Neutron stars, pulsars, pulsar wind nebulae, and more supernova remnants

AbstractMotivated by the wealth of past, existing, and upcoming X-ray and gamma-ray missions, we have developed the first public database of high-energy observations of all known Galactic Supernova Remnants (SNRs): http://www.physics.umanitoba.ca/snr/SNRcat. The catalogue links to, and complements, other existing related catalogues, including Dave Green's radio SNRs catalogue. We here highlight the features of the high-energy catalogue, including allowing users to filter or sort data for various purposes. The catalogue is currently targeted to Galactic SNR observations with X-ray and gamma-ray missions, and is timely with the upcoming launch of X-ray missions (including Astro-H in 2014). We are currently developing the existing database to include an up-to-date Pulsar Wind Nebulae (PWNe)-dedicated webpage, with the goal to provide a global view of PWNe and their associated neutron stars/pulsars. This extensive database will be useful to both theorists to apply their models or design numerical simulations, and to observers to plan future observations or design new instruments. We welcome input and feedback from the SNR/PWN/neutron stars community.

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Pulsar Wind Nebulae: On their growing diversity and association with highly magnetized neutron stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312023782 ◽

2012 ◽

Vol 8 (S291) ◽

pp. 251-256 ◽

Cited By ~ 2

Author(s):

Samar Safi-Harb

Keyword(s):

Neutron Stars ◽

Supernova Remnants ◽

High Energy ◽

Current Status ◽

Pulsar Wind Nebulae ◽

X Ray ◽

The Past ◽

Pulsar Wind

AbstractThe 1968 discovery of the Crab and Vela pulsars in their respective supernova remnants (SNRs) confirmed Baade and Zwicky's 1934 prediction that supernovae form neutron stars. Observations of Pulsar Wind Nebulae (PWNe), particularly with the Chandra X-ray Observatory, have in the past decade opened a new window to focus on the neutron stars' relativistic winds, study their interaction with their hosting SNRs, and find previously missed pulsars. While the Crab has been thought for decades to represent the prototype of PWNe, we now know of different classes of neutron stars and PWNe whose properties differ from the Crab. In this talk, I review the current status of neutron stars/PWNe-SNRs associations, and highlight the growing diversity of PWNe with an X-ray eye on their association with highly magnetized neutron stars. I conclude with an outlook to future high-energy studies.

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The H.E.S.S. Galactic Plane Survey

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310011865 ◽

2009 ◽

Vol 5 (H15) ◽

pp. 808-808

Author(s):

Emma de Oña-Wilhelmi

Keyword(s):

Supernova Remnants ◽

Binary Systems ◽

Galactic Plane ◽

Giant Molecular Clouds ◽

Pulsar Wind Nebulae ◽

Compact Binary ◽

Pulsar Wind ◽

Star Formation Regions ◽

Galactic Sources ◽

Gps Observations

AbstractThe H.E.S.S. Galactic Plane Survey (GPS) has revealed a large number of Galactic Sources, including Pulsar Wind Nebulae (PWN), Supernova Remnants (SNRs), giant molecular clouds, star formation regions and compact binary systems, as well as a number of unidentified objects, or dark sources, for which no obvious counterparts at other wavelengths have yet been found. We will review the latest results from the GPS observations and discuss the most interesting cases.

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Neutron Stars, Pulsars, and Pulsar Wind Nebulae

Astronomy and Astrophysics Library - Physics and Evolution of Supernova Remnants ◽

10.1007/978-3-030-55231-2_6 ◽

2020 ◽

pp. 117-169

Author(s):

Jacco Vink

Keyword(s):

Neutron Stars ◽

Pulsar Wind Nebulae ◽

Pulsar Wind

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Peculiar Differences in Radio and X-ray Synchrotron Radiation from Pulsar Wind Nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900181033 ◽

2004 ◽

Vol 218 ◽

pp. 221-224

Author(s):

