The evolution of clumpy gas in young elliptical galaxies

The authors calculate numerically the mass flow fueled by stellar mass loss at an early epoch during the evolution of an elliptical galaxy. 10⁹ years after "birth" of the galaxy the interstellar gas which has accumulated from an (assumed) initial gas-free state flows towards the center and builds up the fuel of any activity in the nucleus of the galaxy. The authors investigate the influence of the random motions of clouds, generated by broken up supernova remnants and planetary nebulae, on the amount of gas which can be stored in the nucleus of a typical (giant) elliptical galaxy. They find that masses up to approximately 10⁵ M_sun; of neutral gas can be stored in the nucleus. The massive cloud begins to collapse when the dissipation of its kinetic bulk energy sets in rapidly. The result of the collapse can be a supermassive star.