We investigate the evolution of Type Ib/c supernova ( SN Ib/c ) progenitors in close binary systems , using new evolutionary models that include the effects of rotation , with initial masses of 12 – 25 \mathrm { M _ { \odot } } for the primary components , and of single helium stars with initial masses of 2.8 – 20 \mathrm { M _ { \odot } } .
We find that , despite the impact of tidal interaction on the rotation of primary stars , the amount of angular momentum retained in the core at the presupernova stage in different binary model sequences converge to a value similar to those found in previous single star models .
This amount is large enough to produce millisecond pulsars , but too small to produce magnetars or long gamma-ray bursts .
We employ the most up-to-date estimate for the Wolf-Rayet mass loss rate , and its implications for SN Ib/c progenitors are discussed in detail .
In terms of stellar structure , SN Ib/c progenitors in binary systems at solar metallicity are predicted to have a wide range of final masses up to about 7 \mathrm { M _ { \odot } } , with helium envelopes of M _ { \mathrm { He } } \simeq 0.16 - 1.5 ~ { } \mathrm { M _ { \odot } } .
Our results indicate that , if the lack of helium lines in the spectra of SNe Ic were due to small amounts of helium ( e.g . M _ { \mathrm { He } } \lesssim 0.5 ) , the distribution of both initial and final masses of SN Ic progenitors should be bimodal .
Furthermore , we find that a thin hydrogen layer ( 0.001 ~ { } \mathrm { M _ { \odot } } \lesssim M _ { \mathrm { H } } \lesssim 0.01 ~ { } \mathrm { M _ { % \odot } } ) is expected to be present in many SN Ib progenitors at the presupernova stage .
We show that the presence of hydrogen , together with a rather thick helium envelope , can lead to a significant expansion of some SN Ib/c progenitors by the time of supernova explosion .
This may have important consequences for the shock break-out and supernova light curve .
We also argue that some SN progenitors with thin hydrogen layers produced via Case AB/B transfer might be related to Type IIb supernova progenitors with relatively small radii of about 10 ~ { } \mathrm { R _ { \odot } } .