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Titolo:
The metamorphosis of SN 1998bw
Autore:
Patat, F; Cappellaro, E; Danziger, J; Mazzali, PA; Sollerman, J; Augusteijn, T; Brewer, J; Doublier, V; Gonzalez, JF; Hainaut, O; Lidman, C; Leibundgut, B; Nomoto, K; Nakamura, T; Spyromilio, J; Rizzi, L; Turatto, M; Walsh, J; Galama, TJ; van Paradijs, J; Kouveliotou, C; Vreeswijk, PM; Frontera, F; Masetti, N; Palazzi, E; Pian, E;
Indirizzi:
European So Observ, D-85748 Garching, Germany European So Observ Garching Germany D-85748 v, D-85748 Garching, Germany Osservatorio Astron Padova, I-35122 Padua, Italy Osservatorio Astron Padova Padua Italy I-35122 ova, I-35122 Padua, Italy Osservatorio Astron Trieste, I-34131 Trieste, Italy Osservatorio Astron Trieste Trieste Italy I-34131 I-34131 Trieste, Italy Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan Univ Tokyo Tokyo Japan 1130033 Universe, Bunkyo Ku, Tokyo 1130033, Japan Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan Univ Tokyo Tokyo Japan 1130033 t Astron, Bunkyo Ku, Tokyo 1130033, Japan Stockholm Observ, S-13336 Saltsjobaden, Sweden Stockholm Observ Saltsjobaden Sweden S-13336 -13336 Saltsjobaden, Sweden European So Observ, Santiago 19, Chile European So Observ Santiago Chile19 opean So Observ, Santiago 19, Chile Ecole Normale Super Lyon, Ctr Rech Astron Lyon, CNRS, UMR 5574, F-69364 Lyon 07, France Ecole Normale Super Lyon Lyon France 07 MR 5574, F-69364 Lyon 07, France Univ Amsterdam, Astron Inst Anton Pannekoek, CHEAF, NL-1098 SJ Amsterdam, Netherlands Univ Amsterdam Amsterdam Netherlands NL-1098 SJ J Amsterdam, Netherlands Univ Alabama, Dept Phys, Huntsville, AL 35899 USA Univ Alabama HuntsvilleAL USA 35899 Dept Phys, Huntsville, AL 35899 USA NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA NASA Huntsville AL USA 35812 l Space Flight Ctr, Huntsville, AL 35812 USA CNR, Ist Tecnol & Studio Radiaz Extraterr, I-40126 Bologna, Italy CNR Bologna Italy I-40126 tudio Radiaz Extraterr, I-40126 Bologna, Italy
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 555, anno: 2001,
parte:, 1
pagine: 900 - 917
SICI:
0004-637X(20010710)555:2<900:TMOS1>2.0.ZU;2-Z
Fonte:
ISI
Lingua:
ENG
Soggetto:
GAMMA-RAY BURST; 25 APRIL 1998; IA SUPERNOVA 1994D; IB SUPERNOVAE; LIGHT CURVES; SPECTRAL EVOLUTION; UBVRI PHOTOMETRY; HYPERNOVA MODEL; STANDARD STARS; IC SUPERNOVAE;
Keywords:
gamma rays : bursts; supernovae : general; supernovae : individual (SN 1998bw);
Tipo documento:
Review
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
107
Recensione:
Indirizzi per estratti:
Indirizzo: Patat, F European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany European So Observ Karl Schwarzschild Str 2 Garching Germany D-85748
Citazione:
F. Patat et al., "The metamorphosis of SN 1998bw", ASTROPHYS J, 555(2), 2001, pp. 900-917

Abstract

We present and discuss the photometric and spectroscopic evolution of the peculiar SN 1998bw, associated with GRB 980425, through an analysis of optical and near-IR data collected at ESO-La Silla. The spectroscopic data, spanning the period from day -9 to day +376 (relative to B maximum), have shown that this supernova (SN) was unprecedented, although somewhat similar to SN 1997ef. Maximum expansion velocities as high as 3x10(4) km s(-1) to someextent mask its resemblance to other Type Ic SNe. At intermediate phases, between photospheric and fully nebular, the expansion velocities (similar to 10(4) km s(-1)) remained exceptionally high compared to those of other recorded core-collapse SNe at a similar phase. The mild linear polarization detected at early epochs suggests the presence of asymmetry in the emitting material. The degree of asymmetry, however, cannot be decoded from these measurements alone. The He I 1.083 and 2.058 mum lines are identified, and Heis suggested to lie in an outer region of the envelope. The temporal behavior of the fluxes and profiles of emission lines of Mg I] lambda 4571, [O I] lambda lambda 6300, 6364, and a feature ascribed to Fe are traced to stimulate future modeling work. The uniqueness of SN 1998bw became less obviousonce it entered the fully nebular phase (after 1 yr), when it was very similar to other Type Ib/c-IIb objects, such as the Type Ib SN 1996N and the Type IIb SN 1993J, even though SN 1998bw was 1.4 mag brighter than SN 1993J and 3 mag brighter than SN 1996N at a comparable phase. The late-phase optical photometry, which extends up to 403 days after B maximum, shows that the SN luminosity declined exponentially but substantially faster than the decay rate of Co-56. The ultraviolet-optical-infrared bolometric light curve,constructed using all available optical data and the early JHK photometry presented in this work, shows a slight flattening starting on about day +300. Since no clear evidence of ejecta-wind interaction was found in the late-time spectroscopy (see also the work of Sollerman and coworkers), this maybe due to the contribution of the positrons since most gamma -rays escape thermalization at this phase. A contribution from the superposed H II region cannot, however, be excluded.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 26/09/17 alle ore 09:27:58