The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
We analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the <i>ossi X-ray Timing Explorer</i> (<i> RXTE</i>). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From...
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| Autores principales: | , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2013
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/127272 |
| Aporte de: |
| Sumario: | We analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the <i>ossi X-ray Timing Explorer</i> (<i> RXTE</i>). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From the analysis of time-resolved spectra during the cooling phase of the bursts, we found that the relation between the bolometric flux and the temperature is very different from the canonical F ∝ T⁴ relation which is expected if the apparent emitting area on the surface of the neutron star remains constant. The flux-temperature relation can be fitted using a broken power law, with indices ν₁ = 2.0 ± 0.3 and ν₂ = 5.72 ± 0.06. The departure from the F ∝ T⁴ relation during the cooling phase of the X-ray bursts in 4U 1820-30 could be due to changes in the emitting area of the neutron star while the atmosphere cools down, variations in the colour-correction factor due to chemical evolution, or the presence of a source of heat, e.g. residual hydrogen nuclear burning, playing an important role when the burst emission ceases. |
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