  Gamow-Teller transitions in isotopes of chromium play a consequential role in
the presupernova evolution of massive stars. $\beta$-decay and electron capture
rates on chromium isotopes significantly affect the time rate of change of
lepton fraction ($\dot{Y_{e}}$). Fine-tuning of this parameter is one of the
key for simulating a successful supernova explosion. The (anti)neutrinos
produced as a result of electron capture and $\beta$-decay are transparent to
stellar matter during presupernova phases. They carry away energy and this
result in cooling the stellar core. In this paper we present the calculations
of Gamow-Teller strength distributions and (anti)neutrino energy loss rates due
to weak interactions on chromium isotopes of astrophysical importance. We
compare our results with measured data and previous calculations wherever
available.
