Circumstellar Emission from Type Ib and Ic Supernovae

By R. Chevalier, C. Fransson. 2006

253 citations recorded by the source corpus.

The presumed Wolf-Rayet star progenitors of Type Ib/c supernovae have fast, low-density winds, and the shock waves generated by the supernova interaction with the wind are not expected to be radiative at typical times of observation. The injected energy spectrum of radio-emitting electrons typically has an observed index p = 3, which is suggestive of acceleration in cosmic-ray-dominated shocks. The early, absorbed part of the radio light curves can be attributed to synchrotron self-absorption, which leads to constraints on the magnetic field in the emitting region and on the circumstellar density. The range of circumstellar densities inferred from the radio emission is somewhat broader than that for Galactic Wolf-Rayet stars, if similar efficiencies of synchrotron emission are assumed in the extragalactic supernovae. For the observed and expected ranges of circumstellar densities to roughly overlap, a high efficiency of magnetic field production in the shocked region is required (ϵB ≈ 0.1). For the expected densities around a Wolf-Rayet star, a nonthermal mechanism is generally required to explain the observed X-ray luminosities of Type Ib/c supernovae. Inverse Compton emission is a candidate for the emission, if the observations are near optical maximum. In other cases we suggest that the mechanism is X-ray synchrotron emission in a situation in which the shock wave is cosmic-ray-dominated so that the electron energy spectrum flattens at high energy. More comprehensive X-ray observations of a Type Ib/c supernova are needed to determine whether this suggestion is correct.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/679d6e1900a31cfd488fb803343de46711a5c242

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In Astronomy and Astrophysics

1. E. Berger
2. B. Metzger
3. Bing Zhang
4. E. Nakar
5. D. Maoz
6. Ryan Chornock
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8. A. Filippenko

In Nuclear and High Energy Physics

1. E. Berger
2. B. Metzger
3. D. Maoz
4. E. Nakar
5. F. Mannucci
6. T. Piran
7. Stephan Rosswog
8. A. Gal-yam

Citations in the corpus

• NONTHERMAL RADIATION OF YOUNG SUPERNOVA REMNANTS: THE CASE OF RX J1713.7−3946 (2010, result): “This is in agreement with calculations of quasi-parallel collisionless shocks (Zirakashvili 2007) and is supported by radio observations of young extragalactic Ib/c SNRs (Chevalier & Fransson 2006).”
• EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF Type Ia SUPERNOVA 2011fe (2012, methodology): “The coupling of mass to ejecta velocity is simply a function of the bulk explosion energy (E51, in units of 1051 erg) and ejecta mass (Mej; Berger et al. 2002; Chevalier & Fransson 2006).”
• THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES (2010, background): “1986; Chevalier 1998; Bergeret al. 2003; Chevalier & Fransson 2006; Soderberg 2007), SNe Ibc are now recognized as core-collapse explosions of massive stars10 stripped of their hydrogen (and often helium) layers (Eliaset al. , 1985; Filippenko & Sargent, 1985; Wheeler & Levreault, 1985; Uomoto, &…”
• Cosmic ray acceleration and escape from supernova remnants (2013, background): “Initial expansion velocities of very young SNR can reach 30, 000 km s−1 (Manchester et al 2002) or possibly higher for some types of SN (Chevalier & Fransson 2006).”
• Observational Clues to the Progenitors of Type Ia Supernovae (2013, methodology): “The physics and signatures of such interaction have been computed by Chevalier (1982, 1998) and Chevalier & Fransson (2006); see Chomiuk et al. (2012b) and Margutti et al. (2012), for recent generalizations.”
• GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, unknown): “Using the convention from supernovae, we have A∗ ≡ Ṁ/(4πvw)/5× 1011 gmcm−1 (Chevalier & Fransson 2006).”
• SN 2008ha: AN EXTREMELY LOW LUMINOSITY AND EXCEPTIONALLY LOW ENERGY SUPERNOVA (2009, background): “Several SNe Ia have been measured to have no X-ray emission at early times with limits an order of magnitude deeper (Hughes et al. 2007), while SNe Ic typically have X-ray luminosities of 1037–1039 ergs s−1 (Chevalier & Fransson 2006); therefore, our X-ray limits are not particularly constraining.”
• The electromagnetic signals of compact binary mergers (2012, methodology): “The success of this model in explaining the detailed observations of radio Ib/c SNe (e.g. Chevalier 1998; Soderberg et al. 2005; Chevalier & Fransson 2006) allows us to employ the same microphysics here.”
• On the Progenitors of Type Ia Supernovae (2018, unknown): “(5) The relativistic electrons that can produce radio synchrotron emission can also upscatter photons emitted by the explosion to produce inverse Compton x-ray radiation (e.g., Chevalier & Fransson 2006).”
• An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients (2018, methodology): “…~ – needed to explain the luminosity of the radio emission of AT 2018cow are similar to those inferred in previous radio-bright SNe (e.g., SN 2003L; Chevalier & Fransson 2006), but substantially smaller than the values A A105 ~ needed on smaller radial scales to explain the early optical peak if…”
• DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn (2013, methodology): “Using the explosion date determined in the optical data, we find a shock wave velocity of 2.7×104 km s−1, 5CARMA program c1127, PI Horesh 6JVLA program 13A-531, PI Horesh 7ATCA program C2707, PI Hancock which is typical for SNe Ib/c (Chevalier & Fransson 2006).”
• The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. V. Rising X-Ray Emission from an Off-axis Jet (2017, background): “Mildly relativistic outflows with similar Γ and Ek that are found in shocks from supernovae (SN) with fast ejecta (i.e., relativistic SNe) are well described by ~p 3 (e.g., Chevalier & Fransson 2006; Soderberg et al. 2010; Chakraborti et al. 2015).”