John R. Dickel ◽

Shiya Wang

Keyword(s):

Synchrotron Radiation ◽

Radio Emission ◽

Supernova Remnants ◽

Crab Nebula ◽

Pulsar Wind Nebulae ◽

X Ray ◽

Pulsar Wind ◽

The Crab Nebula

Several Crab-type supernova remnants appear to have very bright non-thermal X-ray cores just around the pulsar or expected pulsar. This X-ray brightness is often not matched by a corresponding increase in radio emission. The best example of this phenomenon is in N157B in the LMC. G21.5−0.9 and possibly 3C 58 also show it while the Crab Nebula and 0540−69.3 do not. Some method to enhance the higher energy particles must be present in these objects.

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A catalogue of Galactic supernova remnants in the far-infrared: revealing ejecta dust in pulsar wind nebulae

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2942 ◽

2018 ◽

Vol 483 (1) ◽

pp. 70-118 ◽

Cited By ~ 12

Author(s):

H Chawner ◽

K Marsh ◽

M Matsuura ◽

H L Gomez ◽

P Cigan ◽

...

Keyword(s):

Supernova Remnants ◽

Far Infrared ◽

Pulsar Wind Nebulae ◽

Pulsar Wind

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A LOFAR search for steep-spectrum pulsars in supernova remnants and pulsar wind nebulae

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833922 ◽

2019 ◽

Vol 623 ◽

pp. A90 ◽

Cited By ~ 1

Author(s):

S. M. Straal ◽

J. van Leeuwen

Keyword(s):

Black Hole ◽

Supernova Remnants ◽

Supernova Remnant ◽

Point Sources ◽

Pulsar Wind Nebulae ◽

Upper Limits ◽

Formation History ◽

Propagation Effects ◽

Pulsar Wind ◽

Rule Out

Pinpointing a pulsar in its parent supernova remnant (SNR) or resulting pulsar wind nebula (PWN) is key to understanding its formation history and the pulsar wind mechanism, yet only about half the SNRs and PWNe appear associated with a pulsar. Our aim was to find the pulsars in a sample of eight known and new SNRs and PWNe. Using the LOFAR radio telescope at 150 MHz, each source was observed for 3 h. We covered the entire remnants where needed, by employing many tied-array beams to tile out even the largest objects. For objects with a confirmed point source or PWN we constrained our search to those lines of sight. We identified a promising radio pulsar candidate towards PWN G141.2+5.0. The candidate, PSR J0337+61, has a period of 94 ms and a DM of 226 pc cm−3. We re-observed the source twice with increased sensitivities of 30% and 50%, but did not re-detect it. It thus remains unconfirmed. For our other sources we obtain very stringent upper limits of 0.8 − 3.1 mJy at 150 MHz. Generally, we can rule out that the pulsars travelled out of the remnant. From these strict limits we conclude our non-detections towards point sources and PWNe are the result of beaming and propagation effects. Some of the remaining SNRs should host a black hole rather than a neutron star.

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Pulsar Wind Nebulae

International Astronomical Union Colloquium ◽

10.1017/s0252921100041968 ◽

1996 ◽

Vol 160 ◽

pp. 393-399 ◽

Cited By ~ 2

Author(s):

James M. Cordes

Keyword(s):

Neutron Stars ◽

Radial Velocity ◽

Velocity Component ◽

Pulsar Wind Nebulae ◽

Radial Velocity Component ◽

Ram Pressure ◽

Pulsar Wind ◽

Pulsar Winds

AbstractI discuss pulsar wind nebulae for which ram pressure from the neutron star’s motion is a key element of the morphology. These PWN are tools for determining the pulsar distance, radial velocity component, and interaction of pulsar winds with surrounding media. The Guitar Nebula pulsar (B2224+65) also represents a ‘smoking gun’ for velocity kicks from asymmetric supernovae or other rocket effects. The detectability of wind nebulae from pulsars and from as-yet unknown neutron stars is discussed.

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