An optical counterpart to the anomalous X-ray pulsar 4U0142+61

Article

关键词: WHITE-DWARF;    EMISSION;    STARS;   

DOI  :  10.1038/35047024

来源: SCIE

【 摘 要 】

The energy source of the anomalous X-ray pulsars' (AXPs) is not understood, hence their designation as anomalous. Unlike binary X-ray pulsars, no companions are seen, so the energy cannot be supplied by accretion of matter from a companion star. The loss of rotational energy, which powers radio pulsars, is insufficient to power AXPs. Two models are generally considered: accretion from a large disk left over from the birth process(2,3), or decay of a very strong magnetic field (10(15) G) associated with a 'magnetar'(4). The lack of counterparts at other wavelengths has hampered progress in our understanding of these objects. Here we report deep optical observations of the field around 4U0142+61, which is the brightest AXP in X-rays. The source has no associated supernova remnant, which, together with its spin-down timescale of similar to 10(5)yr (ref. 5), suggests that it may be relatively old. We find an object with peculiar optical colours at the position of the X-ray source, and argue that it is the optical counterpart. The optical emission is too faint to admit the presence of a large accretion disk, but may be consistent with magnetospheric emission from a magnetar.

【 授权许可】

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