Young Core-Collapse Supernova Remnants and Their Supernovae

By R. Chevalier. 2004

239 citations recorded by the source corpus.

Massive star supernovae can be divided into four categories, depending on the amount of mass loss from the progenitor star and the star's radius: red supergiant stars with most of the H envelope intact (SN IIP), stars with some H but most lost (IIL and IIb), stars with all H lost (Ib and Ic), and blue supergiant stars with a massive H envelope (SN 1987A-like). Various aspects of the immediate aftermath of the supernova are expected to develop in different ways, depending on the supernova category: mixing in the supernova, fallback on the central compact object, expansion of any pulsar wind nebula, interaction with circumstellar matter, and photoionization by shock breakout radiation. The observed properties of young supernova remnants allow many of them to be placed in one of the supernova categories; all the categories are represented except for the SN 1987A-like type. Of the remnants with central pulsars, the pulsar properties do not appear to be related to the supernova category. There is no evidence that the supernova categories form a mass sequence, as would be expected in a single-star scenario for the evolution. Models for young pulsar wind nebulae expanding into supernova ejecta indicate initial pulsar periods of 10-100 ms and approximate equipartition between particle and magnetic energies. Ages are obtained for pulsar nebulae, including an age of 2400 ± 500 yr for 3C 58, which is not consistent with an origin in SN 1181. There is no evidence that mass fallback plays a role in neutron star properties.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/42e96f5eaf7b55ab87cfa1dc188f4bf8dfc67c30

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Citations in the corpus

• NONTHERMAL RADIATION OF YOUNG SUPERNOVA REMNANTS: THE CASE OF RX J1713.7−3946 (2010, background): “Such small ejecta masses correspond to Ib/c or IIb core collapse supernova (Chevalier 2005).”
• A burst in a wind bubble and the impact on baryonic ejecta: high-energy gamma-ray flashes and afterglows from fast radio bursts and pulsar-driven supernova remnants (2016, methodology): “Then, we have (Chevalier 2005) Rnb ≈ ( 8Lsd,i 15Mext )1/2 { T 3/2 (T < Tsd) T 3/2 sd (T/Tsd) (T > Tsd) (11) The nebular emission is assumed to come from a uniform sphere expanding at a constant velocity.”
• NEUTRINO EMISSION FROM COOPER PAIRS AND MINIMAL COOLING OF NEUTRON STARS (2009, background): “Moreover, modeling of the energetics of the pulsar wind nebula and its expansion need an age of 2000-3000 yrs (Chevalier 2004, 2005) or even 2000-5000 yrs from the recent X-ray observations of Gotthelf, Helfand, & Newburgh (2007).”
• Supernova remnants: the X-ray perspective (2011, background): “…supernovae, and optical studies of potential progenitor stars confirm that their progenitors have initial masses in the ∼ 8− 17 M⊙ range, and that they explode in the red supergiant phase, while still having a substantial hydrogen envelope (see the discussions in Smartt, 2009; Chevalier, 2005).”
• The evolution and structure of pulsar wind nebulae (2006, background): “The detailed theoretical underpinning for these evolutionary phases is given in studies by Reynolds & Chevalier (1984), Chevalier (1998, 2005), Blondin, Chevalier & Frierson (2001), Bucciantini et al. (2003) and van der Swaluw et al. (2004).”
• Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, background): “2.3 PWN Evolution Theoretical expectations predict three main phases in the evolution of a PWN (Reynolds & Chevalier 1984; Chevalier 1998, 2005), governed in turn by: 1. the expansion of the PWN; 2. interaction of the PWN with the surrounding SNR; 3. the motion of the pulsar powering the PWN.”
• SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “A discussion about properties of SNRs produced by core collapse supernovae can be found in Chevalier (2005).”
• Circumstellar Emission from Type Ib and Ic Supernovae (2006, methodology): “We use results for the interaction in the thin-shell approximation, as described by Chevalier (2005).”