If weakly interactingmassive particles (WIMPs) constitute the bulk of darkmatter (DM), energy from the self-annihilation of these particles can affect Population III (Pop III) star formation via two mechanisms. Before the protostar forms, energy from DM annihilations can couple to primordial gas chemistry and slightly alter the properties of the cloud-without, however, inducing dramatic changes in the final mass of the star. Later, scattering betweenWIMPs and baryons within the protostar can in principle congregate enough DMfor annihilations, rather than nuclear reactions, to support the star against gravity. In these proceedings I briefly summarize the state of the art of the field, as well the prospects for observing such stars. © 2010 American Institute of Physics.
WIMP dark matter and the first stars / Iocco, F.. - 1294:(2010), pp. 66-69. (Intervento presentato al convegno 1st Stars and Galaxies: Challenges for the Next Decade tenutosi a Austin, TX, usa nel 2010) [10.1063/1.3518893].
WIMP dark matter and the first stars
Iocco F.
2010
Abstract
If weakly interactingmassive particles (WIMPs) constitute the bulk of darkmatter (DM), energy from the self-annihilation of these particles can affect Population III (Pop III) star formation via two mechanisms. Before the protostar forms, energy from DM annihilations can couple to primordial gas chemistry and slightly alter the properties of the cloud-without, however, inducing dramatic changes in the final mass of the star. Later, scattering betweenWIMPs and baryons within the protostar can in principle congregate enough DMfor annihilations, rather than nuclear reactions, to support the star against gravity. In these proceedings I briefly summarize the state of the art of the field, as well the prospects for observing such stars. © 2010 American Institute of Physics.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
