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Constraints on Natal Kicks in Galactic Double Neutron Star Systems
High Energy Astrophysical Phenomena · Submitted 13 Aug 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Therefore in these systems, it is not clear which type of supernova is more likely to form the 2nd neutron star.
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The abstract, sentence by sentence
Since the discovery of the first double neutron star (DNS) system in 1975 by Hulse and Taylor, there are currently 8 confirmed DNS in our galaxy. For every system, the masses of both neutron stars, the orbital semi- major axis and eccentricity are measured, and proper motion is known for half of the systems. Using the orbital parameters and kinematic information, if available, as constraints for all system, we investigate the immediate progenitor mass of the second-born neutron star and the magnitude of the supernova kick it received at birth, with the primary goal to understand the core collapse mechanism leading to neutron star formation. Compared to earlier studies, we use a novel method to address the uncertainty related to the unknown radial velocity of the observed systems. For PSR B1534+12 and PSR B1913+16, the kick magnitudes are 150 - 270 km/s and 190 - 450 km/s (with 95% confidence) respectively, and the progenitor masses of the 2nd born neutron stars are 1.3 - 3.4 Msun and 1.4 - 5.0 Msun (95%), respectively. These suggest that the 2nd born neutron star was formed by an iron core collapse supernova in both systems. For PSR J0737-3039, on the other hand, the kick magnitude is only 5 - 120 km/s (95%), and the progenitor mass of the 2nd born neutron star is 1.3 - 1.9 Msun (95%). Because of the relatively low progenitor mass and kick magnitude, the formation of the 2nd born neutron star in PSR J0737-3039 is potentially connected to an electron capture supernova of a massive O - Ne - Mg white dwarf. For the remaining 5 Galactic DNS, the kick magnitude ranges from several tens to several hundreds of km/s, and the progenitor mass of the 2nd formed neutron star can be as low as ~1.5 Msun, or as high as ~8 Msun. Therefore in these systems, it is not clear which type of supernova is more likely to form the 2nd neutron star.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Since the discovery of the first double neutron star (DNS) system in 1975 by Hulse and Taylor, there are currently 8 confirmed DNS in our galaxy. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | For every system, the masses of both neutron stars, the orbital semi- major axis and eccentricity are measured, and proper motion is known for half of the systems. | background 0.99 | 0.09 | 0.01 | asserted 1.00 |
| s2 | Using the orbital parameters and kinematic information, if available, as constraints for all system, we investigate the immediate progenitor mass of the second-born neutron star and the magnitude of the supernova kick it received at birth, with the primary goal to understand the core collapse mechanism leading to neutron star formation. | contribution 0.75 | 0.88 | 0.04 | asserted 0.79 |
| s3 | Compared to earlier studies, we use a novel method to address the uncertainty related to the unknown radial velocity of the observed systems. | contribution 0.71 | 0.90 | 0.02 | asserted 1.00 |
| s4 | For PSR B1534+12 and PSR B1913+16, the kick magnitudes are 150 - 270 km/s and 190 - 450 km/s (with 95% confidence) respectively, and the progenitor masses of the 2nd born neutron stars are 1.3 - 3.4 Msun and 1.4 - 5.0 Msun (95%), respectively. | result 1.00 | 0.93 | 0.11 | asserted 1.00 |
| s5 | These suggest that the 2nd born neutron star was formed by an iron core collapse supernova in both systems. | interpretation 1.00 | 0.82 | 0.21 | hedged possibility 0.90 |
| s6 | For PSR J0737-3039, on the other hand, the kick magnitude is only 5 - 120 km/s (95%), and the progenitor mass of the 2nd born neutron star is 1.3 - 1.9 Msun (95%). | result 1.00 | 0.93 | 0.05 | asserted 1.00 |
| s7 | Because of the relatively low progenitor mass and kick magnitude, the formation of the 2nd born neutron star in PSR J0737-3039 is potentially connected to an electron capture supernova of a massive O - Ne - Mg white dwarf. | interpretation 1.00 | 0.81 | 0.12 | hedged possibility 1.00 |
| s8 | For the remaining 5 Galactic DNS, the kick magnitude ranges from several tens to several hundreds of km/s, and the progenitor mass of the 2nd formed neutron star can be as low as ~1.5 Msun, or as high as ~8 Msun. | result 1.00 | 0.92 | 0.06 | asserted 0.95 |
| s9 | Therefore in these systems, it is not clear which type of supernova is more likely to form the 2nd neutron star. | interpretation 0.91 | 0.73 | 0.22 | asserted 0.62 |
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Original abstract
Since the discovery of the first double neutron star (DNS) system in 1975 by Hulse and Taylor, there are currently 8 confirmed DNS in our galaxy. For every system, the masses of both neutron stars, the orbital semi- major axis and eccentricity are measured, and proper motion is known for half of the systems. Using the orbital parameters and kinematic information, if available, as constraints for all system, we investigate the immediate progenitor mass of the second-born neutron star and the magnitude of the supernova kick it received at birth, with the primary goal to understand the core collapse mechanism leading to neutron star formation. Compared to earlier studies, we use a novel method to address the uncertainty related to the unknown radial velocity of the observed systems. For PSR B1534+12 and PSR B1913+16, the kick magnitudes are 150 - 270 km/s and 190 - 450 km/s (with 95% confidence) respectively, and the progenitor masses of the 2nd born neutron stars are 1.3 - 3.4 Msun and 1.4 - 5.0 Msun (95%), respectively. These suggest that the 2nd born neutron star was formed by an iron core collapse supernova in both systems. For PSR J0737-3039, on the other hand, the kick magnitude is only 5 - 120 km/s (95%), and the progenitor mass of the 2nd born neutron star is 1.3 - 1.9 Msun (95%). Because of the relatively low progenitor mass and kick magnitude, the formation of the 2nd born neutron star in PSR J0737-3039 is potentially connected to an electron capture supernova of a massive O - Ne - Mg white dwarf. For the remaining 5 Galactic DNS, the kick magnitude ranges from several tens to several hundreds of km/s, and the progenitor mass of the 2nd formed neutron star can be as low as ~1.5 Msun, or as high as ~8 Msun. Therefore in these systems, it is not clear which type of supernova is more likely to form the 2nd neutron star.
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How the literature uses it
3 arXiv papers cite this in 11 sentences
Papers citing it · 6 sentences without a confident label
Uses its data or values 1 paper
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Using constraints on the SN kick magnitude derived from the orbital and kinematic parameters of the system [ref] we find that this kick must have been displaced from the center of mass of the exploding star by at least 1 km and probably 5–10 km.
Spin Tilts in the Double Pulsar Reveal Supernova Spin Angular-Momentum Production · Introduction · 0.86
Compares with it 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.
Spin Tilts in the Double Pulsar Reveal Supernova Spin Angular-Momentum Production · The Need for Spin Angular Momentum from the Supernova · 1.00
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