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Microlensing of pulsar-radiation

Published online by Cambridge University Press:  12 April 2016

Norbert Wex ,
Janusz Gil  and
Marek Sendyk
Norbert Wex
Affiliation:
Max Planck Society, Research Unit ‘Theory of Gravitation’, at, the University of Jena, Max-Wien-Platz 1, D-07743 Jena, Germany
Janusz Gil
Affiliation:
Astronomical Centre, Pedagogical University, Lubuska 2, 65-265 Zielona Góra, Poland
Marek Sendyk
Affiliation:
Astronomical Centre, Pedagogical University, Lubuska 2, 65-265 Zielona Góra, Poland

Extract

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When the radiation of a star passes near a massive object, its intensity is magnified due to the microlensing phenomenon. Similar effects should also apply to pulsar signals. However, because of the pulsating nature of pulsar radiation, the flux magnification will be accompanied by a time varying travel-time delay (Krauss and Small 1991, Larchenkova and Doroshenko 1995, Ohnishi et al. 1995, Wexet al. 1996).

Let us denote the epoch of observation by t⊕. A travel-time delay caused by a Schwarzschild-lens is characterized by four parameters: M, the mass of the lens, q, the ratio of the transverse velocity of the lens with respect to the line of sight and the minimum impact parameter, fm, the ratio of the minimum impact parameter and the Einstein radius, and T0, the time of maximum delay. If we denote the ‘intrinsic’ frequency and its derivative with respect to time (corresponding to the barycentric arrival time t = t⊕) by ν and then, we find for the observed phase of the pulsar at the barycentric time t:

Type
Part 2 Precision Measurements
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 127 - 128
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

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Larchenkova, T.I., Doroshenko, 1995, A&A, 297, L607 Google Scholar
Ohnishi, K., Hosokawa, M., Fukushima, T., Takeuti, M., 1995, ApJ, 448, 2710 Google Scholar
Wex, N., Gil, J., Sendyk, M., 1996, A&A, in press, astro-ph/9511023Google Scholar