Large-scale measurements of the red giant core rotation through\n asteroseismology

Red giant stars are solar-like pulsators presenting mixed-modes. Such modes\nconsist in a coupling between pressure waves propagating in the external\nconvective envelope and gravity waves propagating in the radiative interior.\nTherefore, the red giant asteroseismology provides us with a direct view on\ntheir core and opens the possibility to monitor the evolution of their core\nrotation. Previous measurements of the mean core rotation revealed that angular\nmomentum is efficiently transferred from the core to the envelope inside red\ngiants, but the physical mechanisms at work are not yet fully understood. We\nthus need stronger observational constraints on the evolution of the red giant\ncore rotation. In this context, we developed an automated method to determine\nthe mean core rotation of red giant branch stars observed with Kepler. This\nautomated method is paving the way for the future PLATO data, representing\nhundreds of thousands of potential red giant oscillation spectra. Results\nobtained for almost 1200 red giant branch stars indicate that the rate of the\ncore rotation braking is lower than previously estimated and does not seem to\ndepend on the stellar mass.\n