Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

Temim, Tea; Slane, Patrick; Plucinsky, Paul P.; Gelfand, Joseph D.; Castro, Daniel; Kolb, C.

doi:10.3847/1538-4357/aa9d41

Cited by 11 publications

(8 citation statements)

References 14 publications

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“…The average observed pulsar velocity is several hundred km s −1 (e.g., Bailes et al 1990;Caraveo & Mignani 1999;Hobbs et al 2005;Deller et al 2012;Temim et al 2017;Deller et al 2018). There have been several mechanisms put fourth to explain high natal velocities of pulsars.…”

Section: Neutron Star Velocitymentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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The origin of fast radio bursts (FRBs) is still a mystery. One model proposed to interpret the only known repeating object, FRB 121102, is that the radio emission is generated from asteroids colliding with a highly magnetized neutron star (NS). With N -body simulations, we model a debris disc around a central star with an eccentric orbit intruding NS. As the NS approaches the first periastron passage, most of the comets are scattered away rather than being accreted by the NS. To match the observed FRB rate, the debris belt would have to be at least three orders of magnitude more dense than the Kuiper belt. We also consider the rate of collisions on to the central object but find that the density of the debris belt must be at least four orders of magnitude more dense than the Kuiper belt. These discrepancies in the density arise even if (1) one introduces a Kuiper-belt like comet belt rather than an asteroid belt and assume that comet impacts can also make FRBs; (2) the NS moves ∼ 2 orders of magnitude slower than their normal proper-motion velocity due to supernova kicks; and (3) the NS orbit is coplanar to the debris belt, which provides the highest rate of collisions.

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Section: Neutron Star Velocitymentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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“…As seen in Figure 9, the proper motion of the neutron star in G292 lies at the higher end of the distribution of kick velocities for Galactic neutron stars, and has a transverse kick velocity similar to the pulsar located in MSH 15-56 (Temim et al 2017). Wongwathanarat et al (2013) noted that some neutrino-driven supernova models can impart kick velocities in excess of 600 km s −1 within the first few seconds of core-collapse, but that study only considered 20 models, with a limited range of progenitor masses.…”

Section: Discussionmentioning

confidence: 84%

“…In Figure 9 we plot our measured kick velocity for the neutron star in G292 against the distribution of Galactic neutron stars presented in Hobbs et al (2005). We include recent results presented by Mayer & Becker (2021) for a sample of central compact objects (CCOs) in SNRs, and the recent measurement of the pulsar proper motion in MSH 15-56 (Temim et al 2017).…”

Section: Discussionmentioning

confidence: 99%

The Proper Motion of the Pulsar J1124-5916 in the Galactic Supernova Remnant G292.0+1.8

Long,

Patnaude,

Plucinsky

et al. 2022

Preprint

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We present the first direct measurement of the proper motion of pulsar J1124-5916 in the young, oxygen-rich supernova remnant G292.0+1.8. Using deep Chandra ACIS-I observations from 2006 and 2016, we measure a positional change of 0. 21 ± 0. 05 over the ∼ 10 year baseline, or ∼ 0. 02 yr −1 . At a distance of 6.2 ± 0.9 kpc, this corresponds to a kick velocity in the plane of the sky of 612 ± 152 km s −1 . We compare this direct measurement against the velocity inferred from estimates based on the center of mass of the ejecta. Additionally, we use this new proper motion measurement to compare the motion of the neutron star to the center of expansion of the optically emitting ejecta. We derive an age estimate for the supernova remnant of 2000 years. The high measured kick velocity is in line with recent studies of high proper motion neutron stars in other Galactic supernova remnants, and consistent with a hydrodynamic origin to the neutron star kick.

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“…We include recent results presented by Mayer & Becker (2021) for a sample of central compact objects (CCOs) in SNRs and the recent measurement of the pulsar proper motion in MSH 15-56 (Temim et al 2017).…”

Section: Discussionmentioning

confidence: 99%

The Proper Motion of the Pulsar J1124–5916 in the Galactic Supernova Remnant G292.0+1.8

Long

Patnaude

Plucinsky

et al. 2022

ApJ

Self Cite

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We present the first direct measurement of the proper motion of pulsar J1124–5916 in the young, oxygen-rich supernova remnant G292.0+1.8. Using deep Chandra ACIS-I observations from 2006 to 2016, we measure a positional change of 0.″21 ± 0.″05 over the ∼10 yr baseline, or ∼0.″02 yr−1. At a distance of 6.2 ± 0.9 kpc, this corresponds to a kick velocity in the plane of the sky of 612 ± 152 km s−1. We compare this direct measurement against the velocity inferred from estimates based on the center of mass of the ejecta. Additionally, we use this new proper-motion measurement to compare the motion of the neutron star to the center of expansion of the optically emitting ejecta. We derive an age estimate for the supernova remnant of ≳2000 yr. The high measured kick velocity is in line with recent studies of high proper motion neutron stars in other Galactic supernova remnants and consistent with a hydrodynamic origin to the neutron star kick.

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Proper Motion of the High-velocity Pulsar in SNR MSH 15-56

Cited by 11 publications

References 14 publications

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

The Proper Motion of the Pulsar J1124-5916 in the Galactic Supernova Remnant G292.0+1.8

The Proper Motion of the Pulsar J1124–5916 in the Galactic Supernova Remnant G292.0+1.8

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