The central compact object 1E 1207.4-5209 emits pulsed radio waves at its 0.4-second spin period, revealing it as a faint radio pulsar.
Discovery of 424 ms pulsations from the radio-quiet neutron star in the PKS 1209-52 supernova remnant
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The central source of the supernova remnant PKS 1209-52 was observed with the Advanced CCD Imaging Spectrometer aboard Chandra X-ray observatory on 2000 January 6-7. The use of the Continuos Clocking mode allowed us to perform the timing analysis of the data with time resolution of 2.85 ms and to find a period P=0.42412927+/-2.3e-7 s. The detection of this short period proves that the source is a neutron star. It may be either an active pulsar with unfavorably directed radio beam or a truly radio-silent neutron star whose X-ray pulsations are caused by a nonuniform distribution of surface temperature. To infer the actual properties of this neutron star, the period derivative should be measured.
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astro-ph.HE 2representative citing papers
Numerical modeling with GALPROP predicts CTAO detectability of gamma rays from SNR G296.5+10.0 and CCO 1E 1207.4-5209 at 5 sigma after 50 hours, with hadronic processes dominating at lower energies and leptonic at higher.
citing papers explorer
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Pulsed radio emission from a Central Compact Object
The central compact object 1E 1207.4-5209 emits pulsed radio waves at its 0.4-second spin period, revealing it as a faint radio pulsar.
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Probing Low-Luminosity Gamma-Ray Emission from SNR G296.5+10.0 and CCO 1E 1207.4-5209 with CTAO
Numerical modeling with GALPROP predicts CTAO detectability of gamma rays from SNR G296.5+10.0 and CCO 1E 1207.4-5209 at 5 sigma after 50 hours, with hadronic processes dominating at lower energies and leptonic at higher.