Optical spectroscopy of the low-mass X-ray binary GX 9+9
Phase-resolved medium-resolution VLT spectroscopy of the low-mass X-ray binary GX 9+9 has revealed narrow C iii emission lines that move in phase relative to our new estimate of the ephemeris, and show a velocity amplitude of 230 ± 35 km s-1. We identify the origin of these lines as coming from the...
| Main Authors: | , , , , , , |
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| Format: | Journal article |
| Language: | English |
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2007
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| _version_ | 1826259517872013312 |
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| author | Cornelisse, R Steeghs, D Casares, J Charles, P Barnes, A Hynes, R O'Brien, K |
| author_facet | Cornelisse, R Steeghs, D Casares, J Charles, P Barnes, A Hynes, R O'Brien, K |
| author_sort | Cornelisse, R |
| collection | OXFORD |
| description | Phase-resolved medium-resolution VLT spectroscopy of the low-mass X-ray binary GX 9+9 has revealed narrow C iii emission lines that move in phase relative to our new estimate of the ephemeris, and show a velocity amplitude of 230 ± 35 km s-1. We identify the origin of these lines as coming from the surface of the donor star, thereby providing the first estimate of the mass function of f(M1) ≥ 0.22 M⊙. Rotational broadening estimates together with assumptions for the mass donor give 0.07 ≤ q ≤ 0.35 and 182 ≤ K2 ≤ 406 km s -1. Despite a low-mass ratio, there is no evidence for a superhump in our data set. Doppler maps of GX 9+9 show the presence of a stream overflow, either in the form of material flowing downward along the accretion disc rim or in a similar fashion as occurs in high mass transfer rate cataclysmic variables known as the SW Sex stars. Finally, we note that the Bowen region in GX 9+9 is dominated by C iii instead of N iii emission as has been the case for most other X-ray binaries. © 2007 RAS. |
| first_indexed | 2024-03-06T18:51:09Z |
| format | Journal article |
| id | oxford-uuid:1042076a-6cad-45c3-99a6-bf05d937ea7a |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:51:09Z |
| publishDate | 2007 |
| record_format | dspace |
| spelling | oxford-uuid:1042076a-6cad-45c3-99a6-bf05d937ea7a2022-03-26T09:55:39ZOptical spectroscopy of the low-mass X-ray binary GX 9+9Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:1042076a-6cad-45c3-99a6-bf05d937ea7aEnglishSymplectic Elements at Oxford2007Cornelisse, RSteeghs, DCasares, JCharles, PBarnes, AHynes, RO'Brien, KPhase-resolved medium-resolution VLT spectroscopy of the low-mass X-ray binary GX 9+9 has revealed narrow C iii emission lines that move in phase relative to our new estimate of the ephemeris, and show a velocity amplitude of 230 ± 35 km s-1. We identify the origin of these lines as coming from the surface of the donor star, thereby providing the first estimate of the mass function of f(M1) ≥ 0.22 M⊙. Rotational broadening estimates together with assumptions for the mass donor give 0.07 ≤ q ≤ 0.35 and 182 ≤ K2 ≤ 406 km s -1. Despite a low-mass ratio, there is no evidence for a superhump in our data set. Doppler maps of GX 9+9 show the presence of a stream overflow, either in the form of material flowing downward along the accretion disc rim or in a similar fashion as occurs in high mass transfer rate cataclysmic variables known as the SW Sex stars. Finally, we note that the Bowen region in GX 9+9 is dominated by C iii instead of N iii emission as has been the case for most other X-ray binaries. © 2007 RAS. |
| spellingShingle | Cornelisse, R Steeghs, D Casares, J Charles, P Barnes, A Hynes, R O'Brien, K Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title | Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title_full | Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title_fullStr | Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title_full_unstemmed | Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title_short | Optical spectroscopy of the low-mass X-ray binary GX 9+9 |
| title_sort | optical spectroscopy of the low mass x ray binary gx 9 9 |
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