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Spin Tilts in the Double Pulsar Reveal Supernova Spin Angular-Momentum Production
High Energy Astrophysical Phenomena · Submitted 26 Apr 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Regardless of the details of the kick mechanism and the process that produced pulsar B's current spin, the measured spin-spin misalignment in the double pulsar system provides an empirical, direct constraint on the angular momentum production in this supernova.
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The abstract, sentence by sentence
The system PSR J0737-3039 is the only binary pulsar known to consist of two radio pulsars (PSR J0737-3039 A and PSR J0737-3039 B). This unique configuration allows measurements of spin orientation for both pulsars: pulsar A's spin is tilted from the orbital angular momentum by no more than 14 degrees at 95% confidence; pulsar B's by 130 +/- 1 degrees at 99.7% confidence. This spin-spin misalignment requires that the origin of most of B's present-day spin is connected to the supernova that formed pulsar B. Under the simplified assumption of a single, instantaneous kick during the supernova, the spin could be thought of as originating from the off-center nature of the kick, causing pulsar B to tumble to its misaligned state. With this assumption, and using current constraints on the kick magnitude, we find that pulsar B's instantaneous kick must have been displaced from the center of mass of the exploding star by at least 1 km and probably 5--10 km. Regardless of the details of the kick mechanism and the process that produced pulsar B's current spin, the measured spin-spin misalignment in the double pulsar system provides an empirical, direct constraint on the angular momentum production in this supernova. This constraint can be used to guide core-collapse simulations and the quest for understanding the spins and kicks of compact objects.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The system PSR J0737-3039 is the only binary pulsar known to consist of two radio pulsars (PSR J0737-3039 A and PSR J0737-3039 B). | background 1.00 | 0.06 | 0.02 | asserted 1.00 |
| s1 | This unique configuration allows measurements of spin orientation for both pulsars: pulsar A's spin is tilted from the orbital angular momentum by no more than 14 degrees at 95% confidence; pulsar B's by 130 +/- 1 degrees at 99.7% confidence. | result 1.00 | 0.72 | 0.13 | asserted 1.00 |
| s2 | This spin-spin misalignment requires that the origin of most of B's present-day spin is connected to the supernova that formed pulsar B. | interpretation 0.99 | 0.75 | 0.54 | asserted 0.91 |
| s3 | Under the simplified assumption of a single, instantaneous kick during the supernova, the spin could be thought of as originating from the off-center nature of the kick, causing pulsar B to tumble to its misaligned state. | interpretation 0.89 | 0.18 | 0.05 | hedged possibility 1.00 |
| s4 | With this assumption, and using current constraints on the kick magnitude, we find that pulsar B's instantaneous kick must have been displaced from the center of mass of the exploding star by at least 1 km and probably 5--10 km. | result 0.95 | 0.93 | 0.15 | asserted 0.82 |
| s5 | Regardless of the details of the kick mechanism and the process that produced pulsar B's current spin, the measured spin-spin misalignment in the double pulsar system provides an empirical, direct constraint on the angular momentum production in this supernova. | interpretation 0.92 | 0.83 | 0.76 | asserted 1.00 |
| s6 | This constraint can be used to guide core-collapse simulations and the quest for understanding the spins and kicks of compact objects. | future work 0.80 | 0.31 | 0.15 | asserted 0.61 |
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The paper
Original abstract
The system PSR J0737-3039 is the only binary pulsar known to consist of two radio pulsars (PSR J0737-3039 A and PSR J0737-3039 B). This unique configuration allows measurements of spin orientation for both pulsars: pulsar A's spin is tilted from the orbital angular momentum by no more than 14 degrees at 95% confidence; pulsar B's by 130 +/- 1 degrees at 99.7% confidence. This spin-spin misalignment requires that the origin of most of B's present-day spin is connected to the supernova that formed pulsar B. Under the simplified assumption of a single, instantaneous kick during the supernova, the spin could be thought of as originating from the off-center nature of the kick, causing pulsar B to tumble to its misaligned state. With this assumption, and using current constraints on the kick magnitude, we find that pulsar B's instantaneous kick must have been displaced from the center of mass of the exploding star by at least 1 km and probably 5--10 km. Regardless of the details of the kick mechanism and the process that produced pulsar B's current spin, the measured spin-spin misalignment in the double pulsar system provides an empirical, direct constraint on the angular momentum production in this supernova. This constraint can be used to guide core-collapse simulations and the quest for understanding the spins and kicks of compact objects.
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References
How the literature uses it
5 arXiv papers cite this in 5 sentences
Papers citing it · 4 sentences without a confident label
Uses its data or values 1 paper
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For example PSRJ0737-3039B has a spin misaligned with the orbital angular momentum by $≈130^∘$ [ref] .
Numerical Relativity Simulations of Precessing Binary Neutron Star Mergers · Introduction · 0.83
What it cites · 43 sentences without a confident label
Uses data or values from 4 papers
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This unique configuration has permitted measurements of spin orientation for both pulsars [ref] : pulsar A's spin is tilted from the orbital angular momentum vector by no more than 14 degrees at 95% confidence [ref] ; pulsar B's by $130.0^+1.4_-1.2$ degrees at $99.7$% confidence.
The double pulsar: evolutionary constraints from the system geometry · Introduction · 0.95
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This unique configuration has permitted measurements of spin orientation for both pulsars [ref] : pulsar A's spin is tilted from the orbital angular momentum vector by no more than 14 degrees at 95% confidence [ref] ; pulsar B's by $130.0^+1.4_-1.2$ degrees at $99.7$% confidence.
Relativistic Spin Precession in the Double Pulsar · Introduction · 0.95
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This unique configuration has permitted measurements of spin orientation for both pulsars [ref] : pulsar A's spin is tilted from the orbital angular momentum vector by no more than 14 degrees at 95% confidence [ref] ; pulsar B's by $130.0^+1.4_-1.2$ degrees at $99.7$% confidence.
Magnetospheric Eclipses in the Binary Pulsar J0737-3039 · Introduction · 0.95
Compares with 1 paper
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The constraint in Equation [ref] is consistent with the constraint on kick colatitude in Figure 7 of [ref] , but tighter.
Constraints on Natal Kicks in Galactic Double Neutron Star Systems · The Need for Spin Angular Momentum from the Supernova · 1.00
Cites as background 1 paper
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Due to asymmetries associated with the SN ejecta (matter and/or neutrinos) SNe are thought capable of imparting a significant recoil impulse, a “kick”, to any remnant surviving the explosion (see, e.g., [ref] and references therein).
Supernova explosions and the birth of neutron stars · Evolutionary History · 0.95
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