A population study of type II bursts in the Rapid Burster
| العنوان: | A population study of type II bursts in the Rapid Burster |
|---|---|
| المؤلفون: | T. Bagnoli, Caroline D'Angelo, J. J. M. in 't Zand, Duncan K. Galloway |
| المساهمون: | High Energy Astrophys. & Astropart. Phys (API, FNWI) |
| المصدر: | Monthly Notices of the Royal Astronomical Society, 449(1), 268-287 Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 449(1), 268-287. Oxford University Press |
| سنة النشر: | 2015 |
| مصطلحات موضوعية: | Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Thermonuclear fusion, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Flux, Binary number, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Computer Science::Computational Geometry, Magnetic field, Neutron star, Space and Planetary Science, Uniqueness, Astrophysics - High Energy Astrophysical Phenomena, Spin-½ |
| الوصف: | Type II bursts are thought to arise from instabilities in the accretion flow onto a neutron star in an X-ray binary. Despite having been known for almost 40 years, no model can yet satisfactorily account for all their properties. To shed light on the nature of this phenomenon and provide a reference for future theoretical work, we study the entire sample of Rossi X-ray Timing Explorer data of type II bursts from the Rapid Burster (MXB 1730-335). We find that type II bursts are Eddington-limited in flux, that a larger amount of energy goes in the bursts than in the persistent emission, that type II bursts can be as short as 0.130 s, and that the distribution of recurrence times drops abruptly below 15-18 s. We highlight the complicated feedback between type II bursts and the NS surface thermonuclear explosions known as type I bursts, and between type II bursts and the persistent emission. We review a number of models for type II bursts. While no model can reproduce all the observed burst properties and explain the source uniqueness, models involving a gating role for the magnetic field come closest to matching the properties of our sample. The uniqueness of the source may be explained by a special combination of magnetic field strength, stellar spin period and alignment between the magnetic field and the spin axis. Accepted 2015 February 12. Received 2015 February 10; in original form 2014 December 19 |
| وصف الملف: | application/pdf |
| اللغة: | English |
| تدمد: | 0035-8711 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::e80d859849e56d817040c3ec2788dfd6 http://hdl.handle.net/1887/49197 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....e80d859849e56d817040c3ec2788dfd6 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 00358711 |
|---|