The gamma-ray source LSI +61°303: II. Multiwavelength emission model

摘要: The multi–wavelength spectrum of LSI +61° 303 is summarized. X-ray to γ -ray luminosity $L_{\rm ic}\simeq1.5\times10^{35}$ erg/s due inverse Compton emission from relativistic electrons around a pulsar. determines the electron energy index, which consistent with observed radio if it mainly optically thin. compact region peaks at periastron higher density stellar photons. This highly self-absorbed frequencies implying quiescent comes separate diffuse population electrons. number and total in ~0.1 that (~$3\times10^{43}$ electrons, ~$5\times10^{38}$ erg). cannot be static its high internal pressure: expansion leading loss injection new are required. A pulsar spin period $\simeq$0.1 s can provide sufficient power. steady outflow produces too much thick synchrotron emission. alternative bulk bubble, dynamic pressure limiting velocity resulting away Be star. Injection ends as bubble wall facing star stalls pulsar's orbit takes out bubble. Alternately, Rayleigh-Taylor instability could cause break up before exit In either case, rates ~$2~L_{\rm ic}$ into result detached size, content similar initial conditions used by Peracaula ([CITE]) model outbursts for 303.