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Article: Modeling the Hubble Space Telescope ultraviolet and optical spectrum of spot 1 on the circumstellar ring of SN 1987A

TitleModeling the Hubble Space Telescope ultraviolet and optical spectrum of spot 1 on the circumstellar ring of SN 1987A
Authors
KeywordsCircumstellar matter
Supernova remnants
Supernovae: individual (SN 1987A)
Issue Date2002
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2002, v. 572 n. 2 I, p. 906-931 How to Cite?
AbstractWe report and interpret Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) long-slit observations of the optical and ultraviolet (1150-10270 Å) emission line spectra of the rapidly brightening spot 1 on the equatorial ring of SN 1987A between 1997 September and 1999 October (days 3869-4606 after outburst). The emission is caused by radiative shocks created where the supernova blast wave strikes dense gas protruding inward from the equatorial ring. We measure and tabulate line identifications, fluxes, and, in some cases, line widths and shifts. We compute flux correction factors to account for substantial interstellar line absorption of several emission lines. Nebular analysis shows that optical emission lines come from a region of cool (T e ≈ 10 4 K) and dense (n e ≈ 10 6 cm -3) gas in the compressed photoionized layer behind the radiative shock. The observed line widths indicate that only shocks with shock velocities V s < 250 km s -1 have become radiative, while line ratios indicate that much of the emission must have come from yet slower (V s ≲ 135 km s -1) shocks. Such slow shocks can be present only if the protrusion has atomic density n ≳ 3 × 10 4 cm -3, somewhat higher than that of the circumstellar ring. We are able to fit the UV fluxes with an idealized radiative shock model consisting of two shocks (V s = 135 and 250 km s -1). The observed UV flux increase with time can be explained by the increase in shock surface areas as the blast wave overtakes more of the protrusion. The observed flux ratios of optical to highly ionized UV lines are greater by a factor of ∼2-3 than predictions from the radiative shock models, and we discuss the possible causes. We also present models for the observed Ha line widths and profiles, which suggest that a chaotic flow exists in the photoionized regions of these shocks. We discuss what can be learned with future observations of all the spots present on the equatorial ring.
Persistent Identifierhttp://hdl.handle.net/10722/43381
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorPun, CSJen_HK
dc.contributor.authorMichael, Een_HK
dc.contributor.authorZhekov, SAen_HK
dc.contributor.authorMcCray, Ren_HK
dc.contributor.authorGarnavich, PMen_HK
dc.contributor.authorChallis, PMen_HK
dc.contributor.authorKirshner, RPen_HK
dc.contributor.authorBaron, Een_HK
dc.contributor.authorBranch, Den_HK
dc.contributor.authorChevalier, RAen_HK
dc.contributor.authorFilippenko, AVen_HK
dc.contributor.authorFransson, Cen_HK
dc.contributor.authorLeibundgut, Ben_HK
dc.contributor.authorLundqvist, Pen_HK
dc.contributor.authorPanagia, Nen_HK
dc.contributor.authorPhillips, MMen_HK
dc.contributor.authorSchmidt, Ben_HK
dc.contributor.authorSonneborn, Gen_HK
dc.contributor.authorSuntzeff, NBen_HK
dc.contributor.authorWang, Len_HK
dc.contributor.authorCraig Wheeler, Jen_HK
dc.date.accessioned2007-03-23T04:44:38Z-
dc.date.available2007-03-23T04:44:38Z-
dc.date.issued2002en_HK
dc.identifier.citationAstrophysical Journal Letters, 2002, v. 572 n. 2 I, p. 906-931en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43381-
