New insight into the physical essence of pulsar glitch
| Autor: | Jing-Jing Liu, Qiu-He Peng, Chih-Kang Chou |
|---|---|
| Rok vydání: | 2022 |
| Předmět: |
Physics
Phase transition Astrophysics::High Energy Astrophysical Phenomena Astrophysics::Instrumentation and Methods for Astrophysics Phase (waves) Astronomy and Astrophysics Astrophysics Glitch Superfluidity Neutron star Amplitude Pulsar Space and Planetary Science Astrophysics::Solar and Stellar Astrophysics Neutron Instrumentation |
| Zdroj: | New Astronomy. 90:101655 |
| ISSN: | 1384-1076 |
| DOI: | 10.1016/j.newast.2021.101655 |
| Popis: | Based on the oscillation between the B phase and A phase of 3 P 2 neutron superfluid in neutron stars, we propose a new glitch model for young pulsars. According to our model, the glitch is explained as a repeat phenomena from the quasi period 3 P 2 neutron superfluid B phase, to A phase, then to B phase (many repeated glitches with quasi-period). With the repeating of the phase transition, the vortex quantum number of 3 P 2 neutron superfluid vortices is gradually reduced, and the heating rate e ( B ) in B phase also gets lower and lower. After a number of glitches, the time intervals between successive glitches will gradually become longer, and the glitch amplitude decreases. When the heating rate e ( B ) of an old neutron star becomes lower than the cooling rate of the direct Urca, which can happen in a super-strongmagnetic field, the B phase of the 3 P 2 neutron superfluid vortices is no longer returned to the A phase state and the phase oscillation of the system is stopped immediately. The slowing glitch phenomenon of some older pulsars is a natural result of our theory, which means that very old pulsars will no longer present the glitch. Our model will be tested in future pulsar glitch observations. |
| Databáze: | OpenAIRE |
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