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Caterina Ciampi (GANIL)24/09/2026 15:00
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Dr Diego Gruyer (LPC Caen)24/09/2026 15:25Oral Presentation
The equation of state (EoS) of neutron-rich matter is a cornerstone for understanding the structure and dynamics of neutron stars, from their radii and tidal deformability to cooling mechanisms. However, the density dependence of the nuclear symmetry energy term remains a major source of uncertainty, particularly at densities near, and above, nuclear saturation density. While astrophysical...
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Ilham DEKHISSI24/09/2026 15:45Oral Presentation
The second $0_{2}^+$ state of $^{12}$C at an excitation energy of 7.654 MeV, known as the Hoyle state [1], is crucial to understanding how $^{12}$C is formed in stellar nucleosynthesis. Despite recent studies, there is no consensus on the properties of the Hoyle state, with different theoretical models predicting a range of radii and spatial arrangements[2,3].
Experimentally, only a few...
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