N-body simulations demonstrate that post-capture chaotic planet-planet interactions around pulsars can produce stable low-eccentricity orbits after ejections.
Orbital Parameters of the PSR B1620-26 Triple System
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abstract
Previous timing data for PSR~B1620$-$26 were consistent with a second companion mass $m_2$ anywhere in the range $\sim10^{-3}-1\,M_\odot$, i.e., from a Jupiter-type planet to a star. We present the latest timing parameters for the system, including a significant change in the projected semi-major axis of the inner binary, a marginal detection of the fourth time derivative of the pulse frequency, and the pulsar proper motion (which is in agreement with published values for the proper motion of M4), and use them to further constrain the mass $m_2$ and the orbital parameters. Using the observed value of $\stackrel{\ldots.}{f}$, we obtain a one-parameter family of solutions, all with $m_2 \lo 10^{-2}\,M_\odot$, i.e., excluding stellar masses. Varying $\stackrel{\ldots.}{f}$ within its formal $1\sigma$ error bar does not affect the mass range significantly. However, if we vary $\stackrel{\ldots.}{f}$ within a $4\sigma$ error bar, we find that stellar-mass solutions are still possible. We also calculate the predicted rate of change of the projected semi-major axis of the inner binary and show that it agrees with the measured value.
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2026 2representative citing papers
citing papers explorer
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Formation of stable exoplanetary systems around pulsars by capture: An exercise in computational classical mechanics
N-body simulations demonstrate that post-capture chaotic planet-planet interactions around pulsars can produce stable low-eccentricity orbits after ejections.
- The GMRT High-Resolution Southern Sky Survey for pulsars and transients -- VIII: Orbital Variability and the Evolution of a 1-Day He-WD Millisecond Pulsar J2101-4208