On the triple nature of the PSR J0435+3233 system
Abstract
The recent pulsar timing ephemeris of PSR J0435+3233 indicates that this millisecond pulsar (MSP) has a spin-down rate that is much higher than observed in other MSPs and challenges our understanding of the formation and evolution of MSPs. We propose that this system is a hierarchical triple, and that the high spin-down rate is caused by varying acceleration due to a tertiary in a wide orbit. We use pulsar timing methods with radio and gamma-ray observations of PSR J0435+3233 to determine the system properties. We find that a hierarchical triple timing model describes the timing observations of PSR J0435+3233 and that this results in the detection of gamma-ray pulsations back to the beginning of the Fermi Large Area Telescope (LAT) data in 2008. The intrinsic spin-down rate remains uncertain as it correlates with the parameters of the outer orbit, but large spin-down rates are excluded and the intrinsic rate is at least two orders of magnitude lower than the observed rate, in line with other Galactic MSPs. We identify a star located 11 mas from the pulsar position as the optical counterpart to the tertiary companion. From the 1.5-2.5 kpc distance and colours, we infer that the tertiary is a 1.2-solar mass F-type main-sequence star. Along with the pulsar binary, it orbits the common centre of mass with an eccentric (e ~ 0.6), wide (~70 yr) orbit that is likely seen at a low orbital inclination. We conclude that PSR J0435+3233 is a hierarchical triple system. We discuss the motivation and prospects for the continued study of this system. Spectral measurements of the outer star in addition to continued astrometric measurements will yield mass ratio and inclination estimates, while continued pulsar timing may yield a tighter constraint on violations of the Strong Equivalence Principle than are currently obtained from PSR J0337+1715.
Related
BibTeX
@misc{freire2026triple,
title = {{On the triple nature of the PSR J0435+3233 system}},
author = {Paulo C.C Freire and Colin J Clark and Cees G Bassa and Guillaume Voisin and Rutger van Haasteren and Lars Nieder and Benjamin W Stappers},
howpublished = {HAL},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2607.27462},
eprint = {2607.27462},
archivePrefix = {arXiv},
url = {https://hal.science/hal-05734247v1},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - On the triple nature of the PSR J0435+3233 system
AU - Paulo C.C Freire
AU - Colin J Clark
AU - Cees G Bassa
AU - Guillaume Voisin
AU - Rutger van Haasteren
AU - Lars Nieder
AU - Benjamin W Stappers
PY - 2026
DA - 2026/09/01
PB - HAL
DO - 10.48550/arxiv.2607.27462
UR - https://hal.science/hal-05734247v1
AB - The recent pulsar timing ephemeris of PSR J0435+3233 indicates that this millisecond pulsar (MSP) has a spin-down rate that is much higher than observed in other MSPs and challenges our understanding of the formation and evolution of MSPs. We propose that this system is a hierarchical triple, and that the high spin-down rate is caused by varying acceleration due to a tertiary in a wide orbit. We use pulsar timing methods with radio and gamma-ray observations of PSR J0435+3233 to determine the system properties. We find that a hierarchical triple timing model describes the timing observations of PSR J0435+3233 and that this results in the detection of gamma-ray pulsations back to the beginning of the Fermi Large Area Telescope (LAT) data in 2008. The intrinsic spin-down rate remains uncertain as it correlates with the parameters of the outer orbit, but large spin-down rates are excluded and the intrinsic rate is at least two orders of magnitude lower than the observed rate, in line with other Galactic MSPs. We identify a star located 11 mas from the pulsar position as the optical counterpart to the tertiary companion. From the 1.5-2.5 kpc distance and colours, we infer that the tertiary is a 1.2-solar mass F-type main-sequence star. Along with the pulsar binary, it orbits the common centre of mass with an eccentric (e ~ 0.6), wide (~70 yr) orbit that is likely seen at a low orbital inclination. We conclude that PSR J0435+3233 is a hierarchical triple system. We discuss the motivation and prospects for the continued study of this system. Spectral measurements of the outer star in addition to continued astrometric measurements will yield mass ratio and inclination estimates, while continued pulsar timing may yield a tighter constraint on violations of the Strong Equivalence Principle than are currently obtained from PSR J0337+1715.
ER -