupernovae: Individual (Sn 1987A)en_US
dc.titleEvolution of the reverse shock emission from SNR 1987Aen_US
dc.typeArticleen_US
dc.identifier.emailPun, CSJ: jcspun@hkucc.hku.hken_US
dc.identifier.authorityPun, CSJ=rp00772en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/503896en_US
dc.identifier.scopuseid_2-s2.0-33846478255en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33846478255&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume644en_US
dc.identifier.issue2 IIen_US
dc.identifier.spage959en_US
dc.identifier.epage970en_US
dc.identifier.isiWOS:000238340100027-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHeng, K=23989037500en_US
dc.identifier.scopusauthoridMcCray, R=35954431900en_US
dc.identifier.scopusauthoridZhekov, SA=6701727178en_US
dc.identifier.scopusauthoridChallis, PM=7004555495en_US
dc.identifier.scopusauthoridChevalier, RA=7101871369en_US
dc.identifier.scopusauthoridCrotts, APS=35241689000en_US
dc.identifier.scopusauthoridFransson, C=7004051800en_US
dc.identifier.scopusauthoridGarnavich, P=7006524172en_US
dc.identifier.scopusauthoridKirshner, RP=35277140000en_US
dc.identifier.scopusauthoridLawrence, SS=7202646485en_US
dc.identifier.scopusauthoridLundqvist, P=7004499555en_US
dc.identifier.scopusauthoridPanagia, N=35400629400en_US
dc.identifier.scopusauthoridPun, CSJ=7003931846en_US
dc.identifier.scopusauthoridSmith, N=7403172437en_US
dc.identifier.scopusauthoridSollerman, J=6603947073en_US
dc.identifier.scopusauthoridWang, L=52864791500en_US

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