dc.description.abstractWe report and interpret Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) long-slit observations of the optical and ultraviolet (1150-10270 Å) emission line spectra of the rapidly brightening spot 1 on the equatorial ring of SN 1987A between 1997 September and 1999 October (days 3869-4606 after outburst). The emission is caused by radiative shocks created where the supernova blast wave strikes dense gas protruding inward from the equatorial ring. We measure and tabulate line identifications, fluxes, and, in some cases, line widths and shifts. We compute flux correction factors to account for substantial interstellar line absorption of several emission lines. Nebular analysis shows that optical emission lines come from a region of cool (T e ≈ 10 4 K) and dense (n e ≈ 10 6 cm -3) gas in the compressed photoionized layer behind the radiative shock. The observed line widths indicate that only shocks with shock velocities V s < 250 km s -1 have become radiative, while line ratios indicate that much of the emission must have come from yet slower (V s ≲ 135 km s -1) shocks. Such slow shocks can be present only if the protrusion has atomic density n ≳ 3 × 10 4 cm -3, somewhat higher than that of the circumstellar ring. We are able to fit the UV fluxes with an idealized radiative shock model consisting of two shocks (V s = 135 and 250 km s -1). The observed UV flux increase with time can be explained by the increase in shock surface areas as the blast wave overtakes more of the protrusion. The observed flux ratios of optical to highly ionized UV lines are greater by a factor of ∼2-3 than predictions from the radiative shock models, and we discuss the possible causes. We also present models for the observed Ha line widths and profiles, which suggest that a chaotic flow exists in the photoionized regions of these shocks. We discuss what can be learned with future observations of all the spots present on the equatorial ring.en_HK
dc.format.extent2157334 bytes-
dc.format.extent26624 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypeapplication/msword-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectCircumstellar matteren_HK
dc.subjectSupernova remnantsen_HK
dc.subjectSupernovae: individual (SN 1987A)en_HK
dc.titleModeling the Hubble Space Telescope ultraviolet and optical spectrum of spot 1 on the circumstellar ring of SN 1987Aen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=572&issue=2 pt 1&spage=906&epage=931&date=2002&atitle=Modeling+the+Hubble+Space+Telescope+Ultraviolet+and+Optical+Spectrum+of+Spot+1+on+the+Circumstellar+Ring+of+SN+1987Aen_HK
dc.identifier.emailPun, CSJ: jcspun@hkucc.hku.hken_HK
dc.identifier.authorityPun, CSJ=rp00772en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/340453en_HK
dc.identifier.scopuseid_2-s2.0-18244431141en_HK
dc.identifier.hkuros77071-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-18244431141&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume572en_HK
dc.identifier.issue2 Ien_HK
dc.identifier.spage906en_HK
dc.identifier.epage931en_HK
dc.identifier.isiWOS:000176071200018-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridPun, CSJ=7003931846en_HK
dc.identifier.scopusauthoridMichael, E=7004899413en_HK
dc.identifier.scopusauthoridZhekov, SA=6701727178en_HK
dc.identifier.scopusauthoridMcCray, R=35954431900en_HK
dc.identifier.scopusauthoridGarnavich, PM=7006524172en_HK
dc.identifier.scopusauthoridChallis, PM=7004555495en_HK
dc.identifier.scopusauthoridKirshner, RP=35277140000en_HK
dc.identifier.scopusauthoridBaron, E=7102558228en_HK
dc.identifier.scopusauthoridBranch, D=7103272488en_HK
dc.identifier.scopusauthoridChevalier, RA=7101871369en_HK
dc.identifier.scopusauthoridFilippenko, AV=34568722000en_HK
dc.identifier.scopusauthoridFransson, C=7004051800en_HK
dc.identifier.scopusauthoridLeibundgut, B=7007116593en_HK
dc.identifier.scopusauthoridLundqvist, P=7004499555en_HK
dc.identifier.scopusauthoridPanagia, N=35400629400en_HK
dc.identifier.scopusauthoridPhillips, MM=7402770160en_HK
dc.identifier.scopusauthoridSchmidt, B=7402828523en_HK
dc.identifier.scopusauthoridSonneborn, G=7006137500en_HK
dc.identifier.scopusauthoridSuntzeff, NB=7006255654en_HK
dc.identifier.scopusauthoridWang, L=45361626600en_HK
dc.identifier.scopusauthoridCraig Wheeler, J=7403110438en_HK

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