1995
DOI: 10.1086/309714
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The Presupernova H [CSC]ii[/CSC] Region around SN 1987A

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Cited by 162 publications
(216 citation statements)
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“…We also assumed n e ∼ 1.5n H for the ring abundances (e.g., Masai & Nomoto 1994). Considering our simple modeling and the embedded uncertainty in the assumed geometry, the derived range of the electron density is in good agreement with the previously suggested values for the preshock HII region (Chevalier & Dwarkadas 1995;Borkowski et al 1997b;Lundqvist 1999), assuming density enhancement by a factor of 4 at the front of a strong adiabatic shock.…”
Section: Spectrum and Lightcurvesupporting
confidence: 88%
“…We also assumed n e ∼ 1.5n H for the ring abundances (e.g., Masai & Nomoto 1994). Considering our simple modeling and the embedded uncertainty in the assumed geometry, the derived range of the electron density is in good agreement with the previously suggested values for the preshock HII region (Chevalier & Dwarkadas 1995;Borkowski et al 1997b;Lundqvist 1999), assuming density enhancement by a factor of 4 at the front of a strong adiabatic shock.…”
Section: Spectrum and Lightcurvesupporting
confidence: 88%
“…In particular, model Ðts to superresolved images of the radio emission suggest that the source of the radio emission was expanding at only D2800 km s~1 in the period 1992È1995, much lower than the average speed of 35,000 km s~1 required between the time of explosion and the Ðrst imaging observations in 1992 (Gaensler et al 1997). While this expansion speed is not a direct measurement of the speed of the supernova shock, it clearly indicates that the shock had undergone a dramatic deceleration from its initial speed of greater than 50,000 km s~1 (Hanuschik & Dachs 1987), as would occur if the shock encountered a signiÐcant jump in the density of circumstellar material (Chevalier & Dwarkadas 1995 ;Borkowski et al 1997) associated with a dense H II region inside the circumstellar ring. The interpretation is also consistent with the observed soft X-ray emission from SN 1987A (Beuermann, Brandt, & Pietsch 1994 ;Gorenstein, Hughes, & Tucker 1994 ;Hasinger, Aschenbach, & 1996), Trumper though the X-ray evolution is relatively poorly sampled.…”
Section: Up To 1995mentioning
confidence: 86%
“…1997) which required a dramatic deceleration of the supernova shock at or prior to the onset of the second phase of radio emission. More detailed models for the radio emission (Du †y, Ball, & Kirk 1995, hereafter DBK95) and for the hydrodynamics of the interaction of the supernova ejecta with the CSM (e.g., Chevalier & Dwarkadas 1995 ;Borkowski, Blondin, & McCray 1997) all attribute the radio emission to the interaction of the SN shock with a density jump in the CSM. The implied radius of the circumstellar density jump responsible for the reappearance of the radio emission is smaller than that of the dense ring surrounding SN 1987A (Jakobsen et al 1991 ;Plait et al 1995 ;Sonneborn et al 1997).…”
Section: Introductionmentioning
confidence: 99%
“…This interaction was predicted (Luo & McCray 1991;Luo et al 1994;Chevalier & Dwarkadas 1995;Borkowski et al 1997) shortly after the discovery of the circumstellar ring. It began about a decade after the outburst, with the discovery of the first of many "hot spots" Michael et al 2000;Pun et al 2002).…”
Section: Introductionmentioning
confidence: 91%