Untitled

Burenin, V. V.

doi:10.1023/a:1014837506522

Cited by 1 publication

(2 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The curves show the best‐fitting model in X‐ray (1 keV), optical ( R ‐band) and radio (8.5 GHz). Data sources (all 2003): X‐ray –Marshall & Swank (2003); Marshall, Markwardt & Swank (2003); Tiengo et al (2003a,b); Optical/IR –Bikmaev et al (2003); Burenin et al (2003a,b); Fitzgerald & Orosz (2003); Gorosabel et al (2003); Ibrahimov et al (2003a,b); Lamb et al (2003); Lee et al (2003); Price et al (2003a,b,c); Simoncelli et al (2003); Stanek et al (2003); Susuki et al (2003); Testa et al (2003); Uemura et al (2003); Zharikov et al (2003); Submillimetre –Hoge et al (2003); Radio –Berger et al (2003a,b); Bloom et al (2003); Finkelstein, Ipatov & Gnedin (2003); Kuno, Sato & Nakanishi (2003); Pooley et al (2003a,b); Rao et al (2003a,b); Trushkin et al (2003).…”

Section: Multifrequency Datamentioning

confidence: 99%

“…Note that the earliest X‐ray point is derived from the combination of the first two RXTE observations (see Table 2). Data sources (all 2003): X‐ray –Marshall & Swank (2003); Marshall et al (2003); Tiengo et al (2003a,b); Optical –Burenin et al (2003a,b); Fitzgerald & Orosz (2003); Ibrahimov et al (2003a,b); Lamb et al (2003); Lee et al (2003); Simoncelli et al (2003); Testa et al (2003); Zharikov et al (2003).…”

Section: Multifrequency Datamentioning

confidence: 99%

See 1 more Smart Citation

The X-ray, optical and radio evolution of the GRB 030329 afterglow and the associated SN2003dh

Willingale¹,

Osborne

O’Brien

et al. 2004

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Extensive X‐ray, optical and radio observations of the bright afterglow of the gamma‐ray burst GRB 030329 are used to construct the multifrequency evolution the event. The data are fitted using the standard fireball shock model to provide estimates of the initial energy, ɛ= 6.8 × 1052 erg sr−1, the density of the ambient medium, n0= 1 cm−3, the electron and magnetic energy density fractions, εe= 0.24 and εB= 0.0017, the power‐law index of the relativistic electron spectrum, p= 2.25, and the opening angle of the jet, θj= 3°. Deviations from the standard model seen in the optical and radio are most likely attributable to the concurrent hypernova SN2003dh. Peaks at 0.23 and 1.7 d in the R‐band are much brighter than expected from a standard supernova (SN), and there is a large radio excess over the expected afterglow flux for t > 2 d. No deviation from the best‐fitting afterglow model is seen in the X‐ray decline, indicating that the excess optical and radio flux from 1–5 d arises from a later injection of slower electrons by the central engine.

show abstract