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It has been suggested that black hole low‐mass X‐ray binaries (BHLMXBs) with short orbital periods may have evolved from BH binaries with an intermediate‐mass secondary, but the donor star seems to always have higher effective temperatures than measured in BHLMXBs. Here we suggest that the secondary star is originally an intermediate‐mass  (∼2–5 M ⊙ )  star, which loses a large fraction of its mass due to the ejecta impact during the aspherical suparnova explosion that produced the BH. The resulted secondary star could be of low mass  (≲1 M ⊙ ) . Magnetic braking would shrink the binary orbit and drive mass transfer between the donor and the BH, producing a compact BHLMXB.

Aspherical supernova explosions and formation of compact black hole low‐mass X‐ray binaries