Аннотация
The discovery of 150 - 300 M$_ødot$ stars in the Local Group and
pair-instability supernova (PI SN) candidates at low redshifts has excited
interest in this exotic explosion mechanism and poses serious challenges to
current theories of galactic star formation. Realistic light curves for PI SNe
at near-solar metallicities are key to identifying and properly interpreting
these events as more are found. We have modeled the evolution and explosions of
$Z \sim$ 0.1 - 0.4 $Z_ødot$ PI SN progenitors. These stars must be 150 - 500
M$_ødot$ at birth because they lose up to 80% of their mass to strong
line-driven winds and explode as bare He cores. Their light curves and spectra
are quite different from those of Population III pair-instability explosions,
which therefore cannot be used as templates for low-redshift events. Our
numerical models show that non-zero metallicity PI SNe are generally dimmer
than Population III explosions but can still be detected at $z \sim$ 0.1 - 1 by
the new supernova factories. They also reveal that pair-instability explosions
can masquerade as dim, short-duration supernovae, and that under the right
conditions they could be hidden in a wide variety of supernova classes. We also
report for the first time that some PI SNe can create black holes with masses
of $\sim$ 100 M$_ødot$.
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