Masses and Orbital Inclinations of Planets in the PSR B1257+12 System
- Creators
- Konacki, Maciej
- Wolszczan, Alex
Abstract
We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations detectable as microsecond variations of the arrival times of radio pulses from the pulsar. The 6.2 ms pulsar, PSR B1257+12, has been regularly timed with the Arecibo telescope since late 1990. Assuming the standard pulsar mass of 1.4 M_☉, the derived masses of planets B and C are 4.3 ± 0.2 and 3.9 ± 0.2 M_⊕, respectively. The corresponding orbital inclinations of 53° ± 4° and 47° ± 3° (or 127° and 133°) imply that the two orbits are almost coplanar. This result, together with the known near 3 : 2 resonance between the orbits of the two planets, strongly supports the hypothesis of a disk origin of the PSR B1257+12 planetary system. The system's long-term stability is guaranteed by the low Earth-like masses of planets B and C.
Additional Information
© 2003. The American Astronomical Society. Received 2003 April 3; accepted 2003 May 23; published 2003 June 12. M. K. is a Michelson Postdoctoral Fellow and is partially supported by the Polish Committee for Scientific Research, grant 2P03D 001 22. A. W. is supported by NASA grant NAG5-4301 and by the NSF under grant AST 99-88217. The authors thank the referee, Renu Malhotra, for insightful comments on the manuscript.Attached Files
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Additional details
- Eprint ID
- 75891
- Resolver ID
- CaltechAUTHORS:20170408-135641153
- Michaelson Postdoctoral Fellowship
- 2P03D 001 22
- Polish Committee for Scientific Research
- NAG5-4301
- NASA
- AST 99-88217
- NSF
- Created
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2017-04-14Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field