ON THE RADIOFREQUENCY EMISSION FROM THE GEMINGA PULSAR

The famous neutron star Geminga was until quite lately the only pulsar undetected in the radio regime, though observed as a strong pulsating gamma- and X-ray source. Three independent groups from the Pushchino Radio Astronomy Observatory (Russia) reported recently the detection o f pulsed radio emission from Geminga at 102.5 MHz, i.e., the first det ection of the radio pulsar PSR J0633 + 1746 by Kuz'min & Losovskii, Ma lofeev & Malov and Shitov & Pugachev. This pulsar exhibits the weakest radio luminosity known. Its average pulse profile appears to be very wide, filling an entire 360 degrees pulse window according to Kuz'min & Losovskii. We present a model explaining the peculiarities of the Ge minga radio pulsar, based on the assumption that it is an almost align ed rotator. The electromagnetic waves generated in the inner magnetosp here reach the region within the light cylinder with a weak magnetic h eld (at distances of a few Light cylinder radii), where they are stron gly damped due to the cyclotron resonance with particles of magnetosph eric electron-positron plasma. The lowest frequencies that can escape are determined by the value of the magnetic held in the region where t he line of sight passes through the Light cylinder. The specific viewi ng geometry of an almost aligned rotator implies that the observer's L ine of sight probes the emission region near the bundle of the last op en held Lines. This explains the unusually weak emission from Geminga' s low-frequency radio pulsar.