The connection between gamma-ray bursts (GRBs) and core-collapse supernovae (SNe) has been established through observational and theoretical evidence. GRBs, which are brief, intense flashes of high-energy radiation, are often associated with SNe, particularly long-duration, soft-spectrum GRBs. These events are linked to the deaths of massive stars, with the kinetic energy and luminosity of GRB-SNe exceeding those of ordinary SNe. However, the energy in the explosion is primarily contained in nonrelativistic ejecta, not the relativistic jets responsible for the burst. Not all SNe or even all Type Ibc SNe produce GRBs, and the difference lies in the degree of differential rotation in the collapsing iron core of massive stars. Observational evidence, such as the association of GRB 980425 with SN 1998bw, has confirmed the connection. This event showed that the SN and GRB were coincident in time and place, with the SN being a Type Ic-BL supernova. Similar associations have been found for other GRBs, such as GRB 030329 with SN 2003dh. These events suggest that most long-duration GRBs are accompanied by SNe of Type Ic. However, there is evidence for diversity in the brightness, rise times, and evolution of these events. The locations of long-duration GRBs are often in regions of active star formation, with their host galaxies being faint and blue. These galaxies are systematically smaller, dimmer, and more irregular than typical galaxies at similar redshifts. The presence of low metallicity in GRB host galaxies is also notable, as it is associated with the formation of massive stars. The study of GRB-SNe has revealed characteristics such as the concentration of significant kinetic energy in relativistic ejecta, the absence of hydrogen in their spectra, and the presence of broad absorption lines. These features distinguish GRB-SNe from other SNe. The energy released in GRB-SNe is comparable to that of ordinary SNe, but the exact relationship between the two phenomena is still being explored. The connection between GRBs and SNe has implications for the role of rotation in the deaths of massive stars. The most rapidly rotating and massive stars are more likely to produce GRBs, while ordinary SNe come from stars with less significant rotation. The continued observation of GRBs and their associated SNe will provide further insights into the underlying physics of these events. The future of this field remains uncertain, but the association between GRBs and SNe is a key area of research in understanding the most powerful explosions in the universe.The connection between gamma-ray bursts (GRBs) and core-collapse supernovae (SNe) has been established through observational and theoretical evidence. GRBs, which are brief, intense flashes of high-energy radiation, are often associated with SNe, particularly long-duration, soft-spectrum GRBs. These events are linked to the deaths of massive stars, with the kinetic energy and luminosity of GRB-SNe exceeding those of ordinary SNe. However, the energy in the explosion is primarily contained in nonrelativistic ejecta, not the relativistic jets responsible for the burst. Not all SNe or even all Type Ibc SNe produce GRBs, and the difference lies in the degree of differential rotation in the collapsing iron core of massive stars. Observational evidence, such as the association of GRB 980425 with SN 1998bw, has confirmed the connection. This event showed that the SN and GRB were coincident in time and place, with the SN being a Type Ic-BL supernova. Similar associations have been found for other GRBs, such as GRB 030329 with SN 2003dh. These events suggest that most long-duration GRBs are accompanied by SNe of Type Ic. However, there is evidence for diversity in the brightness, rise times, and evolution of these events. The locations of long-duration GRBs are often in regions of active star formation, with their host galaxies being faint and blue. These galaxies are systematically smaller, dimmer, and more irregular than typical galaxies at similar redshifts. The presence of low metallicity in GRB host galaxies is also notable, as it is associated with the formation of massive stars. The study of GRB-SNe has revealed characteristics such as the concentration of significant kinetic energy in relativistic ejecta, the absence of hydrogen in their spectra, and the presence of broad absorption lines. These features distinguish GRB-SNe from other SNe. The energy released in GRB-SNe is comparable to that of ordinary SNe, but the exact relationship between the two phenomena is still being explored. The connection between GRBs and SNe has implications for the role of rotation in the deaths of massive stars. The most rapidly rotating and massive stars are more likely to produce GRBs, while ordinary SNe come from stars with less significant rotation. The continued observation of GRBs and their associated SNe will provide further insights into the underlying physics of these events. The future of this field remains uncertain, but the association between GRBs and SNe is a key area of research in understanding the most powerful explosions in the universe.