The Spectrum of LMC Pulsar B0540-69; Carryover

Details The Spectrum of LMC Pulsar B0540-69; Carryover The Spectrum of LMC Pulsar B0540-69; Carryover

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5780b&link_type=abstract

HST Proposal ID #5780

Computer Science

Hst Proposal Id #5780 Hot Stars

Scientific paper

PSR B0540-69, a 50 ms pulsar located in the Large Magellanic Cloud, is the most distant pulsar known. B0540-69 is one of the few pulsars for which a second time derivative of rotational frequency has been measured. High Speed Photometer observations in a UV + visible passband (1600 - 7000 angstroms) showed a pulse profile identical to that in the X-ray region, with the same pulsed fraction (van Citters et al 1994). The rotational frequency observed by HSP, when compared with previous measurements, gave a value of 2.28 (0.02) for the braking index. B0540-69 is similar to the Crab pulsar in its rotational perior and associated synchrotron-emitting nebula (a "plerion"), but its pulse profile and braking index are strikingly different. We propose her to obtain an objective prism spectrum of B0540-69 to compare its spectral energy distribution in the UV and blue with that of the Crab pulsar and to determine the fractional part of our UV plus visible pulse profile due to UV photons. Our objective prism spectrum with the FOS Blue detector will measure the relative energy distribution between ~1850 and ~5000 angstroms.

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