Salvato in:
| Autori principali: | , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2023
|
| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2304.05280 |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866913220085678080 |
|---|---|
| author | Çoban, Ömer Faruk Ertan, Unal |
| author_facet | Çoban, Ömer Faruk Ertan, Unal |
| contents | We show that a typical X-ray outburst light curve of Aql X-1 can be reproduced by accretion onto the neutron star in the frame of the disk instability model without invoking partial accretion or propeller effect. The knee and the subsequent sharp decay in the X-ray light curve can be generated naturally by taking into account the weak dependence of the disk aspect ratio, $h/r$, on the disk mass-flow rate, $\dot{M}_\mathrm{in}$, in the X-ray irradiation flux calculation. This $\dot{M}_\mathrm{in}$ dependence of $h/r$ only slightly modifies the irradiation temperature profile along the hot disk in comparison to that obtained with constant $h/r$. Nevertheless, this small difference has a significant cumulative effect on the hot disk radius leading to a much faster decrease in the size of the hot disk, and thereby to a sharper decay in the X-ray outburst light curve. The same model also produces the long-term evolution of the source consistently with its observed outburst recurrence times and typical light curves of Aql X-1. Our results imply that the source accretes matter from the disk in the quiescent state as well. We also estimate that the dipole moment of the source $μ\lesssim 4 \times 10^{26}$ G cm$^3~$($B \lesssim 4 \times 10^{8}$ G at the surface). |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2304_05280 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Typical X-ray Outburst Light Curves of Aql X-1 Çoban, Ömer Faruk Ertan, Unal High Energy Astrophysical Phenomena 85A10 We show that a typical X-ray outburst light curve of Aql X-1 can be reproduced by accretion onto the neutron star in the frame of the disk instability model without invoking partial accretion or propeller effect. The knee and the subsequent sharp decay in the X-ray light curve can be generated naturally by taking into account the weak dependence of the disk aspect ratio, $h/r$, on the disk mass-flow rate, $\dot{M}_\mathrm{in}$, in the X-ray irradiation flux calculation. This $\dot{M}_\mathrm{in}$ dependence of $h/r$ only slightly modifies the irradiation temperature profile along the hot disk in comparison to that obtained with constant $h/r$. Nevertheless, this small difference has a significant cumulative effect on the hot disk radius leading to a much faster decrease in the size of the hot disk, and thereby to a sharper decay in the X-ray outburst light curve. The same model also produces the long-term evolution of the source consistently with its observed outburst recurrence times and typical light curves of Aql X-1. Our results imply that the source accretes matter from the disk in the quiescent state as well. We also estimate that the dipole moment of the source $μ\lesssim 4 \times 10^{26}$ G cm$^3~$($B \lesssim 4 \times 10^{8}$ G at the surface). |
| title | Typical X-ray Outburst Light Curves of Aql X-1 |
| topic | High Energy Astrophysical Phenomena 85A10 |
| url | https://arxiv.org/abs/2304.05280 |