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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| Formato: | Articulo |
| Lenguaje: | Inglés |
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2013
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| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/127272 |
| Aporte de: |
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I19-R120-10915-127272 |
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dspace |
| institution |
Universidad Nacional de La Plata |
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I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Astronomía stars: individual: 4U 1820−30 stars: neutron X-rays: binaries X-rays: bursts |
| spellingShingle |
Astronomía stars: individual: 4U 1820−30 stars: neutron X-rays: binaries X-rays: bursts García, Federico Zhang, Guobao Méndez, Mariano R. The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| topic_facet |
Astronomía stars: individual: 4U 1820−30 stars: neutron X-rays: binaries X-rays: bursts |
| description |
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. |
| format |
Articulo Articulo |
| author |
García, Federico Zhang, Guobao Méndez, Mariano R. |
| author_facet |
García, Federico Zhang, Guobao Méndez, Mariano R. |
| author_sort |
García, Federico |
| title |
The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| title_short |
The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| title_full |
The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| title_fullStr |
The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| title_full_unstemmed |
The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation |
| title_sort |
cooling phase of type i x-ray bursts observed with rxte in 4u 1820−30 does not follow the canonical f ∝ t⁴ relation |
| publishDate |
2013 |
| url |
http://sedici.unlp.edu.ar/handle/10915/127272 |
| work_keys_str_mv |
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Repositorios |
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1764820451530375171 |