GRB 060218: A Relativistic Supernova Shock Breakout

By E. Waxman, P. Mészáros, S. Campana. 2007

165 citations recorded by the source corpus.

We show that the prompt and afterglow X-ray emission of GRB 060218, as well as its early (t ≲ 1 day) optical-UV emission, can be explained by a model in which a radiation-mediated shock propagates outward from a compact progenitor star into a dense wind. The prompt thermal X-ray emission is produced in this model when the mildly relativistic shock, β ≈ 0.85, carrying a few times 1049 erg, reaches the wind (Thomson) photosphere, where the postshock thermal radiation is released and the shock becomes collisionless. Adopting this interpretation of the thermal X-ray emission, we predict a subsequent X-ray afterglow, due to synchrotron emission and inverse Compton scattering of supernova UV photons by electrons accelerated in the collisionless shock. Early optical-UV emission is also predicted, due to the cooling of the outer δM ~ 10-3 M☉ envelope of the star, which was heated to high temperature during the shock passage. The observed X-ray afterglow and the early optical-UV emission are both consistent with those expected in this model. Detailed analysis of the early optical-UV emission may provide detailed constraints on the density distribution near the stellar surface.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e0cb38676c1d8f3a56cadf03d883916942c400cd

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Citations in the corpus

• Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “…the cocoon breaks out of the star, and feasibly leads to a different type of burst, which may resemble a low-luminosity GRB (Kulkarni et al. 1998; MacFadyen et al. 2001; Tan et al. 2001; Wang et al. 2007; Waxman et al. 2007; Katz et al. 2010; Bromberg et al. 2011; Nakar & Sari 2012; Nakar 2015).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, unknown): “References [58, 59] derived a BB radius of 5–8× 10(12) cm for GRB 060218; [65] found ≈8 × 10(11) cm for GRB 100316D; [41] found ≈7 × 10(13) cm for GRB 120422A; and [75] derived a radius of ≈9 × 10(13) cm for GRB 140606B.”
• ULTRAVIOLET LIGHT CURVES OF SUPERNOVAE WITH THE SWIFT ULTRAVIOLET/OPTICAL TELESCOPE (2009, background): “This first peak has been attributed to the shock breakout from a dense stellar wind (Campana et al. 2006; Blustin 2007; Waxman et al. 2007) or self-absorbed synchrotron radiation (Ghisellini et al. 2007).”
• THE EARLY UV/OPTICAL EMISSION FROM CORE-COLLAPSE SUPERNOVAE (2010, methodology): “(19) of Waxman et al. (2007) and eq.”
• Nearby Supernova Rates from the Lick Observatory Supernova Search. II. The Observed Luminosity Functions and Fractions of Supernovae in a Complete Sample (2010, background): “…SN IIb 1993J showed a double-peaked light curve (Richmond et al. 1994), with a very early first peak, which we now think is most likely due to black-body emission from the expanding and cooling shock-heated stellar envelope (e.g., Waxman et al. 2007), and the regular Ni56-powered main maximum.”
• FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, methodology): “…“X-ray flash” (XRF, see Heise et al. 2001) is used in the literature when referring to the high-energy event 060218, the transient 060218 was qualitatively different from classical X-ray flashes, in that it likely exhibited a shock breakout component (Campana et al. 2006; Waxman et al. 2007).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “…thermal break-out signal is expected to 40 precede the canonical γ-rays observed in GRBs with massive progenitors as the shock breaks through the stellar surface and exposes the hot shocked material (MacFadyen et al. 2001, Ramirez-Ruiz et al. 2002c, Waxman and Mészáros 2003, Waxman et al. 2007).”