Hostname: page-component-76fb5796d-x4r87 Total loading time: 0 Render date: 2024-04-26T10:51:57.833Z Has data issue: false hasContentIssue false
  • English
  • Français

Macho Detection by Pulsar Timing Observation

Published online by Cambridge University Press:  12 April 2016

Kouji Ohnishi ,
Mizuhiko Hosokawa ,
Toshio Fukushima  and
Mine Takeuti
Kouji Ohnishi
Affiliation:
Kansai Advanced Research Center, Communications Research Laboratory, Kobe 651-24, Japan
Mizuhiko Hosokawa
Affiliation:
Communications Research Laboratory, Koganei, Tokyo 184, Japan
Toshio Fukushima
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
Mine Takeuti
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-77, Japan

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The magnitudes of some general relativistic effects depend on the mass of gravitating objects; therefore, these effects can be used for the stellar mass measurement. Several methods have been proposed; for example, the microlensing effect (Paczyński 1986), and the parallactic variation of gravitational deflection of the light from the source (Hosokawa et al. 1993).

Recently some candidates for MACHOs – a kind of dark matter candidates in the Galactic halo – have been discovered by their microlensing effect, and their masses were estimated to be of the order of 0.1Mʘ, under many assumptions. Actual measurement of MACHO masses are important in specifying what kind of object the MACHO is.

Type
Part 2 Precision Measurements
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 125 - 126
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

Hosokawa, M., Ohnishi, K., Fukushima, T. & Takeuti, M. 1993, A&A, 278, L27 Google Scholar
Ohnishi, K., Hosokawa, M., Fukushima, T. & Takeuti, M. 1995, ApJ, 448, 271 Google Scholar
Paczyński, B. 1986, ApJ, 304, 1 CrossRefGoogle Scholar