Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
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Linear stability analysis and non-linear hydrodynamical simulations link the stochastic low-frequency variability of ε Ori to strange-mode instabilities that excite finite-amplitude pulsations.
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Type Ib Supernovae are bluer than Type Ic Supernovae
Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
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On the origin of variability in $\alpha$ Cygni variable $\epsilon$ Ori (HD 37128) using TESS observations and modelling
Linear stability analysis and non-linear hydrodynamical simulations link the stochastic low-frequency variability of ε Ori to strange-mode instabilities that excite finite-amplitude pulsations.