X-Ray and Near-Infrared Observations of the Middle-aged Pulsar B1055–52, Its Multiwavelength Spectrum, and Proper Motion*

Journal article

The diffusion coefficients around the pulsar $\gamma$-ray halos are highly suppressed compared with the value in the interstellar medium. It is suggested in the literature that the $\gamma$-ray halos can be explained by a ballistic-diffusive (BD) propagation without slow diffusion. However our calculation shows that the BD propagation can not account for the $\gamma$-ray halo profile well. Furthermore the transfer efficiency of the pulsar spin down energy to the high energy electrons and positrons is even larger than 1 in the BD scenario. Therefore slow diffusion is necessary to account for the pulsar $\gamma$-ray halos. Taking the slow diffusion into account the contribution of positron flux originated from nearby pulsars to the AMS-02 data is reexamined. We may also expect a slow diffusion disk of the Milky Way as many such slow diffusion regions exist. The positron contribution to the AMS-02 data from dark matter annihilation in the new propagation model is also reexamined. We find that the dark matter scenario satisfies all the $\gamma$-ray limits in the new propagation model.Comment: 10 pages, 8 figures. Proceedings of the 38th International Cosmic Ray Conference (ICRC2023) in Nagoya, Japa

Authors: Posselt, B; Pavlov, GG; Kargaltsev, O; Hare, J

• Publication status: Published
• Peer review status: Peer reviewed
• Publisher: American Astronomical Society
• Journal: The Astrophysical Journal
• Volume: 952
• Issue: 2
• Pages: 134-134
• Publication date: 2023-07-24
• DOI: 10.3847/1538-4357/acd9d1
• EISSN: 1538-4357
• ISSN: 0004-637X
• Language: English
• Keywords: Physics; Infrared; Stars; Pulsar; Proper motion; Astronomy; Astrophysics; Spectrum (functional analysis); Classical mechanics; Motion (physics)