Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind?
We find soft X-ray emission lines from the X-ray binary Swift J1858.6–0814 in data from XMM–NewtonReflection Grating Spectrometer (RGS): N VII, O VII, and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionization transitions. These could be associated with the di...
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| Autores principales: | , , , , , , , , , , , , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
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2020
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| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/125586 |
| Aporte de: |
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I19-R120-10915-125586 |
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| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Ciencias Astronómicas Accretion Accretion discs Black hole physics Stars: neutron X-rays: binaries |
| spellingShingle |
Ciencias Astronómicas Accretion Accretion discs Black hole physics Stars: neutron X-rays: binaries Buisson, D. J. K. Altamirano, Diego Diaz Trigo, M. Mendez, Mariano Padilla, M. Armas Castro Segura, N. Degenaar, Nathalie van den Eijnden, J. Fogantini, Federico Adrián Gandhi, Poshak Knigge, Christian Muñoz-Darias, T. Arabaci, M. Ozbey Vincentelli, F. M. Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| topic_facet |
Ciencias Astronómicas Accretion Accretion discs Black hole physics Stars: neutron X-rays: binaries |
| description |
We find soft X-ray emission lines from the X-ray binary Swift J1858.6–0814 in data from XMM–NewtonReflection Grating Spectrometer (RGS): N VII, O VII, and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionization transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6–0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionization parameter log (ξ) = 1.35 ± 0.2 and a density n > 1.5 × 10¹¹ cm⁻³. From this, we infer that the emitting plasma must be within 1013 cm of the ionizing source, ∼5 × 10⁷ rg for a 1.4 M⊙ neutron star, and from the line width that it is at least 10⁴ rg away [2 × 10⁹(M/1.4 M⊙) cm]. We compare this with known classes of emission-line regions in other X-ray binaries and active galactic nuclei. |
| format |
Articulo Articulo |
| author |
Buisson, D. J. K. Altamirano, Diego Diaz Trigo, M. Mendez, Mariano Padilla, M. Armas Castro Segura, N. Degenaar, Nathalie van den Eijnden, J. Fogantini, Federico Adrián Gandhi, Poshak Knigge, Christian Muñoz-Darias, T. Arabaci, M. Ozbey Vincentelli, F. M. |
| author_facet |
Buisson, D. J. K. Altamirano, Diego Diaz Trigo, M. Mendez, Mariano Padilla, M. Armas Castro Segura, N. Degenaar, Nathalie van den Eijnden, J. Fogantini, Federico Adrián Gandhi, Poshak Knigge, Christian Muñoz-Darias, T. Arabaci, M. Ozbey Vincentelli, F. M. |
| author_sort |
Buisson, D. J. K. |
| title |
Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| title_short |
Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| title_full |
Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| title_fullStr |
Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| title_full_unstemmed |
Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: Disc atmosphere or wind? |
| title_sort |
soft x-ray emission lines in the x-ray binary swift j1858.6-0814 observed with xmm-newton-rgs: disc atmosphere or wind? |
| publishDate |
2020 |
| url |
http://sedici.unlp.edu.ar/handle/10915/125586 |
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Repositorios |
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