Optical, Ultraviolet, and Infrared Observations of SN 1993J

Filippenko, A. V.; Matheson, T.

doi:10.1007/3-540-26633-x_5

Cited by 6 publications

(5 citation statements)

References 61 publications

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“…The listed velocity of IC 49 is 4562 km s −1 . Phillips (1991b) classified it as a Type Ib; this was confirmed by Filippenko & Matheson (1991b), despite an earlier misidentification as a Type II (Filippenko & Matheson 1991a). Our spectra (Figure 11), although noisy, show distinctly the He I series.…”

Section: Description Of Individual Supernovaementioning

confidence: 50%

Optical Spectroscopy of Type I[CLC]b[/CLC]/[CLC]c[/CLC] Supernovae

Matheson¹,

Filippenko²,

Li³

et al. 2001

The Astronomical Journal

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210

301

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We present 84 spectra of Type Ib/c and Type IIb supernovae (SNe), describing the individual SNe in detail. The relative depths of the helium absorption lines in the spectra of the SNe Ib appear to provide a measurement of the temporal evolution of the SN, with He I λ5876 and He I λ7065 growing in strength relative to He I λ6678 over time. Light curves for three of the SNe Ib provide a sequence for correlating the heliumline strengths. We find that some SNe Ic show evidence for weak helium absorption, but most do not. Aside from the presence or absence of the helium lines, there are other spectroscopic differences between SNe Ib and SNe Ic. On average, the O I λ7774 line is stronger in SNe Ic than in SNe Ib. In addition, the SNe Ic have distinctly broader emission lines at late times, indicating either a consistently larger explosion energy and/or lower envelope mass for SNe Ic than for SNe Ib. While SNe Ib appear to be basically homogeneous, the SNe Ic are quite heterogeneous in their spectroscopic characteristics. Three SNe Ic that may have been associated with gamma-ray bursts are also discussed; two of these have clearly peculiar spectra, while the third seems fairly typical.

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Section: Description Of Individual Supernovaementioning

confidence: 50%

Optical Spectroscopy of Type I[CLC]b[/CLC]/[CLC]c[/CLC] Supernovae

Matheson¹,

Filippenko²,

Li³

et al. 2001

The Astronomical Journal

Self Cite

210

301

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“…However, the spectra quickly evolved to show He I lines associated with the Type Ib class (Filippenko et al 1993b), thus acquiring the transitional classification Type IIb (Filippenko et al 1993c) anticipated by Woosley et al (1987). The relatively isolated location and nearby distance of SN 1993J has enabled close monitoring of emission in the X-ray (Zimmermann et al 1994;Suzuki & Nomoto 1995;Chandra et al 2009) radio (Bartel et al 1994;van Dyk et al 1994;Bartel et al 2000;Weiler et al 2007), and optical (Woosley et al 1994;Filippenko et al 1994;Matheson et al 2000a,b;Filippenko & Matheson 2003;Fransson et al 2005).…”

Section: Sn 1980kmentioning

confidence: 99%

Late-Time Optical Emission From Core-Collapse Supernovae

Milisavljevic

Fesen

Chevalier

et al. 2012

ApJ

102

113

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Ground-based optical spectra and Hubble Space Telescope images of ten core-collapse supernovae (CCSNe) obtained several years to decades after outburst are analyzed with the aim of understanding the general properties of their late-time emissions. New observations of SN 1957D, 1970G, 1980K, and 1993J are included as part of the study. Blueshifted line emissions in oxygen and/or hydrogen with conspicuous line substructure are a common and long-lasting phenomenon in the late-time spectra. Followed through multiple epochs, changes in the relative strengths and velocity widths of the emission lines are consistent with expectations for emissions produced by interaction between SN ejecta and the progenitor star's circumstellar material. The most distinct trend is an increase in the strength of [O III]/([O I]+[O II]) with age, and a decline in Hα/([O I]+[O II])which is broadly consistent with the view that the reverse shock has passed through the H envelope of the ejecta in many of these objects. We also present a spatially integrated spectrum of the young Galactic supernova remnant Cassiopeia A (Cas A). Similarities observed between the emission line profiles of the ≈330 yr old Cas A remnant and decades old CCSNe suggest that observed emission line asymmetry in evolved CCSN spectra may be associated with dust in the ejecta, and that minor peak substructure typically interpreted as 'clumps' or 'blobs' of ejecta may instead be linked with large-scale rings of SN debris.

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“…The final SNe of WR stars are expected to be of Type Ib (no hydrogen observed in spectrum) or Ic (no hydrogen or helium). The observation of SNe for which the type changed from II to Ib over time (Filippenko & Matheson 1993) and detection of helium in Type Ic supernovae (Matheson et al 2000) suggests that there is probably a continuum between all three types determined by the composition of the outer layers of the star. The properties of the SN of a WR star (if indeed one occurs) will depend critically on the final mass of the star and on its composition.…”

Section: Comparison With Observationsmentioning

confidence: 99%

Chemical enrichment by Wolf-Rayet stars: non-solar metallicities

Dray¹,

Tout²

2003

Monthly Notices of the Royal Astronomical Society

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Following on from our recent Paper I, we present theoretical models of Wolf–Rayet (WR) stars for non‐solar metallicities from Z= 0.03 to 0.0001 by mass fraction with different mass‐loss rate assumptions. We find that some single WR stars may still form even at the lowest metallicities, but whether this occurs or not depends critically on the upper cut‐off point of the initial mass function used. As at solar metallicity, a population of binaries is required to fully reproduce WR star observations. For most scenarios, these binaries dominate the low‐metallicity WR population but probably not the enrichment. We find comparable carbon enrichment from single WR stars to that from asymptotic giant branch stars at all metallicities for which data are available, but which of them is the dominant source of carbon depends strongly on the set of asymptotic giant branch yields adopted and the assumed initial mass function. We find an increase in carbon enrichment with increasing metallicity but a decrease in oxygen enrichment, as confirmed by observation.

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Optical, Ultraviolet, and Infrared Observations of SN 1993J

Cited by 6 publications

References 61 publications

Optical Spectroscopy of Type I[CLC]b[/CLC]/[CLC]c[/CLC] Supernovae

Optical Spectroscopy of Type I[CLC]b[/CLC]/[CLC]c[/CLC] Supernovae

Late-Time Optical Emission From Core-Collapse Supernovae

Chemical enrichment by Wolf-Rayet stars: non-solar metallicities

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