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Solar activity, in particular coronal mass ejections (CMEs), are oftenaccompanied by bursts of radiation at metre wavelengths. Some of these burstshave a long duration and extend over a wide frequency band, namely, type IVradio bursts. However, the association of type IV bursts with coronal massejections is still not well understood. In this article, we perform the firststatistical study of type IV solar radio bursts in the solar cycle 24. Ourstudy includes a total of 446 type IV radio bursts that occurred during thiscycle. Our results show that a clear majority, $\sim 81 \%$ of type IV bursts,were accompanied by CMEs, based on a temporal association with white-light CMEobservations. However, we found that only $\sim 2.2 \%$ of the CMEs areaccompanied by type IV radio bursts. We categorised the type IV bursts asmoving or stationary based on their spectral characteristics and found thatonly $\sim 18 \%$ of the total type IV bursts in this study were moving type IVbursts. Our study suggests that type IV bursts can occur with both `Fast'($\geq 500$ km/s) and `Slow' ($< 500$ km/s), and also both `Wide' ($\geq60^{\circ}$) and `Narrow' ($< 60^{\circ}$) CMEs. However, the moving type IVbursts in our study were mostly associated with `Fast' and `Wide' CMEs ($\sim52 \%$), similar to type II radio bursts. Contrary to type II bursts,stationary type IV bursts have a more uniform association with all CME types.

On the occurrence of type IV solar radio bursts in the solar cycle 24 and their association with coronal mass ejections