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The pulsar J1852+0040 in Kes 79 and the nature of central compact objects in supernova remnants

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Abstract

A possible model for the pulsar PSR J1852+0040 associated with the supernova remnant Kes 79 and detected in place of a central compact object in this remnant is discussed. The main observational properties of the pulsar can be understood as consequences of its weak surface magnetic field (B s < 3 × 1011 G) and short rotational period (P ∼ 0.1 s). Its X-ray emission is thermal, and is generated in a small region near the surface of the neutron star due to cooling of the surface as the surface accretes matter from a relict disk surrounding the pulsar. The radio emission is generated in the outer layers of the pulsar magnetosphere by the synchrotron (cyclotron) mechanism. The optical luminosity of J1852+0040 is estimated to be L opt < 1028 erg/s. If the spectral features in another central compact object, 1E 1207.4+5209, are interpreted as electron cyclotron lines, this provides evidence for a weak surface magnetic field for this neutron star as well (B < 6 × 1010 G). The hypothesis that all central compact objects have weak surface fields makes it possible to explain the number of detected central compact objects, the absence of pulsar-wind nebulae associated with these objects, and the fact that no pulsar has yet been detected at the position of SN 1987a. We suggest that, after the supernova remnant has dissipated, the central compact object becomes a weak X-ray source (XDINS), whose weak emission is also due to the weakness of its magnetic field.

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Authors and Affiliations

  1. Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117810, Russia

    I. F. Malov

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  1. I. F. Malov
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Original Russian Text © I.F. Malov, 2009, published in Astronomicheskiĭ Zhurnal, 2009, Vol. 86, No. 5, pp. 512–517.

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Malov, I.F. The pulsar J1852+0040 in Kes 79 and the nature of central compact objects in supernova remnants. Astron. Rep. 53, 472–476 (2009). https://doi.org/10.1134/S1063772909050114

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  • DOI: https://doi.org/10.1134/S1063772909050114

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