E-viri
Recenzirano
Odprti dostop
-
Perley, Daniel A.; Sollerman, Jesper; Schulze, Steve; Yao, Yuhan; Fremling, Christoffer; Gal-Yam, Avishay; Ho, Anna Y. Q.; Yang, Yi; Kool, Erik C.; Irani, Ido; Yan, Lin; Andreoni, Igor; Baade, Dietrich; Bellm, Eric C.; Brink, Thomas G.; Chen, Ting-Wan; Cikota, Aleksandar; Coughlin, Michael W.; Dahiwale, Aishwarya; Dekany, Richard; Duev, Dmitry A.; Filippenko, Alexei V.; Hoeflich, Peter; Kasliwal, Mansi M.; Kulkarni, S. R.; Lunnan, Ragnhild; Masci, Frank J.; Maund, Justyn R.; Medford, Michael S.; Riddle, Reed; Rosnet, Philippe; Shupe, David L.; Strotjohann, Nora Linn; Tzanidakis, Anastasios; Zheng, WeiKang
The Astrophysical journal, 03/2022, Letnik: 927, Številka: 2Journal Article
Abstract We present observations of SN 2021csp, the second example of a newly identified type of supernova (SN) hallmarked by strong, narrow, P Cygni carbon features at early times (Type Icn). The SN appears as a fast and luminous blue transient at early times, reaching a peak absolute magnitude of −20 within 3 days due to strong interaction between fast SN ejecta ( v ≈ 30,000 km s −1 ) and a massive, dense, fast-moving C/O wind shed by the WC-like progenitor months before explosion. The narrow-line features disappear from the spectrum 10–20 days after explosion and are replaced by a blue continuum dominated by broad Fe features, reminiscent of Type Ibn and IIn supernovae and indicative of weaker interaction with more extended H/He-poor material. The transient then abruptly fades ∼60 days post-explosion when interaction ceases. Deep limits at later phases suggest minimal heavy-element nucleosynthesis, a low ejecta mass, or both, and imply an origin distinct from that of classical Type Ic SNe. We place SN 2021csp in context with other fast-evolving interacting transients, and discuss various progenitor scenarios: an ultrastripped progenitor star, a pulsational pair-instability eruption, or a jet-driven fallback SN from a Wolf–Rayet (W-R) star. The fallback scenario would naturally explain the similarity between these events and radio-loud fast transients, and suggests a picture in which most stars massive enough to undergo a W-R phase collapse directly to black holes at the end of their lives.
Avtor
![loading ... loading ...](themes/default/img/ajax-loading.gif)
Vnos na polico
Trajna povezava
- URL:
Faktor vpliva
Dostop do baze podatkov JCR je dovoljen samo uporabnikom iz Slovenije. Vaš trenutni IP-naslov ni na seznamu dovoljenih za dostop, zato je potrebna avtentikacija z ustreznim računom AAI.
Leto | Faktor vpliva | Izdaja | Kategorija | Razvrstitev | ||||
---|---|---|---|---|---|---|---|---|
JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
Baze podatkov, v katerih je revija indeksirana
Ime baze podatkov | Področje | Leto |
---|
Povezave do osebnih bibliografij avtorjev | Povezave do podatkov o raziskovalcih v sistemu SICRIS |
---|
Vir: Osebne bibliografije
in: SICRIS
To gradivo vam je dostopno v celotnem besedilu. Če kljub temu želite naročiti gradivo, kliknite gumb Nadaljuj.