Volume 450, Number 1, April IV 2006
|Page(s)||295 - 303|
|Section||Stellar structure and evolution|
|Published online||03 April 2006|
The ultra-cool white dwarf companion of PSR J0751+1807
Astronomical Institute, Utrecht University, PO Box 80 000, 3508 TA Utrecht, The Netherlands e-mail: firstname.lastname@example.org
2 Department of Astronomy and Astrophysics, University of Toronto, 60 Saint George Street, Toronto, ON M5S 3H8, Canada
3 Palomar Observatory, California Institute of Technology 105-24, Pasadena, CA 91125, USA
Accepted: 29 December 2005
We present optical and near-infrared observations with Keck of the binary millisecond pulsar PSR J0751+1807. We detect a faint, red object – with ± 0.07, ± 0.3, and ± 0.10 – at the celestial position of the pulsar and argue that it is the white dwarf companion of the pulsar. The colours are the reddest among all known white dwarfs, and indicate a very low temperature, K. This implies that the white dwarf cannot have the relatively thick hydrogen envelope that is expected on evolutionary grounds. Our observations pose two puzzles. First, while the atmosphere was expected to be pure hydrogen, the colours are inconsistent with this composition. Second, given the low temperature, irradiation by the pulsar should be important, but we see no evidence for it. We discuss possible solutions to these puzzles.
Key words: stars: pulsars: individual: PSR J0751+1807 / stars: binaries: close / stars: neutron / stars: white dwarfs
© ESO, 2006
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