Table 7.
Parameters of the stellar wind in the Vela X-1 system as derived by different authors, see Sects. 3.2.3 and 3.2.4.
| Reference | vesc [km s−1] | v∞ [km s−1] | β | Ṁ [10−6 M⊙ yr−1] | Comments |
|---|---|---|---|---|---|
| Lamers et al. (1976) (L76) | – | – | – | 0.5 | X-ray fluxes & wind accretion |
| Hutchings (1976) (H76) | – | – | – | 7 | Spectroscopy, mass-loss model |
| Conti (1978) | 519 | 1600 | – | (H76) | Similar study to L76 |
| Dupree et al. (1980) (D80) | 489 | ∼1700 | 0.5 | ∼1 | |
| McCray et al. (1984) (M84) | – | (D80) | 1 | 4 | |
| Sadakane et al. (1985) | – | ∼1500 | – | (D80) | Multiple components with different velocities |
| Sato et al. (1986) | – | 1600(a) | (D80) | 2.4 ± 1.2 | |
| Prinja et al. (1990) | (590) | 1105 | – | – | vesc is mean for spectral type |
| Sako et al. (1999) | – | (D80) | 0.79 ± 0.23 |  (b) |
X-ray DEM modeling |
| van Loon et al. (2001) | – | 600 ± 100 | – | – | Modeling of UV lines |
| Watanabe et al. (2006) | – | 1100(c) | 0.8 | 1.5–2.0 | X-ray line MC modeling |
| Krtička et al. (2012) | 750 | (∼0.8) | 1.5 | See reference for details | |
| Falanga et al. (2015) | – | 640 ± 190 | – | < (1–5.3) | See reference for details |
| Manousakis & Walter (2015b) | – | (D80) | 0.55 | (M84) | Simulating hard X-ray light curve |
| Giménez-García et al. (2016) | 436 ± 65 |  |
1.0 | 0.4–1 | |
| Sander et al. (2018), no X-rays | – | 532 | (∼2.2) | 0.65 | See reference for details |
| – ditto –, moderate X-ray illum. | – | 584 | (∼2.2) | 0.66 | |
| – ditto –, strong X-ray illumination | – | 378 | (∼2.2) | 0.85 |
Notes. When a value was taken from a previous publication, we mark this by a shorthand, e.g., D80 for Dupree et al. (1980). Numbers in italics in the table have been set as fixed in the respective publications. Krtička et al. (2012) and Sander et al. (2018) did not assume a basic β-law for wind acceleration, and the value given in this table corresponds to an approximate β-law fit to their results for comparison. For other parameters, see Tables 4 and 5.
Referring to Dupree et al. (1980).
Argued to be the mass fraction in hot ionized gas, while most mass would be contained in cool clumps.
Referring to Prinja et al. (1990).
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