TY - JOUR
T1 - SNR G292.0+1.8
T2 - A Remnant of a Low-mass Progenitor Stripped-envelope Supernova
AU - Temim, Tea
AU - Slane, Patrick
AU - Raymond, John C.
AU - Patnaude, Daniel
AU - Murray, Emily
AU - Ghavamian, Parviz
AU - Renzo, Mathieu
AU - Jacovich, Taylor
N1 - Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/6/1
Y1 - 2022/6/1
N2 - We present a study of the Galactic supernova remnant (SNR) G292.0+1.8, a classic example of a core-collapse SNR that contains oxygen-rich ejecta, circumstellar material, a rapidly moving pulsar, and a pulsar wind nebula (PWN). We use hydrodynamic simulations of the remnant's evolution to show that the SNR reverse shock is interacting with the PWN and has most likely shocked the majority of the supernova ejecta. In our models, such a scenario requires a total ejecta mass of ≲3 M ⊙ and implies that there is no significant quantity of cold ejecta in the interior of the reverse shock. In light of these results, we compare the estimated elemental masses and abundance ratios in the reverse-shocked ejecta to nucleosynthesis models, and further conclude that they are consistent with a progenitor star with an initial mass of 12-16 M ⊙. We conclude that the progenitor of G292.0+1.8 was likely a relatively low-mass star that experienced significant mass loss through a binary interaction and would have produced a stripped-envelope supernova explosion. We also argue that the region known as the "spur"in G292.0+1.8 arises as a result of the pulsar's motion through the supernova ejecta, and that its dynamical properties may suggest a line-of-sight component to the pulsar's velocity, leading to a total space velocity of ∼600 km s-1 and implying a significant natal kick. Finally, we discuss binary mass-loss scenarios relevant to G292.0+1.8 and their implications for the binary companion properties and future searches.
AB - We present a study of the Galactic supernova remnant (SNR) G292.0+1.8, a classic example of a core-collapse SNR that contains oxygen-rich ejecta, circumstellar material, a rapidly moving pulsar, and a pulsar wind nebula (PWN). We use hydrodynamic simulations of the remnant's evolution to show that the SNR reverse shock is interacting with the PWN and has most likely shocked the majority of the supernova ejecta. In our models, such a scenario requires a total ejecta mass of ≲3 M ⊙ and implies that there is no significant quantity of cold ejecta in the interior of the reverse shock. In light of these results, we compare the estimated elemental masses and abundance ratios in the reverse-shocked ejecta to nucleosynthesis models, and further conclude that they are consistent with a progenitor star with an initial mass of 12-16 M ⊙. We conclude that the progenitor of G292.0+1.8 was likely a relatively low-mass star that experienced significant mass loss through a binary interaction and would have produced a stripped-envelope supernova explosion. We also argue that the region known as the "spur"in G292.0+1.8 arises as a result of the pulsar's motion through the supernova ejecta, and that its dynamical properties may suggest a line-of-sight component to the pulsar's velocity, leading to a total space velocity of ∼600 km s-1 and implying a significant natal kick. Finally, we discuss binary mass-loss scenarios relevant to G292.0+1.8 and their implications for the binary companion properties and future searches.
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U2 - 10.3847/1538-4357/ac6bf4
DO - 10.3847/1538-4357/ac6bf4
M3 - Article
AN - SCOPUS:85132826422
SN - 0004-637X
VL - 932
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 26
ER -