Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind
We present the analysis of six Chandra X-ray high-resolution observations of the black hole low-mass X-ray binary 4U 1630-47 taken during its 2012–2013 outburst. Fe XXVI K α, K β, Fe XXV K α, K β, and Ca XX K α blueshifted absorption lines were identified in the first four observations, which corres...
| Main Authors: | , , , |
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| Format: | Journal Article |
| Published: |
Oxford University Press
2019
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| Online Access: | http://purl.org/au-research/grants/arc/FT140101082 http://hdl.handle.net/20.500.11937/74104 |
| _version_ | 1848763181918322688 |
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| author | Gatuzz, E. Trigo, M. Miller-Jones, James Migliari, S. |
| author_facet | Gatuzz, E. Trigo, M. Miller-Jones, James Migliari, S. |
| author_sort | Gatuzz, E. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We present the analysis of six Chandra X-ray high-resolution observations of the black hole low-mass X-ray binary 4U 1630-47 taken during its 2012–2013 outburst. Fe XXVI K α, K β, Fe XXV K α, K β, and Ca XX K α blueshifted absorption lines were identified in the first four observations, which correspond to soft accretion states. The remaining observations, associated to intermediate and possibly hard accretion states, do not show significant absorption features down to equivalent width of 1 eV for both Fe XXVI and Fe XXV. We inferred wind launching radii between 1.2 − 2.0 (1012 cm/n) × 1011 cm and column densities N(H) > 1023 cm−2. In the first four observations, we found that thermal pressure is likely to be the dominant launching mechanism for the wind, although such conclusions depend on the assumed density. We used the spectral energy distributions obtained from our continuum modelling to compute thermal stability curves for all observations using the XSTAR photoionization code. We found that the absence of lines in the transitional state cannot be attributed to an evolution of the plasma caused by thermal instabilities derived from the change in the continuum spectrum. In contrast, the disappearance of the wind could indicate an acceleration of the flow or that the plasma has been exhausted during the soft state. |
| first_indexed | 2025-11-14T10:59:23Z |
| format | Journal Article |
| id | curtin-20.500.11937-74104 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T10:59:23Z |
| publishDate | 2019 |
| publisher | Oxford University Press |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-741042022-11-23T06:51:08Z Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind Gatuzz, E. Trigo, M. Miller-Jones, James Migliari, S. We present the analysis of six Chandra X-ray high-resolution observations of the black hole low-mass X-ray binary 4U 1630-47 taken during its 2012–2013 outburst. Fe XXVI K α, K β, Fe XXV K α, K β, and Ca XX K α blueshifted absorption lines were identified in the first four observations, which correspond to soft accretion states. The remaining observations, associated to intermediate and possibly hard accretion states, do not show significant absorption features down to equivalent width of 1 eV for both Fe XXVI and Fe XXV. We inferred wind launching radii between 1.2 − 2.0 (1012 cm/n) × 1011 cm and column densities N(H) > 1023 cm−2. In the first four observations, we found that thermal pressure is likely to be the dominant launching mechanism for the wind, although such conclusions depend on the assumed density. We used the spectral energy distributions obtained from our continuum modelling to compute thermal stability curves for all observations using the XSTAR photoionization code. We found that the absence of lines in the transitional state cannot be attributed to an evolution of the plasma caused by thermal instabilities derived from the change in the continuum spectrum. In contrast, the disappearance of the wind could indicate an acceleration of the flow or that the plasma has been exhausted during the soft state. 2019 Journal Article http://hdl.handle.net/20.500.11937/74104 10.1093/mnras/sty2850 http://purl.org/au-research/grants/arc/FT140101082 Oxford University Press fulltext |
| spellingShingle | Gatuzz, E. Trigo, M. Miller-Jones, James Migliari, S. Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title | Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title_full | Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title_fullStr | Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title_full_unstemmed | Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title_short | Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind |
| title_sort | chandra high-resolution spectra of 4u 1630-47: the disappearance of the wind |
| url | http://purl.org/au-research/grants/arc/FT140101082 http://hdl.handle.net/20.500.11937/74104 |