Discovery of a pulsar wind nebula around B0950 + 08 with the ELWA
| Autor: | G. B. Taylor, D. Ruan, Paul Demorest, Jayce Dowell, Frank K. Schinzel, Kevin Stovall |
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| Rok vydání: | 2020 |
| Předmět: |
010504 meteorology & atmospheric sciences
Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Pulsar wind nebula law.invention Pulsar law 0103 physical sciences Cylinder 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences High Energy Astrophysical Phenomena (astro-ph.HE) Physics Spectral index Compton scattering Astronomy and Astrophysics Radius Synchrotron Imaging analysis 13. Climate action Space and Planetary Science Astrophysics - High Energy Astrophysical Phenomena |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 495:2125-2134 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/staa1305 |
| Popis: | With the Expanded Long Wavelength Array and pulsar binning techniques, we searched for off-pulse emission from PSR B0950 + 08 at 76 MHz. Previous studies suggest that off-pulse emission can be due to pulsar wind nebulae (PWNe) in younger pulsars. Other studies, such as that done by Basu et al., propose that in older pulsars this emission extends to some radius that is on the order of the light cylinder radius, and is magnetospheric in origin. Through imaging analysis, we conclude that this older pulsar with a spin-down age of 17 Myr has a surrounding PWN, which is unexpected since as a pulsar ages its PWN spectrum is thought to shift from being synchrotron to inverse Compton scattering dominated. At 76 MHz, the average flux density of the off-pulse emission is 0.59 ± 0.16 Jy. The off-pulse emission from B0950+08 is ∼ 110 ± 17 arcsec (0.14 ± 0.02 pc) in size, extending well beyond the light cylinder diameter and ruling out a magnetospheric origin. Using data from our observation and the surveys VLSSr, TGSS, NVSS, FIRST, and VLASS, we have found that the spectral index for B0950 + 08 is about −1.36 ± 0.20, while the PWN’s spectral index is steeper than −1.85 ± 0.45. |
| Databáze: | OpenAIRE |
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